ALBERT

Description: Inhaltsverzeichnis : EHLERS, J. & MENSCHING, H.: Küstenversatz und Prielverlagerungen an der Nordseeküste. S. 9-22 ; FRÄNZLE, O.: Periglaziäre Formung der Altmoränengebiete Schleswig-Holsteins. S. 23-35 ; HEMPEL, L.: Rezente und fossile Mesoformen der Abtragung und Aufschüttung in Ausräumen von Schichtkammlandschaften im Teutoburger Wald. S. 37-47 ; LEHMEIER, F.: Zum Formenschatz der Schichtkammlandschaft im Niedersächsischen Bergland. S. 49-61 ; GARLEFF, K., BRUNOTTE, E. & STINGL, H.: Fußflächen im zentralen Teil der Hessischen Senke. S. 63-76 ; MÖLLER, K.: Das Eschweger Becken und seine Randbereiche — Ergebnisse geomorphographischer und hydrochemischer Analysen. S. 77-92 ; GLATTHAAR, D.: Vertikalbewegungen und ihre Bedeutung für die Formenentwicklung im Westerwald. S. 93-106 ; MÜLLER, M.J.: Periglaziärfluviale, solifluidale und abluale Formung im westlichen Hunsrück und am Ostrand der Trier-Bitburger Mulde. S. 107-118 ; BARSCH, D. & MÄUSBACHER, R.: Zur fluvialen Dynamik beim Aufbau des Neckarschwemmfächers. S. 119-128 ; LESER, H.: Schichtstufen und Talrandstufen in Südwestdeutschland. S. 129-147 ; FARRENKOPF, D.: Relief und Wasserhaushalt im Eyachtal, Nordschwarzwald. S. 149-154 ; LESER, H. & METZ, B.: Vergletscherungen im Hochschwarzwald. S. 155-175 ; HABBE, K.A.: Was kann eine geomorphologische Vollkartierung für die Stratigraphie des Quartärs leisten? S. 177-196 ; RATHJENS, C.: Jungglaziale Formung und spätglazialer Eisabbau im Chiemgau. S. 197-205 ; FISCHER, K.: Die würmzeitliche und stadiale Vergletscherung der Berchtesgadener Alpen. S. 207-225 ;

Description: research

Description: DFG, SUB Göttingen

Description: Zur Vereinfachung wird die Vielfalt der Karstformenbezeichnungen bereinigt. Erdfall wird als Form, die in nicht verkarstungsfähigen Serien liegt, aber auf Tiefensubrosion zurückgeht, der Doline, einer Form, die in verkarstungsfähigem Material liegt, gegenübergestellt. Als Grundlage der Arbeit wurde eine detaillierte Kartierung der Auslaugungsformen durchgeführt. Hinsichtlich rezenter Subrosion erwies es sich als notwendig, die in Oberflächenwässern und wasserwirtschaftlich erfaßten Wässern gelösten Bestandteile von Chlorid, Sulfat und Karbonat zu ermitteln. Die Auswertung der gewonnenen Daten zeigt, daß ein Zusammenhang mit Gebieten besteht, die durch aktuelle Erdfälle und Dolineneinbrüche gekennzeichnet sind. Als Voraussetzung zur Reliefgenese gilt, daß das Gebiet des Unterwerra-Sattels entscheidend durch die saxonische Gebirgsbildung an der Wende Jura/Kreide und die nachfolgende klimageomorphologische Entwicklung geprägt ist. Anhand der geomorphographischen Analyse wird der Einfluß der Salz-, aber auch der Sulfatauslaugung auf die Landschaftsgenese belegt. Die Auslaugung des Salzes (Nal), dessen Mächtigkeit im Untersuchungsgebiet mit mindestens 120 m angenommen wird, und der unterlagernden ca. 130 m nächtigen Zechsteingipse (A 1 - A 3) zerrüttet die überlagernden triassischen Schichten weiter. Darüber hinaus wirkt die Subrosion von mehr als 30 m Rötgipsen und 50 m Gipsen des Mittleren Muschelkalkes im Hangenden des Zechsteins reliefformend. Die ermittelten Ergebnisse - rezente und subrezente Formen, Lösungswerte – werden zunächst in kleineren Gebietseinheiten analysiert. Die Ergebnisse der Nasseranalysen bestätigen das geomorphographische Ergebnis, so daß in Anlehnung an die Gipshorizonte von Stockwerkssubrosion gesprochen werden kann. Entscheidend geprägt ist die heutige Situation jedoch durch vorangegangene Zechsteinsalzauslaugung im tieferen Untergrund. Diese hat in den Hangendserien die Wasserwegsamkeit verstärkt, so daß die nachfolgende Sulfatsubrosion den Kleinformenschatz vor der Schichtstufe des Mittleren Buntsandsteins steuern konnte. Aufgrund ihrer für Auslaugungsgebiete typischen Ausprägung wird die Lage der Schichtstufe in weiten Teilen des Untersuchungsgebietes an das in Auslaugung befindliche Salz geknüpft. Das Auftreten von Subrosionsformen vor der Landstufe des Kaufunger Waldes, den östlichen Meißnerhängen, dem Anstieg des Schlierbachswaldes sowie vor dem Anstieg des Buntsandsteins zwischen Heldra, Frieda und Bad Sooden-Allendorf untermauert diese Interpretation. In der südlichen und südöstlichen Umrahmung des Untersuchungsgebietes wird der Salzhang aufgrund geomorphographischer Kriterien unter dem Steilanstieg des Unteren Muschelkalkes ausgewiesen. Aufgrund dieser Befunde wird die primäre Salzverbreitung als über den Unterwerra-Sattel reichend angenommen, womit sich, abgesehen von den Einflüssen der saxonischen Tektonik, alle Reliefentwicklungsprozesse allein durch Auslaugung und folgende geomorphologische Überprägung erklären lassen. Darüber hinaus ist dieses Gebiet in Nordhessen nicht nur durch eine über alle Schichten hinweggreifende Rumpfflächenbildung gekennzeichnet, sondern die Resistenzunterschiede wurden - unabhängig vom Klima - beständig herausgearbeitet. Aus diesen Ergebnissen wurde ein übergeordnetes Modell zur Reliefentwicklung erstellt. Danach existieren im Untersuchungsgebiet fünf Reliefgenerationen, wobei die postsaxonische Reliefentwicklung mit zerstörtem, die Auslaugung begünstigendem Hangendverband nach der Landhebung bzw. dem Einbruch der das Gebiet begrenzenden Grabenstrukturen, die bis ins Alttertiär reicht, nicht erfaßt werden konnte. [...]

Description: research

Description: DFG, SUB Göttingen

Description: In der vorliegenden Arbeit wurden Ergebnisse hydrologischer und stratigraphischer Studien zur Entwicklungsgeschichte von Brandenburger Kesselmooren vorgestellt. Für die Erfassung der aktuellen und historischen biotischen und abiotischen Standortfaktoren wurden verschiedene Methoden angewandt: floristische und vegetationskundliche Untersuchungen sowie hydrologische, hydrochemische, geochemische, geophysikalische und sedimentologische Untersuchungen und Makrorest-‚ Mikrorest- und Pollenanalyse. Der zeitlichen Einordnung der entwicklungsgeschichtlichen Prozesse dienten Radiocarbondatierungen und die pollenanalytischen Untersuchungen. Ziel der Arbeit war es, Entwicklungsstadien auszuscheiden, die von den untersuchten Mooren seit ihrer Entstehung durchlaufen wurden. Aufgrund der stratigraphischen Untersuchungen wurden Aussagen zur Beckengenese und zu den einzelnen See- und Moorentwicklungsphasen getroffen, zum Verlandungsvorgang, zu Moorbildungsbedingungen und Sukzessionsstadien. Den Entwicklungsstadien konnten über geochemische und -physikalische Untersuchungen abiotische Standortfaktoren zugeordnet werden. Die aktuellen Standortveränderungen wurden erfaßt und die vorgenommenen Erhaltungs- und Wiedervernässungsmaßnahmen dokumentiert und bewertet.

Description: research

Description: DFG, SUB Göttingen

Description: Dieser Band enthält 63 Artikel zu Themengebieten der Physik der festen Erde, zu magnetischen und elektrischen Feldern der Erde, zu der Physik der Atmophäre und der angewandten Geophysik veröffentlicht durch die Deutsche Geophysikalische Gesellschaft in dem Jahr 1934.

Description: 〈html〉 〈body〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0004.pdf"〉Titelseite〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0005.pdf"〉Autorenverzeichnis〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0006.pdf"〉Sachverzeichnis〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0007.pdf"〉Karl Mack †〈/a〉〈br〉(Hiller, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0008.pdf"〉Die südalbanischen Erdbeben 1930/31〈/a〉〈br〉(Nowack, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0009.pdf"〉Seismische Untersuchungen des Geophysikalischen Instituts in Göttingen〈/a〉〈br〉(Gräfe, H., v. zur Mühlen, W., Müller, H. K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0017.pdf"〉Horizontalsicht bei örtlich veränderlicher Trübung und Beleuchtung〈/a〉〈br〉(Steinhäusser, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0018.pdf"〉Referate und Mitteilungen〈/a〉〈br〉(Haase, H., Köhler, R., Berroth, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0019.pdf"〉Beitrag zur Berechnung von Minimum-Stabpendeln〈/a〉〈br〉(Graf, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0020.pdf"〉Zur Theorie elastischer Pendel mit besonderer Berücksichtigung des Holweck-Lejayschen Stabpendels〈/a〉〈br〉(Graf, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0021.pdf"〉Eine neue Methode für sehr präzise magnetische Messungen〈/a〉〈br〉(Koulomzine, T., Bondaletoff, N.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0022.pdf"〉Zur Frage der mit dem temperaturkompensierten Magnetsystem erreichbaren Meßgenauigkeit〈/a〉〈br〉(Kohl, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0023.pdf"〉Die Höhenverteilung der Erd-, Luft- und Höhenstrahlung〈/a〉〈br〉(Suckstorff, G. A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0024.pdf"〉Erdstrahlungsmessungen in Bad Nauheim nach der Gammastrahlenmethode〈/a〉〈br〉(Masuch, V.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0025.pdf"〉Referate〈/a〉〈br〉(Jung, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0026.pdf"〉Abschnitt〈/a〉〈br〉(Angenheister, G., Kohlschütter, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0027.pdf"〉Hergesell geb. 29. Mai 1859〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0028.pdf"〉Hecker geb. 21. Mai 1864〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0029.pdf"〉Sprengungen zur Forschungszwecken mit Unterstützung der Notgemeinschaft der Deutschen〈/a〉〈br〉(Duckert, P.)〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0037.pdf"〉Beiträge zu den Luftschallmessungen〈/a〉〈br〉(Meißer, O., Martin, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0039.pdf"〉Seismische Untersuchungen des Geophysikalischen Instituts in Göttingen〈/a〉〈br〉(Regula, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0042.pdf"〉Berechnung der Laufzeitkurven des anormalen Schalles für windstille Atmosphäre und Vergleich mit der Laufzeitkurve der Oldebroek-Sprengung vom 15. Dezember 1932〈/a〉〈br〉(Jung, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0043.pdf"〉Ergebisse der Registrierungen von Schallwellen an kreisförmig um den Sprengherd angeordneten Stationen〈/a〉〈br〉(Duckert, P.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0044.pdf"〉Beobachtungsergebnisse über den Einfluß der "akustischen Umkehrschicht" auf die Schallausbreitung〈/a〉〈br〉(Sandmann, B.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0045.pdf"〉Zur Frage der anomalen Schallausbreitung〈/a〉〈br〉(Kölzer, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0046.pdf"〉Schalluntersuchungen im Polargebiet〈/a〉〈br〉(Wölcken, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0049.pdf"〉Betrachtungen über ebene Pendel〈/a〉〈br〉(Hahnkamm, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0051.pdf"〉Außenraum und Innenraum (Schlichtung des Streites um die Schwerkraftreduktion)〈/a〉〈br〉(Schwinner, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0052.pdf"〉Bemerkungen zu den Geoiden von Ackerl und Hirvonen〈/a〉〈br〉(Ledersteger, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0053.pdf"〉Auto-Radio als Hilfsmittel geologischer Kartierung〈/a〉〈br〉(Cloos, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0054.pdf"〉Zur photographischen Registrierung von Stationsseismometern〈/a〉〈br〉(Meißer, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0056.pdf"〉Ein Horizontalseismometer für die Aufzeichnung von starken Orts- und Nahbeben〈/a〉〈br〉(Critikos, N. A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0059.pdf"〉Die Bedeutung der Unstetigkeiten im Verlauf der Schallgeschwindigkeit mit der Höhe für die normale und anomale〈/a〉〈br〉(Sandmann, B.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0060.pdf"〉Referate und Mitteilungen〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0061.pdf"〉Die Relativität der Undulationen〈/a〉〈br〉(Hopfner, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0062.pdf"〉Ein detonierendes Meteor über dem Weserbergland am 2. Januar 1934〈/a〉〈br〉(Hartmann, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0063.pdf"〉Der Meteorfall bei Stadt Rehburg am 2. Januar 1934〈/a〉〈br〉(Trommsdorff, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0064.pdf"〉Vergleich zwischen der Intensität der kosmischen Ultrastrahlung über Grönland und über Deutschland〈/a〉〈br〉(Wölcken, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0065.pdf"〉Das Grundeis〈/a〉〈br〉(Jakuschoff, P.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0066.pdf"〉Le problème des microséismes et le déferlement des vagues〈/a〉〈br〉(Gherzi, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0067.pdf"〉Note on the Hayford-Bowie tables for calculation 〈i〉g〈/i〉〈/a〉〈br〉(Bullard, E. C.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0068.pdf"〉Kann die Laplacesche Differentialgleichung für das Schwerkraftpotential auch innerhalb der Erdkruste als erfüllt angesehen werden?〈/a〉〈br〉(Grabowski, L.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0069.pdf"〉Vorträge, gehalten auf der XI. Tagung der Deutschen Geophysikalischen Gesellschaft, am 13. bis 15. September 1934 in Pyrmont〈/a〉〈br〉(Jung, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0072.pdf"〉Der geophysikalische Nachweis des Zechsteindolomits〈/a〉〈br〉(Müller, M.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0073.pdf"〉Berichtigung〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0074.pdf"〉Vorträge, gehalten auf der XI. Tagung der Deutschen Geophysikalischen Gesellschaft, am 13. bis 15. September 1934 in Pyrmont〈/a〉〈br〉(von Seidlitz, W., Sieberg, A., Linke, F., Gerlach, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0079.pdf"〉Zur Frage der Geländekorrektion bei Drehwaagemessungen〈/a〉〈br〉(Tuchel, G.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0080.pdf"〉Emanation in Boden- und Freiluft〈/a〉〈br〉(Israël, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0081.pdf"〉Die Energie der Heliokathodenstrahlen in ihrer Beziehung zur fortschreitenden Bewegung der Elektronen in den Polarlichtstrahlen〈/a〉〈br〉(Rudolph, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0082.pdf"〉Weitere Untersuchungen mit dem Sanford-Elektrometer〈/a〉〈br〉(Stoppel, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0083.pdf"〉Das Strömungssystem der Luft über Mogadischu〈/a〉〈br〉(Bossolasco, M.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0084.pdf"〉Messungen mit transportablen statischen Schweremessern〈/a〉〈br〉(Schleusener, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0086.pdf"〉Über den Energietransport bei der Sprengseismik〈/a〉〈br〉(v. Schmidt, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0087.pdf"〉Formen der Bodenschwingung bei sinusförmiger Anregung〈/a〉〈br〉(Köhler, R.)〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0088.pdf"〉Die Ausbreitungsgeschwindigkeit sinusförmiger elastischer Wellen im Boden〈/a〉〈br〉(Ramspeck, A.)〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0089.pdf"〉Referate und Mitteilungen〈/a〉〈br〉(Haase, H.)〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0090.pdf"〉Bericht über die elfte Tagung der Deutschen Geophysikalischen Gesellschaft vom 13. bis 15. September 1934 in Bad Pyrmont〈/a〉〈br〉(Jung, K.)〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0091.pdf"〉Berichtigung〈/a〉〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0092.pdf"〉Geophysikalische Berichte〈/a〉〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0093.pdf.pdf"〉Register der Geophysikalischen Berichte〈/a〉〈/li〉 〈li〉〈a href=" https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0010/LOG_0094.pdf"〉Mitgliederverzeichnis der Deutschen Geophysikalischen Gesellschaft nach dem Stande vom 1. Dezember 1934〈/a〉〈/li〉 〈/body〉 〈/html〉

Description: research

Description: DGG, DFG, SUB Göttingen

Description: Deutschlands Erdbebentätigkeit pflegt unterschätzt zu werden, weil sie gewöhnlich so harmlos erscheint. Zwar bringt der Jahresverlauf nur wenige Beben, abgesehen von gelegentlichen Schwärmen mit vielen hunderten von Einzelstößen, wie sie besonders dem Vogtland eigentümlich sind. Zudem handelt es sich dabei vorwiegend um schadlose Erderschütterungen, die kaum Beobachtung finden. Aber der Fachmann kennt daneben auch bis in die neueste Zeit hinein Erdbeben mit erheblichen Schäden und selbst Zerstörungen, die für längere Zeit das öffentliche Leben völlig beherrscht haben; mitunter wurde fast Großbebencharakter erreicht.

Description: research

Description: DFG, SUB Göttingen

Description: Die nachstehenden neueren Untersuchungen auf verschiedenen Gebieten geophysikalischer Forschung, die von Mitgliedern der Reichsanstalt für Erdbebenforschung in Jena durchgeführt sind, wurden erstmalig in der Festschrift zum 70. Geburtstage des früheren Direktors der Reichsanstalt, Herrn Geheimrat Professor Dr. Oskar Hecker (Beitrage zur Angewandten Geophysik, Band 4, Heft 3, Leipzig 1934) veröffentlicht. Sämtliche Arbeiten, ausgenommen diejenigen von Krumbach, gehören zu den von der Notgemeinschaft der Deutschen Wissenschaft unterstützten geophysikalischen Forschungen. A. Sieberg

Description: research

Description: DFG, SUB Göttingen

Description: Am Beispiel des "Leegmoores" im Timpemoor - einem ehemaligen "Heidemoor" - wurde auf Grund von boden- und moorkundlichen Untersuchungen sowie von landeskundlich-historischen Recherchen die Entwicklung der Heidemoore überprüft. Dazu wurden erstmalig die flächenhaften Verluste an Moorsubstanz durch - wiederholte Moorbrandkultur, - Entnahme von Heidesoden (Abplaggen) und - Winderosion qualitativ und quantitativ erfaßt, dazu die Moorsackung errechnet. Aus den vorhandenen moorkundlichen Fakten konnte das natürliche Moorrelief des Timpemoores rekonstruiert werden. Die Autoren weisen nach, daß die von JONAS (1934, 1935) beschriebenen Heidemoore "durch den Menschen beeinflußte Moore" darstellen. Das untersuchte Timpemoor hat sich danach im Verlauf mehrerer Jahrhunderte aus einem natürlichen gewölbten Hochmoor gebildet.

Description: On the basis of pedological, peatland and historical investigations the origin of raised bogs with heather vegetation ("Heidemoore")was examined at the example "Leegmoor", a part of the "Timpemoor". In addition to that for the first time the loss of peat substance by - burnt-over peatland cultivation, - cutaway heather sods, - erosion by wind and - bog subsidence was calculated. With the available peatland facts it was possible to reconstruct the natural bog relief. The authors are able to demonstrate that the "Heidemoore" described by JONAS (1934, 1935) are bogs influenced by man. During the last centuries the Timpemoor developed from a natural raised bog (with convex centre) to a raised bog with heather vegetation.

Description: research

Description: DFG, SUB Göttingen

Description: Vergleichende Darstellung und Analyse der Arbeitsvorgänge in den Agrarlandschaften der Erde. Dieser Aufgabe unterzieht sich in einem ersten Schritt die vorliegende Studie. Sie strebt an, mit der Darstellung und Analyse des jährlichen Arbeitsvorganges die bisher wenig berücksichtigte dynamische Seite der Agrarlandschaft – ihre Rhythmik nämlich – in exakter Weise erfassen zu können. Im Vordergrund steht zunächst weniger die regionale als vielmehr die sachliche Erörterung, auf der Beispielsgrundlage jedoch einer regionalen Kontrastierung innerhalb Deutschlands bzw. aus naheliegenden Gründen der Bundesrepublik Deutschland. Späteren großräumigen Untersuchungen erst kann es vorbehalten sein, von der hier geschaffenen Plattform aus auf eine speziell regionale Betrachtungsweise überzugehen.

Description: research

Description: DFG, SUB Göttingen

Description: An der Hand von Erdbeben, die im Boden Deutschlands entstanden sind, sollen folgende Fragen untersucht werden: 1) Die Wirkungsweise der einzelnen Bebenherde, von denen anzunehmen ist, dass sie verschiedenartige Charaktereigenschaften haben. Hierfür ist es notwendig, festzustellen einmal Lage und geometrisches Bild des Herdes als geologische Störungsstelle, andererseits den das Erdbeben auslösenden Bewegungsvorgang in der Herdstörung. 2) Die Abhängigkeit der scheinbaren Bebenstarken innerhalb des Schüttergebietes von Bodenbeschaffenheit und Tektonik.

Description: research

Description: DFG, SUB Göttingen

Description: Dieser Band enthält 77 Beiträge zu Themengebieten der Physik der festen Erde, des magnetischen und elektrischen Felds der Erde, der Physik der Atmosphäre sowie der Angewandten Geophysik, veröffentlicht durch die Deutsche Geophysikalische Gesellschaft in den Jahren 1930.

Description: 〈html〉 〈body〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0004.pdf"〉Titelseite〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0005.pdf"〉Ein neuer Vierpendelapparat für relative Schweremessungen〈/a〉〈br〉(Meisser, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0007.pdf"〉Geophysikalische Messungen unter Tage〈/a〉〈br〉(Meisser, O., Wolf, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0008.pdf"〉Die ersten Dickenmessungen des grönländischen Inlandeises〈/a〉〈br〉(Sorge, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0010.pdf"〉Die seismische Bodenunruhe in Hamburg und ihr Zusammenhang mit der Brandung〈/a〉〈br〉(Mendel, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0012.pdf"〉Die sonnenbelichteten Nordlichtstrahlen und die Konstitution der höheren Atmosphärenschichten〈/a〉〈br〉(Vegard, L.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0013.pdf"〉Nochmals: Zur Frage der Laufzeitkurven〈/a〉〈br〉(Gutenberg, B.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0014.pdf"〉Erwiderung zur vorstehenden Arbeit von Herrn Prof. Gutenberg〈/a〉〈br〉(Krumbach, G.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0015.pdf"〉Bemerkungen zu der vorstehenden Erwiderung〈/a〉〈br〉(Gutenberg, B.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0016.pdf"〉Einfluß des Mondes auf die erdmagnetischen Elemente in Samoa〈/a〉〈br〉(Fanselau, G.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0017.pdf"〉Ein Diagramm zur Bestimmung der Differenz der Schwerestörung 〈i〉Δg〈/i〉 in zwei Beobachtungspunkten〈/a〉〈br〉(Oserezky, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0018.pdf"〉Zur Ermittlung ausgedehnter Schichten verschiedener Leitfähigkeit〈/a〉〈br〉(Koenigsberger, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0019.pdf"〉Über tägliche erdmagnetische Variationen in zwei Alpentälern〈/a〉〈br〉(Koenigsberger, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0020.pdf"〉Die Wirkung der obersten Erdschicht auf die Anfangsbewegung einer Erdbebenwelle〈/a〉〈br〉(Hasegawa, M.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0021.pdf"〉Über die Elastizität von Gesteinen〈/a〉〈br〉(Breyer, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0023.pdf"〉Über den Horizontalabstand von Pendelstationen〈/a〉〈br〉(Schwinner, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0024.pdf"〉Die Belowsche Methode zur Bestimmung der Wirkung gegebener Massen auf Krümmungsgröße und Gradient, ihre Verallgemeinerung für beliebige Massenformen und ihre Anwendung auf "zweidimensionale" Massenanordnungen〈/a〉〈br〉(Jung, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0028.pdf"〉Harmonische Schwingungen des Untergrundes〈/a〉〈br〉(Köhler, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0029.pdf"〉Mitteilungen〈/a〉〈br〉(Fleming, I. A., Linke, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0030.pdf"〉Über die Ursache der erdmagnetischen Störung im Gebiet der Freien Stadt Danzig〈/a〉〈br〉(Haalck, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0031.pdf"〉Die kontinentalen Verschiebungen von Amerika und Madagaskar〈/a〉〈br〉(Livländer, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0032.pdf"〉Magnetische Vermessung einiger tertiärer Eruptivgänge und -stöcke im sächsischen Elbsandsteingebirge〈/a〉〈br〉(Schulze, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0033.pdf"〉Über die Existenz einer mondentägigen Variation in den Erdströmen〈/a〉〈br〉(Egedal, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0034.pdf"〉Zum Trübungsfaktor〈/a〉〈br〉(Feussner, K., Friedrichs, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0035.pdf"〉Temperature changes between Torsion balance readings in the State of Texas〈/a〉〈br〉(Harris, S.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0036.pdf"〉Über isostatische Schwereanomalien und deren Beziehung zu den totalen Anomalien〈/a〉〈br〉(Jung, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0037.pdf"〉Bemerkungen zu den Ausführungen von H. Jung〈/a〉〈br〉(Ansel, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0038.pdf"〉Mitteilungen〈/a〉〈br〉(Linke, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0040.pdf"〉Wesensgleiche und wesensverschiedene Darstellungen〈/a〉〈br〉(Nippoldt, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0041.pdf"〉Die Säkularvariation in der Rheinpfalz in den Jahren 1850 bis 1928〈/a〉〈br〉(Burmeister, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0042.pdf"〉Größenverhältnis von remanentem zu induziertem Magnetismus in Gesteinen; Größe und Richtung des remanenten Magnetismus〈/a〉〈br〉(Koenigsberger, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0043.pdf"〉Über eine magnetische Anomalie am Lebasee in Ostpommern〈/a〉〈br〉(Reich, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0045.pdf"〉Die Ergebnisse der magnetischen Messungen in der Ostsee in den Jahren 1924 bis 1929〈/a〉〈br〉(v. Gernet-Reval, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0047.pdf"〉Erdmagnetische Messungen in Bulgarien, Mazedonien, Trazien und in der Dobrudja〈/a〉〈br〉(Popoff, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0048.pdf"〉Einige Bemerkungen über erdmagnetische Messungen, welche in Feodossia ausgeführt wurden〈/a〉〈br〉(Palazzo, L.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0049.pdf"〉Possible causes of abnormal polarizations of magnetic formations〈/a〉〈br〉(Heiland, C.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0050.pdf"〉Die geologische Bedeutung der Schaffung einer Isanomalenkarte der magnetischen Vertikalintensität von Deutschland〈/a〉〈br〉(Schuh, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0051.pdf"〉Die innere Genauigkeit von Inklinationsmessungen mit dem Erdinduktor〈/a〉〈br〉(Venske, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0052.pdf"〉Theorie einer neuen galvanischen Waage〈/a〉〈br〉(Bock, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0053.pdf"〉Messungen im Luftschiff〈/a〉〈br〉(Haussmann, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0054.pdf"〉Une modification de l'enregistreur à marche rapide et à petite consommation de papier de Ad. Schmidt pour l'application aux stations de l'Anneé Polaire 1932–1933〈/a〉〈br〉(la Cour, D.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0056.pdf"〉Was sagen uns die Parameter eines Magneten?〈/a〉〈br〉(Fanselau, G.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0057.pdf"〉Über die Herleitung des Potentials des täglichen erdmagnetischen Variationsfeldes〈/a〉〈br〉(Egedal, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0058.pdf"〉Über den Vektor der magnetischen Störungen im aperiodischen Verlauf〈/a〉〈br〉(Keränen, J.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0059.pdf"〉Forschungsmethode über den Zusammenhang zwischen der Sonnenfleckentätigkeit und den erdmagnetischen Störungen〈/a〉〈br〉(Gehlinsch, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0060.pdf"〉Der Temperaturverlauf im Sandboden〈/a〉〈br〉(Süring, R.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0061.pdf"〉Die dominierende Luftdruckwelle des strengen Winters 1928/29〈/a〉〈br〉(Weickmann, L.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0063.pdf"〉Über einige meteorologische Begriffe〈/a〉〈br〉(Tetens, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0066.pdf"〉Über die Feinstruktur des Temperaturgradienten längs Berghängen〈/a〉〈br〉(Wagner, A.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0067.pdf"〉Das unperiodische Element im Tropenklima〈/a〉〈br〉(Knoch, K.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0068.pdf"〉Zur Theorie der Maxwellschen Geschwindigkeitsverteilung in turbulenten Strömungen〈/a〉〈br〉(Ertel, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0069.pdf"〉Wie tief dringen die Polarlichter in die Erdatmosphäre ein?〈/a〉〈br〉(Störmer, C.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0072.pdf"〉Gammastrahlen an Kaliumsalzen〈/a〉〈br〉(Kolhörster, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0073.pdf"〉Über die Form der Fernschallwelle〈/a〉〈br〉(Kühl, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0074.pdf"〉Die Seismizität des Südantillenbogens〈/a〉〈br〉(Tams, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0076.pdf"〉Eine neue württembergische Erdbebenwarte〈/a〉〈br〉(Kleinschmidt, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0077.pdf"〉Über den Zusammenhang zwischen Typhusmorbidität (bzw. Typhusmortalität) und Niederschlagsschwankungen nebst einer Kritik der Brücknerschen Klimaperiode〈/a〉〈br〉(Wenzel Pollak, L.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0079.pdf"〉Über die Abhängikeit der Schwerkraft vom Zwischenmedium〈/a〉〈br〉(Schlomka, T.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0080.pdf"〉On the Determination of the Lunar Atmospheric Tide〈/a〉〈br〉(Chapman, S.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0081.pdf"〉Die Wärmeumsatz durch die Wärmestrahlung des Wasserdampfes in der Atmosphäre〈/a〉〈br〉(Albrecht, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0082.pdf"〉Ein Universal-Induktionsmagnetometer〈/a〉〈br〉(Uljanin, W.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0083.pdf"〉Der große Staubfall vom 26. bis 29. April 1928 in Südosteuropa〈/a〉〈br〉(Stenz, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0085.pdf"〉Ein neues Verfahren der luftelektrischen Raumladungsmessung〈/a〉〈br〉(Wigand, A., Schubert, J., Frankenberger, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0086.pdf"〉Kurze Erwiderung auf Vegards Bemerkungen über sonnenbelichtete Nordlichtstrahlen〈/a〉〈br〉(Störmer, C.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0088.pdf"〉Die Invariabilität und Abstimmung von Minimumpendeln〈/a〉〈br〉(Kohlschütter, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0089.pdf"〉Bemerkung zu der Arbeit "Die Invariabilität und Abstimmung von Minimumpendeln" von E. Kohlschütter〈/a〉〈br〉(Meisser, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0090.pdf"〉Erwiderung〈/a〉〈br〉(Kohlschütter, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0091.pdf"〉Bemerkungen zu der Arbeit von Herrn Dr. O. Meisser: "Ein neuer Vierpendelapparat für relative Schweremessungen"〈/a〉〈br〉(Heiland, C.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0092.pdf"〉Bemerkungen zu den vorstehenden Ausführungen von Herrn Prof. Dr. C. A. Heiland〈/a〉〈br〉(Meisser, O.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0093.pdf"〉Das Epizentrum des südatlantischen Großbebens vom 27. Juni 1929〈/a〉〈br〉(Tams, E.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0094.pdf"〉Seismische Untersuchungen auf dem Pasterzegletscher. I〈/a〉〈br〉(Brockamp, B., Mothes, H.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0096.pdf"〉Bericht über die neunte Tagung der Deutschen Geophysikalischen Gesellschaft vom 11. bis 14. September 1930 in Potsdam〈/a〉〈br〉(Mügge, Linke, F.)〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0097.pdf"〉Autorenverzeichnis〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0098.pdf"〉Sachverzeichnis〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0099.pdf"〉Literaturverzeichnis〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0100.pdf"〉Geophysikalische Berichte〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0101.pdf"〉Register der Geophysikalischen Berichte〈/a〉〈/li〉 〈li〉〈a href="https://gdz.sub.uni-goettingen.de/download/pdf/PPN101433392X_0006/LOG_0102.pdf"〉Mitgliederverzeichnis der Deutschen Geophysikalischen Gesellschaft nach dem Stande vom 1. Oktober 1930〈/a〉〈/li〉 〈/body〉 〈/html〉

Description: research

Description: DGG, DFG, SUB Göttingen

Description: This release note discusses the planetary transit search data products produced by the Science Processing Operations Center at Ames Research Center from Sectors 1-2 observations made with the TESS (Transiting Exoplanet Survey Satellite) spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: In order to observe the lunar sodium exosphere out to one-half degree around the Moon, we designed, built and installed a small robotically controlled coronagraph at the Winer Observatory in Sonoita, Arizona. Observations are obtained remotely every available clear night from our home base at Goddard Space Flight Center or from Prescott, Arizona. We employ an Andover temperature-controlled 1.5-angstrom-wide narrow-band filter centered on the sodium D2 line, and a similar 1.5-angstrom filter centered blueward of the D2 line by 3 angstroms for continuum observations. Our data encompass lunations in 2015, 2016, and 2017, thus we have a long baseline of sodium exospheric calibrated images. During the course of three years we have refined the observational sequence in many respects. Therefore this paper only presents the results of the spring, 2017, observing season. We present limb profiles from the south pole to the north pole for many lunar phases. Our data do not fit any power of cosine model as a function of lunar phase or with latitude. The extended Na exosphere has a characteristic temperature of about 22506750 degrees Kelvin, indicative of a partially escaping exosphere. The hot escaping component may be indicative of a mixture of impact vaporization and a sputtered component.

Description: We present Zwicky Transient Facility (ZTF) observations of the tidal disruption flare AT2018zr/PS18kh reported by Holoien et al. and detected during ZTF commissioning. The ZTF light curve of the tidal disruption event (TDE) samples the rise-to-peak exceptionally well, with 50 days of g- and r-band detections before the time of maximum light. We also present our multi-wavelength follow-up observations, including the detection of a thermal (kT 100 eV) X-ray source that is two orders of magnitude fainter than the contemporaneous optical/UV blackbody luminosity, and a stringent upper limit to the radio emission. We use observations of 128 known active galactic nuclei (AGNs) to assess the quality of the ZTF astrometry, finding a median host-flare distance of 0farcs2 for genuine nuclear flares. Using ZTF observations of variability from known AGNs and supernovae we show how these sources can be separated from TDEs. A combination of light-curve shape, color, and location in the host galaxy can be used to select a clean TDE sample from multi-band optical surveys such as ZTF or the Large Synoptic Survey Telescope.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from the Sector 1-9 transiting planet search with observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: We present multiwavelength observations of the tidal disruption event (TDE) iPTF15af, discovered by the intermediate Palomar Transient Factory survey at redshift z = 0.07897. The optical and ultraviolet (UV) light curves of the transient show a slow decay over 5 months, in agreement with previous optically discovered TDEs. It also has a comparable blackbody peak luminosity of L(sub peak) approx. = 1.5 x 10(exp 44) erg s(exp -1). The inferred temperature from the optical and UV data shows a value of (35) 10(exp 4) K. The transient is not detected in X-rays up to L(sub X) 〈 3 x 10(exp 42) erg s(exp -1) within the first 5 months after discovery. The optical spectra exhibit two distinct broad emission lines in the He ii region, and at later times also H emission. Additionally, emission from [N iii] and [O iii] is detected, likely produced by the Bowen fluorescence effect. UV spectra reveal broad emission and absorption lines associated with high-ionization states of N v, C iv, Si iv, and possibly P v. These features, analogous to those of broad absorption line quasars (BAL QSOs), require an absorber with column densities N(sub H) 〉 10(exp 23) cm(exp -2). This optically thick gas would also explain the nondetection in soft X-rays. The profile of the absorption lines with the highest column density material at the largest velocity is opposite that of BAL QSOs. We suggest that radiation pressure generated by the TDE flare at early times could have provided the initial acceleration mechanism for this gas. Spectral UV line monitoring of future TDEs could test this proposal.

Description: The first measurements of infrared (IR) band intensities of solid dimethyl carbonate are presented along with measurements of this compounds refractive index and density near 15 K, neither of which has been reported. Molar refractions are used to compare these results to other new data from ices made of methyl acetate, acetone, acetic acid, and acetaldehyde, four molecules known to exist in the interstellar medium. Comparisons are made to IR intensities taken from the literature on amorphous ices. The value and importance of comparisons based on molecular structures, to predict and test laboratory results, are highlighted.

Description: We have adapted the algorithmic tools developed during the Kepler mission to vet the quality of transit-like signals for use on the K2 mission data. Using the four sets of publicly available light curves at MAST, we produced a uniformly vetted catalog of 772 transiting planet candidates from K2 as listed at the NASA Exoplanet Archive in the K2 Table of Candidates. Our analysis marks 676 of these as planet candidates and 96 as false positives. All confirmed planets pass our vetting tests. Sixty of our false positives are new identifications, effectively doubling the overall number of astrophysical signals mimicking planetary transits in K2 data. Most of the targets listed as false positives in our catalog show either prominent secondary eclipses, transit depths suggesting a stellar companion instead of a planet, or significant photocenter shifts during transit. We packaged our tools into the open-source, automated vetting pipeline Discovery and Vetting of Exoplanets (DAVE), designed to streamline follow-up efforts by reducing the time and resources wasted observing targets that are likely false positives. DAVE will also be a valuable tool for analyzing planet candidates from NASA's TESS mission, where several guest-investigator programs will provide independent light-curve setsand likely many more from the community. We are currently testing DAVE on recently released TESS planet candidates and will present our results in a follow-up paper.

Description: This release note discusses the planetary transit search data products produced by the Science Processing Operations Center at Ames Research Center from Sectors 1-6 observations made with the TESS (Transiting Exoplanet Survey Satellite) spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: Most violent and energetic processes in our universe, including mergers of compact objects,explosions of massive stars and extreme accretion events, produce copious amounts of X-rays. X-ray follow-up is an efficient tool for identifying transients: (1) X-rays can quickly localize transients with large error circles; (2) X-rays reveal the nature of transients that may not have unique signatures at other wavelengths. Here, we identify key science questions about several extragalactic multi-messenger andmulti-wavelength transients, and demonstrate how X-ray follow-up helps answer these questions.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 3 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: This release note discusses the planetary transit search data products produced by the Science Processing Operations Center at Ames Research Center from Sectors 1-3 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: No abstract available

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 7 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 8 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 4 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 6 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 5 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: On 5 February 2015, a previously unknown meteor shower, the Lyrids were observed for the first time. Because of the Sun-Earth-Moon viewing geometry, however, stream members were observed almost exclusively by the Canadian Meteor Orbit Radar (CMOR). The Lyrids did not appear again until 2018, and that outburst was stronger than in 2015. This study analyzed the 2015 and 2018 CMOR data in order to determine the orbital parameters of the stream in an attempt to determine the Lyrid parent body. Of primary importance is to determine if the Lyrids will recur in a predictable manner. Two bodies, with dramatically different orbital parameters and evolutionary behaviors, emerged as the leading candidates: 2003 EH1 and 1854 R1.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 2 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: Impact cratering is the dominant geo-logic process affecting the surfaces of solid bodies throughout our solar system. Because large impacts are (luckily) rare on Earth, the process is studied through experiments, observations of existing structures, numerical modeling, and theory, most of which make the simplifying assumptions that the target is homogeneous, with no substantial topography. Craters do not always form on level targets com-posed of homogeneous loose material. Rather (Fig. 1), they often form on sloped surfaces and in layered tar-gets, both of which significantly influence the excavation and ejecta deposition processes. Such craters are common on the Moon and asteroids. We are investigating crater formation in two separate suites of experiments using sloped and layered targets (Fig. 2) at the Experimental Impact Laboratory at NASA Johnson Space Center. An experiment was also performed in a flat, homogenous target to serve as a reference.

Description: The Laser Interferometer Space Antenna (LISA), requires high precision displacement measurement between widely spaced pairs of freely floating test masses. We describe a proposed design for the optical telescopes that form an essential part of the laser heterodyne interferometry measurement system and discuss how the design and implementation will address the unique challenges of this specialized application.

Description: X-ray observations are indispensable for understanding the cosmos. Their power is immense because much of the baryonic matter and the sites for the most active energy releases in the Universe are primarily observable in X-rays. For the 2030s and beyond, an X-ray observatory with power matching the capabilities in other wavebands is a necessary discovery engine for full exploration of the Universe. JWST and other upcoming major space- and ground-based facilities are expected to greatly expand science frontiers in the coming decades. is presents both a great opportunity and a challenge for a next-generation X-ray observatory. In many areas, such as tracing black holes during the CosmicDawn and understanding the formation and evolution of galaxies, an X-ray observatory is the logical next step. e challenge is that the X-ray science at these new frontiers requires expansion of capabilities by orders of magnitude beyond the current state of the art or anything already planned. Until recently, such gains were not technologically possible. is has changed thanks to recent breakthroughs and sustained maturation of key technologies for X-ray mirrors and detectors. We are reaping the fruits of U.S. investments in these areas over the past 1015 years. An X-ray observatory that can extend the science frontiers of the post-JWST era is now entirely feasible. Lynx is the mission concept that realizes this vision. It will y revolutionary optics and instrumentation onboard a simple, proven spacecraft. In all aspects, Lynx will be a next-generation Great Observatory that is certain to make a profound impact across the astrophysical landscape. It will provide the depth and breadth to answer the fundamental questions that confront us today; just as importantly, it will have capabilities to address questions we have yet to even ask.

Description: The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of Herschel, the largest telescope flown in space to date. After a 3 year study, the Origins Science and Technology Definition Team will recommend to the Decadal Survey a concept for Origins with a 5.9-m diameter telescope cryo cooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (MISC-T) will measure the spectra of transiting exoplanets in the 2.8 20 m wavelength range and offer unprecedented sensitivity, enabling definitive biosignature detections. The Far-IR Imager Polarimeter (FIP) will be able to survey thousands of square degrees with broadband imaging at 50 and 250 m. The Origins Survey Spectrometer (OSS) will cover wavelengths from 25 588 m, make wide-area and deep spectroscopic surveys with spectral resolving power R ~ 300, and pointed observations at R ~ 40,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The telescope has a Spitzer-like architecture and requires very few deployments after launch. The cryo-thermal system design leverages JWST technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins natural background limited sensitivity.

Description: The purpose of this document is to provide a forecast of major meteor shower activity in low Earth orbit (LEO). Typical activity levels are expected for nearly all showers in 2020; only the Geminids, which are gradually increasing in strength over time, are expected to be stronger than in previous years. No meteor storms or outbursts are predicted for 2020.

Description: The Orbital Debris Program Office at NASA Johnson Space Center has a long history of an optical observational program. The Meter Class Autonomous Telescope, MCAT, was dedicated to Eugene Stansbery (now also known as ES-MCAT) in 2017. MCAT, a 1.3m DFM telescope, has a proven capability for tracking known objects from Low-Earth Orbits (LEO) out to Geosynchronous (GEO) orbits. Monitoring the population of the GEO belt is accomplished through surveys. A GEO survey statistically samples the GEO belt (0 to ~15 deg orbital inclinations) to detect both correlated and uncorrelated targets. A GEO survey, the initial focus for MCAT, will commence in 2019 to map out the current state of the GEO population as input for the ORbital Debris Engineering Model (ORDEM 4.x). If a break-up occurs, surveys of the break-up field can be followed for discovery and investigations of daughter debris fragments from the parent satellite. Discovery can be accomplished by surveying orbits near to and including the parent objects orbit. Targeted observations of debris can be taken with a suite of broadband filters for characterizing individual objects by rate-tracking their known or calculated orbital elements (Two-Line Element sets, TLEs). These observations can be used in conjunction with NASAs Standard Satellite Break-up Model (SSBM). In 2018, MCATs primary mirror was realuminized with a high-end protected, enhanced silver ZeCoat and the CCD chip was replaced in the Spectral Instruments camera. With these updates completed, MCAT is now well on track to reach Full Operational Capability (FOC) in 2019 for its survey and rate-track capabilities. A full overview of MCATs operational state, capabilities, and mission will be discussed.

Description: Outline -Introduction: Fermi Gamma-Ray Burst Monitor (GBM); Gamma-Ray Bursts (GRBs). -GRB 170817A: GBMs most famous GRB; Gamma-ray and Gravitational Wave (GW) Observations; Science from Joint GW/GRB observations; Timeline of follow-up observations. -Similar GRBs in GBM data: GRB 150101B; Other similar GRBs. -What comes next?: Joint GBM and LIGO (Laser Interferometer Gravitational-Wave Observatory) / Virgo (Michelson interferometer operated by a European consortium) observations; Science from new GW/GRB observations; New types of coincident events. -Other types of transient and variable sources observed with Fermi GBM.

Description: Exoplanet science mission concepts require ultra-stable telescopes for multiple hours exposures. Predictive Thermal Control Study (PTCS) matures technology to enable active thermal controlled telescopes required to make ultra-high contrast observations of exoplanets. PTCS' goal is to develop an active thermal control technology that can keep mirrors at a constant temperature (〈 10 mK) regardless of where the telescope points on the sky.

Description: No abstract available

Description: Comet C/2016 R2 (PanSTARRS) has a peculiar volatile composition, with CO being the dominant volatile, as opposed to H2O, and one of the largest N2/CO ratios ever observed in a comet. Using observations obtained with the Spitzer Space Telescope, NASAs Infrared Telescope Facility, the 3.5 m Astrophysical Research Consortium telescope at Apache Point Observatory, the Discovery Channel Telescope at Lowell Observatory, and the Arizona Radio Observatory 10 m Submillimeter Telescope, we quantified the abundances of 12 different species in the coma of R2 PanSTARRS: CO, CO2, H2O, CH4, C2H6, HCN, CH3OH, H2CO, OCS, C2H2, NH3, and N2. We confirm the high abundances of CO and N2 and heavy depletions of H2O, HCN, CH3OH, and H2CO compared to CO reported by previous studies. We provide the first measurements (or most sensitive measurements/constraints) on H2O, CO2, CH4, C2H6, OCS, C2H2, and NH3, all of which are depleted relative to CO by at least 12 orders of magnitude compared to values commonly observed in comets. The observed species also show strong enhancements relative to H2O, and, even when compared to other species like CH4 or CH3OH, most species show deviations from typical comets by at least a factor of 23. The only mixing ratios found to be close to typical are CH3OH/CO2 and CH3OH/CH4. The CO2/CO ratio is within a factor of 2 of those observed for C/1995 O1 (Hale- Bopp) and C/2006 W3 (Christensen) at a similar heliocentric distance, though it is at least an order of magnitude lower than many other comets observed with AKARI. While R2 PanSTARRS was located at a heliocentric distance of 2.8 au at the time of our observations in 2018 January/February, we argue, using sublimation models and comparison to other comets observed at similar heliocentric distance, that this alone cannot account for the peculiar observed composition of this comet and therefore must reflect its intrinsic composition. We discuss possible implications for this clear outlier in compositional studies of comets obtained to date and encourage future dynamical and chemical modeling in order to better understand what the composition of R2 PanSTARRS tells us about the early solar system.

Description: No abstract available

Description: Properly assessing the asteroid threat depends on the knowledge of asteroid pre-entry parameters, such as size, velocity, mass, density, and strength. Although a vast number of possible bodies to study exist, such characterization of asteroid populations is currently limited by substantial costs associated with space rendezvous missions and rare meteorite findings. As asteroids fragment, ablate, and decelerate in the atmosphere, they emit light detectable by ground-based and space-borne instruments. Earths atmosphere, thus, becomes an accessible laboratory that enables impactor risk assessments by facilitating inference of the pre-entry parameters. These asteroid pre-entry conditions are typically deduced by modeling the entry and breakup physics that best reproduce the observed light or energy deposition curve. However, this process requires extensive manual trial-and-error of uncertain modeling parameters. Automating meteor modeling and inference would improve property distributions used in risk assessments and enable population characterization as more light curves become more readily available through the presence of space assets and ground-based camera networks. We previously developed a genetic algorithm to automate meteor modeling by using the fragment-cloud model (FCM) to search for the values of the FCM input parameters (e.g., diameter) that generate energy deposition profiles that match the observed one. Now, we apply deep learning to infer asteroid diameter, velocity, and density from observed energy deposition curves. We trained and tested our neural network models with synthetic energy deposition curves modeled using the FCM rubble pile implementation. We present an application of a 1D convolutional neural network and compare its performance to other attempted regressors and machine learning techniques, such as a fully connected neural network and Random Forest regression, to demonstrate its capabilities. We validate our model weights and approach using the Chelyabinsk, Tagish Lake, Beneov, Koice, and Lost City meteors.

Description: Exoplanet Transmission Spectroscopy with LUVOIR

Description: In Section 1 we summarize the technological approaches to the Large Balloon Reflector (LBR) that are discussed at length in our Phase I Technical report. Within each subsection we highlight how the work was advanced in Phase II. In Section 2 the work and lessons learned from the 3 and 5 meter LBR prototypes are described. In Section 3 the LBR Sensor Package stratospheric flight is described. Section 4 puts LBR in the context of on-going NASA missions.In Sections 5 and 6 the dissemination of results and plans to realize a stratospheric LBR are discussed. Instead of attempting to maintain the pointing of a large telescope at the end of a tether, we propose to deploy a telescope in the benign, protected environment within the carrier balloon. The telescope is itself a balloon, spherical in shape, metalized on one side and anchored to the top of the carrier balloon via a rotating azimuth plate (see Figure 2). The carrier balloon serves as both a stable mount and a radome for the inner balloon reflector. Light from space (or the atmosphere or ground) first passes through the ~2 mil thick polyethylene skin of the carrier balloon and then through the ~1 mil thickMylar side of the inner balloon. Together these layershave 〈 8% absorption at the wavelengths of interest.The incoming light then encounters the aluminized,spherical, back surface of the inner balloon and isthen focused into a receiving system. To achieve the performance of a 10 meter parabolic reflector, a 20 meter diameter inner balloon can be used with a modest size (~1 meter) spherical corrector.

Description: Short-period sub-Neptunes with substantial volatile envelopes are among the most common type of known exoplanets. However, recent studies of the Kepler population have suggested a dearth of sub-Neptunes on highly irradiated orbits, where they are vulnerable to atmospheric photoevaporation. Physically, we expect this "photoevaporation desert" to depend on the total lifetime X-ray and extreme ultraviolet flux, the main drivers of atmospheric escape. In this work, we study the demographics of sub-Neptunes as a function of lifetime exposure to high-energy radiation and host-star mass. We find that for a given present-day insolation, planets orbiting a 0.3 solar mass star experience approximately 100 times more X-ray flux over their lifetimes versus a 1.2 solar mass star. Defining the photoevaporation desert as a region consistent with zero occurrence at 2 sigma, the onset of the desert happens for integrated X-ray fluxes greater than 1.43 times 10 (sup 22) to 8.23 times 10 (sup 20) as a function of planetary radii for 1.8 to 4 Earth radius. We also compare the location of the photoevaporation desert for different stellar types. We find much greater variability in the desert onset in the bolometric flux space compared to the integrated X-ray flux space, suggestive of photoevaporation driven by steady-state stellar X-ray emissions as the dominant control on desert location. Finally, we report tentative evidence for the sub-Neptune valley, first seen around Sun-like stars, for M&K dwarfs. The discovery of additional planets around low-mass stars from surveys such as the Transiting Exoplanet Survey Satellite (TESS) mission will enable detailed exploration of these trends.

Description: Summary: GW170817 / GRB 170817A is one of the best observed transient and highlights the science impact of multi-messenger observations; Many open questions remain, with increased GW (Gravitational Wave) interferometer sensitivity, there will be more joint detections with GBM (Gamma-ray Burst Monitor), enabling deeper population studies of SGRBs (Short Gamma-Ray Bursts) -Additional distance measures which yield source energetics -Constrain jet structure and opening angle distribution -Cocoon emission from SGRBs -Causes of precursor and extended emission -Rates of SGRBs in the universe with implications for source evolution; Fermi GBM is currently the most prolific short GRB detector -Subthreshold searches are crucial to increasing GBM sensitivity and the detection horizon to weakevents like GRB 170817A; Looking forward to future multimessenger discoveries -Neutron star...Black hole merger, neutrinos, Fast Radio Bursts?

Description: We have performed a comprehensive spectral and timing analysis of the first NuSTAR observation of the high-mass X-ray binary 4U 1538522. The observation covers the X-ray eclipse of the source, plus the eclipse ingress and egress. We use the new measurement of the mid-eclipse time to update the orbital parameters of the system and find marginally significant evolution in the orbital period, with P(sub orb) / P(sub orb) = (-0.95 +/- 0.37) x 10(exp -6) yr(exp -1). The cyclotron line energy is found to be approximately 1.2 keV higher than RXTE measurements from 1997 to 2003, in line with the increased energy observed by Suzaku in 2012 and strengthening the case for secular evolution of 4U 1538522's CRSF. We additionally characterize the behavior of the iron fluorescence and emission lines and line-of-sight absorption as the source moves into and out of eclipse.

Description: No abstract available

Description: Recent development in coating deposition processes for aluminum mirrors that are protected with a metal-fluoride overcoat (such as LiF, MgF2, or LiF) have improved reflectance.

Description: The 1.3m ES-MCAT telescope (or MCAT for short) now has a proven capability for observing objects from Low- Earth Orbit (LEO) out to Geosynchronous (GEO) orbit, and the ability to run all systems autonomously. A GEO survey, the initial focus for MCAT, will commence in late 2019 to map out the current state of the GEO population as input for the ORbital Debris Engineering Model (ORDEM 4.x). This survey will statistically sample the GEO belt (0 to ~15 deg orbital inclinations) to detect both known and unknown targets. If a break-up occurs, additional surveys of the break-up field can be followed for discovery and investigations of daughter debris fragments from the parent satellite. Discovery can be accomplished by tracking orbits near to and including the parent objects orbit. Targeted observations of debris can be taken with a suite of broadband filters for characterizing individual objects by ratetracking their known or calculated orbital elements (Two-Line Element sets, TLEs). Several modifications and upgrades have been made to the instrumentation and systems originally installed in 2015 and are reported here. In 2018, MCATs primary mirror was recoated with a high-end protected, enhanced silver by the ZeCoat Corporation. The CCD chip was replaced in the Spectral Instruments camera with a broad-band antireflective coated chip. The automated weather systems have been modified from the original system, removing some weather sensors and installing replacements that are better suited to Ascensions weather and environment. A new 2.5-m ObservaDome replaced the Astrohaven dome on the nearby tower platform that will house an auxiliary 0.4-meter telescope. Finally, in 2019, the Observatory Control System was upgraded to 2.0 which includes additional flexibility for automating data collection and reduction. With these updates completed, MCAT is now well on track to reach Full Operational Capability (FOC) in 2019 for its survey, rate-track, and TLE tracking capabilities.

Description: Abstract: Current information on the potential distribution and condition of peatland soils are of great importance. This applies notably for actions with respect to climate and environmental protection. The Ministry of infrastructure and agriculture in the federal state of Brandenburg (MIL) therefore initiated a project to provide a complete and updated map of peatland soils for the federal state of Brandenburg, Germany, for the year 2013. Extensive legacy data on both, areal extent of peatland soils as well as soil profile information where made digitally available in a homogeneous map and a consistent database. Approximately 7.725 sites were randomly selected from legacy soil data and currently reinvestigated to draw inference on the current condition of peatland soils. Statistically derived peatland subsidence rates at grassland sites of 0.50 cm/yr and 0.57 cm/yr at arable sites fit well with published values in comparable regions of central Europe. Our results prove the great dynamics of soil development on agriculturally used peatlands. Concerning Brandenburg, the area of peatland soils decreased from 270.000 ha in the early 20th century (Prussian geological map) to actually 163.000 ha.

Description: Zusammenfassung: Aktuelle Informationen zur Verbreitung und zum Zustand der Moorböden sind vor dem Hintergrund der geplanten Einführung von Agrarumwelt- und Klimamaßnahmen in der Landwirtschaft von besonderer Bedeutung. Das Ministerium für Infrastruktur und Landwirtschaft des Landes Brandenburg (MIL) hat hierzu das Projekt „Schaffung einer Datengrundlage für die Ableitung von Agrarumwelt- und Klimamaßnahmen auf Moorstandorten in Brandenburg“ initiiert. Mit dem Ziel der Bereitstellung einer auf das Jahr 2013 bezogenen Moorkarte wurden umfangreiche, bis dato nicht genutzte Datenbestände zur Verbreitung von Moorböden in Brandenburg zu einer überschneidungsfreien Karte und umfassenden Datenbank moorbodenkundlicher Bodenprofile verarbeitet. Um den aktuellen Zustand der Moorböden zu erfassen, wurden flächenrepräsentativ und zufällig an 7.725 Standorten mit ausreichender Datenbasis erneut bodenkundliche Erhebungen durchgeführt und statistisch ausgewertet. Im Ergebnis konnten Mächtigkeitsverlustraten für landwirtschaftlich genutzte Moorstandorte in Brandenburg abgeleitet werden. Für flachgründige Niedermoorstandorte unter Grünland liegen sie bei 0,50 cm/a, vergleichbare ackerbaulich genutzte Standorte liegen mit 0,57 cm/a darüber. Dies deckt sich gut mit publizierten Werten an vergleichbaren Standorten in Zentraleuropa. Die Fläche der Moorböden in Brandenburg hat sich von Anfang des 20. Jahrhunderts von 270.000 ha, ausgewiesen auf Basis der Preußisch geologisch-agronomische Karte (PGK), auf heute noch 163.000 ha reduziert.

Description: DFG, SUB Göttingen, DGMT

Description: research

Description: Abstract: Peatlands are intensively exchanging greenhouse gases with the free atmosphere. Natural peatlands, mires, sequester carbon dioxide as carbon in the peat and emit methane. Peatlands under agriculture or forest are mostly drained and emit carbon dioxide due to peat mineralization and nitrous oxide due to fertilization and nitrogen mineralization. In order to characterize the actual situation and to evaluate measures for the reduction of greenhouse gas emissions measured values on gas exchange are needed. Within two national projects direct measurements of the greenhouse gas exchange have been conducted on a wide range of sites, covering different peatland types, land use forms and hydrological situations and using a standardized methodology. Between 2007 and 2012 22 sites have been studied in Lower Saxony over at least two years using the closed cover method. An overview on sites and results is given. Moreover, approaches to estimate the greenhouse gas emissions due to peat excavation and horticultural peat use are presented. Own emission factors and data from literature are used to estimate the contribution of peatlands and peat use to the greenhouse gas emissions of Lower Saxony. Finally measures for the reduction of greenhouse gas emissions are discussed and estimates on reduction costs are given from examples.

Description: Zusammenfassung: Moore stehen in einem intensiven Gasaustausch mit der Atmosphäre. Natürliche Moore haben über Jahrtausende Kohlendioxid aufgenommen und den Kohlenstoff als Torf gespeichert. Dabei haben sie Methan abgegeben. Entwässerte und genutzte Moore setzen den Kohlenstoff als Kohlendioxid wieder frei und emittieren zudem klimarelevantes Lachgas als Ergebnis der Stickstoffdüngung und der Torfmineralisation. Zur Charakterisierung der Ist-Situation und zur Beurteilung von Maßnahmen ist es erforderlich, belastbare Daten über die Treibhausgasemissionen der Moore zu haben. Im Rahmen von zwei bundesweit angelegten Verbundvorhaben wurden an einer Vielzahl von Standorten unterschiedlichen Moortyps, unterschiedlicher Nutzung und unterschiedlicher Klima- und Wasserregime mit einer abgestimmten Methodik die Flüsse der wesentlichen Treibhausgase direkt gemessen. Im Rahmen dieser Verbundvorhaben wurden in Niedersachsen zwischen 2007 und 2012 an 22 Standorten mindestens zweijährige Messungen mit der Haubentechnik vorgenommen. Dieser Beitrag gibt einen Überblick über untersuchte Standorte und Messergebnisse. Darüber hinaus werden Ansätze zur Ermittlung der Treibhausgasemissionen aus der industriellen Torfgewinnung dargestellt. Unter Verwendung eigener Ergebnisse und von Literaturdaten wird eine Abschätzung der Treibhausgasemissionen aus Moor und Torfgewinnung für das Land Niedersachsen vorgenommen. Abschließend geht der Beitrag auf Maßnahmen zur Verminderung der Treibhausgasemissionen aus Mooren sowie beispielhaft auf Emissionsminderungskosten ein.

Description: DFG, SUB Göttingen, DGMT

Description: research

Description: STÄBLEIN, G.: Regionale Geomorphologie ; KERTESZ, A.: Geomorphologische Kartierung in der Bundesrepublik Deutschland und in Ungarn. Ein Vergleich der Methodik ; BOLLMANN, I.: Geomorphologische Daten und kartographische Darstellung ; PACHUR, H.-J. & RÖPER, H.-P.: Geolimnologische Befunde des Berliner Raumes ; REMMELE, G.: Holozäne Morphodynamik an Schichtstufenhängen — Untersuchungen in Nordwest-Irland ; MÜLLER, MJ. & STRASSER, R.: Holozäne Geomorphodynamik und Landschaftsentwicklung am Ostrand der Trier-Luxemburger Mulde ; KLEBER, A.: Zur jungtertiären Reliefentwicklung im Vorland der südlichen Frankenalb ; HAMANN, C.: Windwurf als Ursache der Bodenbuckelung am Südrand des Tennengebirges, ein Beitrag zur Genese der Buckelwiesen ; ZÖLLER, L.: Neotektonik am Hunsrückrand ; SEPPÄLÄ, M.: Glazialhydrologie des Inlandeises, eine geomorphologische Interpretation der Verhältnisse in Finnland ; JÄKEL, D.: Untersuchungen und Analysen zur Entstehung der Hamada ; GARLEFF, K. & STINGL, H.: Neue Befunde zur jungquartären Vergletscherung in Cuyo und Patagonien ; STINGL, H. & GARLBFF, K.: Tertiäre und pleistozäne Reliefentwicklung an der interozeanischen Wasserscheide in Südpatagonien (Gebiet von Rio Turbio, Argentinien) ; SCHMIDT, K.H.: Nachweis junger Krustenbewegungen auf dem Colorado Plateau, USA ; KUHLE, M.: Zur Geomorphologie Tibets, Bortensander als Kennformen semiarider Vorlandvergletscherung . ; STÄBLEIN, G.: Deutscher Arbeitskreis für Geomorphologie ;

Description: research

Description: DFG, SUB Göttingen, FU Berlin

Description: Abstract: In addition to the widespread use of peatlands for agricultural purposes, which is also common in other German states, the raised bogs in Lower Saxony are still also used up to the present day for housing, as well as for industrial peat extraction. The Peatland Conservation Programme in Lower Saxony launched in 1981 therefore only covered raised bogs to disentangle the different uses, and to systematise the nature protection activities in raised bogs. The priority areas for the extraction of peat defined in the Federal State Regional Planning Programme are to be rescinded. The new State Development Programme being formulated will not only include the nature conservation of peatlands, but also for the first time, deal with the climate protection afforded by these very important storage areas for carbon. An important aspect in this regard is the incorporation of fens, and the discharge from peatlands into underlying water bodies. The database and the conclusions which contribute to the implementation of climate protection in peatland conservation programmes, will be discussed and compared with the peatland conservation previously implemented pursuant to the Peatland Conservation Programme in Lower Saxony. An overview describes various approaches for peatland and climate protection implemented by private initiatives, nature conservation societies, EU-Life-Projects, contractual nature protection, publicly owned businesses and authorities in Lower Saxony, research projects on alternative uses, and climate certificate trading. These varied instruments are compared to highlight their relative areal effectiveness, and relevance, followed by an estimate of the potential for future peatland and climate protection in Lower Saxony.

Description: Zusammenfassung: Neben der auch in anderen Bundesländern weit verbreiteten landwirtschaftlichen Nutzung von Mooren werden die niedersächsischen Hochmoore bis heute auch als Siedlungsraum und zur industriellen Torfgewinnung genutzt. Daher umfasste das niedersächsische Moorschutzprogramm von 1981 nur die Hochmoore, um diese verschiedenen Nutzungen zu entflechten und den Naturschutz in Hochmooren zu systematisieren. Die bisher im Landesraumordnungsprogramm ausgewiesenen Vorranggebiete für die Rohstoffgewinnung von Torf sollen gestrichen werden. In ein neu aufzustellendes Landesentwicklungsprogramm soll neben dem Naturschutz von Mooren erstmalig auch der Klimaschutz dieser wichtigen Kohlenstoffspeicher eingehen. Von besonderer Bedeutung sind hierbei die Einbeziehung der Niedermoore und der Stoffaustrag aus Mooren in unterliegende Gewässer. Die Datengrundlagen und Schlussfolgerungen, die zur Implementierung des Klimaschutzes in den Moorschutz beitragen, werden diskutiert und mit dem bisher umgesetzten Moorschutz nach dem niedersächsischen Moorschutzprogramm verglichen. Ein Überblick beschreibt verschiedene Ansätze zum Moor- und Klimaschutz von Privatinitiativen, von Naturschutzverbänden, mit EU-Life-Projekten, im Vertragsnaturschutz, von niedersächsischen Landesbetrieben und Behörden, von Forschungsprojekten zu alternativen Nutzungen und beim Handel mit Klima-Zertifikaten. Diese unterschiedlichen Instrumente werden in ihrer Flächenwirksamkeit und Relevanz in Beziehung gesetzt und das Potenzial für den künftigen Moor- und Klimaschutz in Niedersachsen abgeschätzt.

Description: DFG, SUB Göttingen, DGMT

Description: research

Description: V350 Sgr is a classical Cepheid suitable for mass determination. It has a hot companion which is prominent in the ultraviolet (UV) and which is not itself a binary. We have obtained two high-resolution echelle spectra of the companion at orbital velocity maximum and minimum with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope in the 1320 to 1510 region. By cross-correlating these spectra we obtained the orbital velocity amplitude of the companion with an uncertainty in the companion amplitude of 1.9 km s(exp 1). This provides a mass ratio of the Cepheid to the companion of 2.1. The UV energy distribution of the companion provides the mass of the companion, yielding a Cepheid mass of 5.2 0.3 solar mass. This mass requires some combination of moderate main sequence core convective overshoot and rotation to match evolutionary tracks.

Description: We present 15 high-mass X-ray binary (HMXB) candidates in the disk of M31 for which we are able to infer compact object type, spectral type of the donor star, and age using multiwavelength observations from NuSTAR, Chandra, and the Hubble Space Telescope. The hard X-ray colors and luminosities from NuSTAR permit the tentative classification of accreting X-ray binary systems by compact object type, distinguishing black hole from neutron star systems. We find hard-state black holes, pulsars, and non-magnetized neutron stars associated with optical point-source counterparts with similar frequency. We also find nine non-magnetized neutron stars coincident with globular clusters and an equal number of pulsars with and without point-source optical counterparts. We perform spectral energy distribution (SED) fitting for the most likely optical counterparts to the HMXB candidates, finding seven likely high-mass stars and one possible red helium-burning star. The remaining seven HMXB optical counterparts have poor SED fits, so their companion stars remain unclassified. Using published star formation histories, we find that the majority of HMXB candidatesX-ray sources with UV-bright point-source optical counterpart candidatesare found in regions with star formation bursts less than 50 Myr ago, and three are associated with young stellar ages (〈10 Myr). This is consistent with similar studies of HMXB populations in the Magellanic Clouds, M33, NGC 300, and NGC 2403.

Description: The OSIRIS-REx spacecraft launched on September 8, 2016, on a seven-year journey to return samples from asteroid (101955) Bennu. This presentation summarizes the scientific results from the Approach and Preliminary Survey phases. Bennu observations are set to begin on August 17, 2018,when the asteroid is bright enough for detection by the PolyCam. PolyCam and MapCam collect data to survey the asteroid environment for any hazards and characterize the asteroid point-source photometric properties. Resolved images acquired during final approach, starting in late October 2018, allow the creation of a shape model using stereophotoclinometry (SPC), needed by both the navigation team and science planners. The OVIRS and OTES spectrometers characterize the point- source spectral properties over a full rotation period, providing a first look at any features and thermophysical properties. TAGSAM is released from the launch container and deployed into the sampling configuration then returned to the stow position.Preliminary Survey follows the Approach Phase in early December 2018. This phase consists of a series of hyperbolic trajectories that cross over the North and South poles and the equator of Bennu at a close-approach distance of 7 km. Images from these Preliminary Survey passes provide data to complete the 75-cm resolution SPC global shape model and solve for the rotation state. Once the shape model is complete, the asteroid coordinate system is defined for co-registration of all data products. These higher-resolution images also constrain the photometric properties and allow for an initial assessment of the geology. In Preliminary Survey the team also obtains the first OLA data, providing a measure of the surface topography. OVIRS and OTES collect data as "ride-along" instruments, with the spacecraft pointing driven by imaging constraints. These data provide a first look at the spectral variation across the surface of Bennu. Radio science measurements, combined with altimetry and imagery, determine Bennu's mass, a prerequisite to placing the spacecraft into orbit in late December 2018. Together, data from the Approach and Preliminary Survey phases set the stage for the extensive mapping planned for 2019. These dates are the baseline plan. Any contingency or unexpected discovery may change this mission profile.

Description: Clouds and hazes are commonplace in the atmospheres of solar system planets and are likely ubiquitous in the atmospheres of extrasolar planets as well. Clouds affect every aspect of a planetary atmosphere, from the transport of radiation, to atmospheric chemistry, to dynamics and they influence - if not control - aspects such as surface temperature and habitability. In my presentations I aim to provide an introduction to the role and properties of clouds in exoplanetary atmospheres and will discuss the lessons learned from the past two decades of studying clouds in brown dwarf atmospheres. I will consider the role clouds play in influencing the spectra of extrasolar giant planets and will discuss the relative simple approaches that have been taken so far to model exoplanet clouds. I will also review how the scattering and extinction efficiencies of cloud particles may be approximated in certain limiting cases of small and large particles in order to facilitate physical understanding and will discuss the need for optimized cloud models that can be applied to exoplanet transmission spectra. Finally I will discuss the various sources of aerosol opacity, including photochemistry, disequilibrium chemistry, and equilibrium condensation.

Description: Meteor showers occur when the Earth encounters a stream of particles liberated from the surface of a comet or, more rarely, an asteroid. Initially, meteoroids follow a trajectory that is similar to that of their parent comet but modified by both the outward flow of gas from the nucleus and radiation pressure. Sublimating gases impart an "ejection velocity" to solid particles in the coma; this ejection velocity is larger for smaller particles but cannot exceed the speed of the gas itself. Radiation pressure provides a repulsive force that, like gravity, follows an inverse square law, and thus effectively reduces the central potential experienced by small particles. Depending on the optical properties of the particle, the speed of the particle may exceed its effective escape velocity; such particles will be unbound and hence excluded from meteoroid streams and meteor showers. These processes also modify the heliocentric distance at which meteoroid orbits cross the ecliptic plane, and can thus move portions of the stream out of range of the Earth. This talk presents recent work on these components of the early evolution of meteoroid streams and their implications for the meteoroid environment seen at Earth.

Description: NASA's Kepler spacecraft, launched in 2009, has been a resounding success. More than 4000 planet candidates have been identified using data from Kepler primary mission, which ended in 2013, and greater than 2000 of these candidates have been verified as bona fide exoplanets. After the loss of two reaction wheels ended the primary mission, the Kepler spacecraft was repurposed in 2014 to observe many fields on the sky for short periods. This new mission, dubbed K2, has led to the discovery of greater than 600 planet candidates, approximately 200 of which have been verified to date; most of these exoplanets are closer to us than the majority of exoplanets discovered by the primary Kepler mission. TESS, launching in 2018, will survey most of the sky for exoplanets, with emphasis on those orbiting nearby and/or bright host stars, making these planets especially well-suited for follow-up observations with other observatories to characterize atmospheric compositions and other properties. More than one-third of the planet candidates found by NASA's are associated with target stars that have more than one planet candidate, and such 'multis' account for the majority of candidates that have been verified as true planets. The large number of multis tells us that flat multiplanet systems like our Solar System are common. Virtually all of the candidate planetary systems are stable, as tested by numerical integrations that assume a physically motivated mass-radius relationship. Statistical studies performed on these candidate systems reveal a great deal about the architecture of planetary systems, including the typical spacing of orbits and flatness. The characteristics of several of the most interesting confirmed Kepler & K2 multi-planet systems will also be discussed.

Description: We demonstrate KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR8799, using PyKLIP. We report new and re-reduced spectrophotometry of HR8799 c, d, and e from H-K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting fake sources and recovering them over a range of parameters. The K1/K2 spectra for planets c and d are similar to previously published results from the same dataset. We also present a K band spectrum of HR8799e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We compare planets c, d, and e with M, L, and T-type field objects. All objects are consistent with low gravity mid-to-late L dwarfs, however, a lack of standard spectra for low gravity late L-type objects lead to poor fit for gravity. We place our results in context of atmospheric models presented in previous publications and discuss differences in the spectra of the three planets.

Description: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 1 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.

Description: Carbonaceous materials are a primary compo-nent of interstellar dust, forming in the outflow of carbon stars and the diffuse interstellar me-dium (DISM). Over time, the low density DISM is swept into dense molecular clouds, the principal formation sites and repositories of most interstellar molecules. Organic com-pounds created in these clouds are the first step towards the complex materials that help to make planets habitable. Ground- and space-based telescopic observations trace interstellar organics from the diffuse to dense interstellar clouds, revealing that organic material in the diffuse ISM is predominantly hydrocarbon in nature, possessing little N or O, with the C distributed between the aromatic and aliphatic forms. A remarkable similarity between the hydrocarbons in dust in our Galaxy to that of distant galaxies, indicates that this organic component of the DISM is widespread and may be an important universal reservoir of prebiotic organic carbon. Spectroscopy of background stars seen through quiescent dust in clouds with no star formation activity re-veals that chemistry occurs early-on. Mean-while, observations of certain asteroids, com-ets, interplanetary dust particles, planets and planetary satellites present an intricate inter-weaving of preserved interstellar components and those that have been subsequently altered. The composition ofinterstellar dust grains and the evolution of dust between dense clouds (where stars and planetary systems form) and the diffuse inter-stellar medium (where stardust components are ejected), will be presented in this workshop on Carbon in the Solar System.

Description: Organic matter exists in comets (most notably in 81P/Wild 2 [Stardust], 67P/Churyomov- Gerasimenko (67P/C-G) [Rosetta], chondritic porous IDPS, and UCAMMs) and in primitive carbonaceous chondrites that likely retain some chemistry that reflects an origin in the prenatal cold molecular cloud (Alexander+2017). Heavy isotopic enrichments, 15N/14N and possibly D/H, signify preserved molecular cloud organics. In the cold outer disk, if grains are lofted above the disk mid-plane then organics likely experience significant UV processing (Ciesla+2012). In remote sensing of comet comae, organics in the dust are considered refractory or semirefractory. Semi-refractory organics have limited comae lifetimes and produce distributed sources of molecules (H2CO and CO). Rosetta's close passes of 67P/C-G's nucleus (10-15 km) reveals a distributed source of glycine, methyl amine and ethylamine (Altwegg+2016). Cometary samples and primitive meteorites have two types of organic matter: (1) acid-insoluble organic matter (IOM), which is a macromolecular polymer with a mixture of aromatic and aliphatic moieties, and (2) labile, soluble organics, which includes the amino acids, such as glycine (Stardust, Elsila+2009). Meteoritic IOM is robust, withstanding experimental temperatures of 1200 K (Dobrica+2011, Cody+2008). Nanoglobules are a type of IOM; they have a distinct physical structure, but often share the same chemistry as the other IOM from the same meteorite. Moderate-sized PAHs (20 C-atoms) are detected in Stardust samples (Clemett+2010). Refractory organic IOM is ubiquitous yet has a great diversity of abundances between cometary samples. IOM is in primitive chondrites, 67P/C-G (Rosetta), 81P/Wild 2 (Stardust), 1P/Halley, 26P/Grigg-Skjellerup, UCAMMs, anhydrous IDPs, and in chondritic porous IDPs (CP IDPs) and larger cluster IDPs (e.g., Fray+2016, Fomenkova+94, Busemann+ 09, Dobrica+2011, Dobrica+2012). 81P's refractory organic matter is of two types (De Gregorio+2011): nanoglobules of highly aromatic refractory organic matter and polyaromatic carbonyl-containing organic matter, which is similar to IOM in primitive meteorites and IDPs. Fray+2017 estimate that 50% of carbon in 67P/C-G is in IOM. 67P/C-G's organics appear to lack the soluble organic matter, aliphatic carbon, amino acids, and PAHs (Fray+2016). Other notable aspects of the diversity in IOM in cometary samples are the ranges of atomic ratios of N/C, O/C, and H/C, and the range of isotopic enrichments of 15N/14N and D/H. Aqueous and thermal processing on asteroids changes the balance of soluble to insoluble organics, and may be important for diversifying the range of OM delivered to Earth.

Description: The Alpha Centauri system contains the Solar System's closest stellar neighbors. If an earth-like planet is present in the system, it could in principle be detected using a small space-based telescope. As Alpha Centauri is billions of years old, planets are only expected to be found in regions where their orbits are long-lived. We evaluate the extent of the regions within the Alpha Centauri AB system where small planets are able to orbit for billion-year timescales, as well as how closely-spaced planetary orbits can be within those regions in which individual planets can survive. Individual planets on nearly circular, coplanar orbits can survive throughout the habitable zones of both stars. However, perturbations from the companion star imply that the spacing of such planets in multi-planet systems must be significantly larger than the spacing of similar systems orbiting single stars in order to be long-lived. Because the binary companion induces a forced eccentricity upon the orbits of planets in orbit around either star, appropriately-phased circumstellar orbits with small initial eccentricities are stable to slightly larger initial semi-major axes than are initially circular orbits. Small initial eccentricities have a much larger effect on how closely planetary orbits can be spaced. Our results are of special interest as they can guide observers designing instrumentation and search strategies to attempt to discover planets orbiting the nearest sun-like stars. Results remain significantly higher than for planets orbiting single stars.

Description: NASA's New Horizons mission acquired a large set of images and other data making possible thorough geological analysis of landscapes in the Pluto System. Pluto and Charon exhibit strikingly different surface appearances, despite their similar densities and presumed bulk compositions. Systematic investigation, modelling and mapping revealed that much of Pluto's surface is attributed to surface-atmosphere interactions and the mobilization of volatile ices by insolation. Many mapped valley systems appear to be the consequence of glaciation involving nitrogen ice. Other geological activity requires or required long periods of internal heating, such as Pluto's extensive tectonic fabric. The convection and advection of volatile ices in Sputnik Planitia are thought to be powered by present-day radiogenic heat loss. The prominent mountains at the western margin of Sputnik Planitia, and the strange, multi-km-high mound features to the south, probably composed of H2O, are young geologically as inferred by light cratering and superposition relationships. These multi-km-high mound features might be cryo-volcanoes. Their origin, and what drove their formation so late in Solar System history, is under investigation. East of Sputnik Planitia are large fields of aligned ranks of sharp-crested ridges found only at high altitude that are apparently composed of massive deposits of CH4 ice, referred to as Bladed Terrain. New Horizons found evidence that Bladed Terrain may cover much of Pluto's low latitudes and may have originally formed there as a consequence of Pluto's very high obliquity. Currently Bladed Terrain is undergoing net erosion. This observation, along with evidence for formally more extensive nitrogen glaciation implies that Pluto undergoes significant climate evolution. The dynamic remolding of landscapes by volatile transport seen on Pluto is not unambiguously evident in the mapping of Charon. Charon does, however, display a large resurfaced plain and globally engirdling extensional tectonic network attesting to its early endogenic vigor.

Description: Although there are a large number of known exoplanets, there is little data on their global atmospheric properties.Phase-resolved spectroscopy of transiting planets - continuous spectroscopic observation of planets during their full orbits - probes varied depths and longitudes in the atmospheres thus measuring their three-dimensional thermal and chemical structure and contributing to our understanding of their global circulation. Planets with characteristics suitable for atmospheric characterization have orbits of several days, so phase curve observations are highly resource intensive, especially for shared use facilities. The Exoplanet Climate Infrared TElescope (EXCITE) is a balloon-borne near-infrared spectrometer designed to observe from 1 to 5 meters to perform phase-resolved spectroscopy of hot Jupiters. Flying from a long duration balloon (LDB) platform, EXCITE will have the stability to continuously stare at targets for days at a time and the sensitivity to produce data of the quality and quantity needed to signicantly advance our understanding of exoplanet atmospheres. We describe the EXCITE design and show results of analytic and numerical calculations of the instrument sensitivity. We show that an instrument like EXCITE will produce a wealth of quality data, both complementing and serving as a critical bridge between current and future space-based near infrared spectroscopic instruments.

Description: To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2300 keV band and the Kashima NICT radio telescope in the 1.41.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 fluctuations of the X-ray fluxes at the pulse peaks, and the 3 upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.510 keV and 70300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) 10(exp 11) erg cm(exp 2), respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magnetosphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a 〉0.02% brightening of the pulse-peak flux under such conditions.

Description: No abstract available

Description: The Origins Space Telescope (OST) is studied as a future Mid- and Far-Infrared flagship-class observatory. OST will cover the wavelength range from 6 to 600 microns. To reach the sky background for 200-micron wavelengths temperatures of 4 degrees Kelvin or lower are required. To achieve this low temperature active cooling is required, along with passive shielding and passive radiation to deep space. Currently two concepts are being studied: Concept 1 with a 9-meter-diameter primary and a suite of 5 extremely capable instruments providing both imaging and spectroscopy over the entire wavelength range. Concept 2 is a more modest sized telescope with a collecting area equivalent to a 5-meter primary, fewer deployments and 3 or 4 instruments also covering the entire wavelength range for imaging and spectroscopy, although with somewhat reduced spectroscopic resolution, and somewhat slower mapping speed. This paper will describe OST Concept 2's cryogenic thermal architecture and thermal model results.

Description: An asteroid entering Earth's atmosphere deposits energy along its path due to thermal ablation and dissipative forces that can be measured by ground-based and spaceborne instruments. Inference of pre-entry asteroid properties and characterization of the atmospheric breakup is facilitated by using an analytic fragment-cloud model (FCM) in conjunction with a Genetic Algorithm (GA). This optimization technique is used to inversely solve for the asteroid's entry properties, such as diameter, density, strength, velocity, entry angle, and strength scaling, from simulations using FCM. The previous parameters' fitness evaluation involves minimizing error to ascertain the best match between the physics-based calculated energy deposition and the observed meteors. This steady-state GA provided sets of solutions agreeing with literature, such as the meteor from Chelyabinsk, Russia in 2013 and Tagish Lake, Canada in 2000, which were used as case studies in order to validate the optimization routine. The assisted exploration and exploitation of this multi-dimensional search space enables inference and uncertainty analysis that can inform studies of near-Earth asteroids and consequently improve risk assessment.

Description: The Wide-Field Infrared Survey Telescope (WFIRST) is planned to have a coronagraphic instrument (CGI) to enable high-contrast direct imaging of exoplanets around nearby stars. The majority of nearby FGK stars are located in multi-star systems, including the Alpha Centauri stars which may represent the best quality targets for the CGI on account of their proximity and brightness potentially allowing the direct imaging of rocky planets. However, a binary system exhibits additional leakage from the off-axis companion star that may be brighter than the target exoplanet. Multi-Star Wavefront Control (MSWC) is a wavefront-control technique that allows suppression of starlight of both stars in a binary system thus enabling direct imaging of circumstellar planets in binary star systems such as Alpha Centauri. We explore the capabilities of the WFIRST CGI instrument to directly image multi-star systems using MSWC. We consider several simulated scenarios using the WFIRST CGI's Shaped Pupil Coronagraph Disk Mask. First, we consider close binaries such as Mu Cassiopeia that require no modifications to the WFIRST CGI instrument and can be implemented as a purely algorithmic solution. Second, we consider wide binaries such as Alpha Centauri that require a diffraction grating to enable suppression of the off-axis starlight leakage at Super-Nyquist separations. We demonstrate via simulation dark holes in 10 percent broadband compatible with the WFIRST CGI.

Description: No abstract available

Description: No abstract available

Description: We present a reanalysis of five transit and eight eclipse observations of the ultrashort-period super-Earth 55 Cancri e observed using the Spitzer Space Telescope during 2011-2013. We use pixel-level decorrelation to derive accurate transit and eclipse depths from the Spitzer data, and we perform an extensive error analysis. We focus on determining possible variability in the eclipse data, as was reported in Demory et al. From the transit data, we determine updated orbital parameters, yielding T (sub 0) = 2,455,733.0037 +/- 0.0002, P = 0.7365454 +/- 0.0000003 days, i = 83.5 +/- 1fdg3, and R p = 1.89 +/- 0.05 R . Our transit results are consistent with a constant depth, and we conclude that they are not variable. We find a significant amount of variability between the eight eclipse observations and confirm agreement with Demory et al. through a correlation analysis. We convert the eclipse measurements to brightness temperatures, and generate and discuss several heuristic models that explain the evolution of the planet's eclipse depth versus time. The eclipses are best modeled by a year-to-year variability model, but variability on shorter timescales cannot be ruled out. The derived range of brightness temperatures can be achieved by a dark planet with inefficient heat redistribution intermittently covered over a large fraction of the substellar hemisphere by reflective grains, possibly indicating volcanic activity or cloud variability. This time-variable system should be observable with future space missions, both planned (JWST) and proposed (i.e., ARIEL).

Description: NASA's Kepler Mission was launched in March 2009 as NASA's first mission capable of finding Earth-size planets orbiting in the habitable zone of Sun-like stars, that range of distances for which liquid water would pool on the surface of a rocky planet. Kepler has discovered over 1000 planets and over 4600 candidates, many of them as small as the Earth. Today, Kepler's amazing success seems to be a fait accompli to those unfamiliar with her history. But twenty years ago, there were no planets known outside our solar system, and few people believed it was possible to detect tiny Earth-size planets orbiting other stars. Motivating NASA to select Kepler for launch required a confluence of the right detector technology, advances in signal processing and algorithms, and the power of supercomputing.

Description: No abstract available

Description: No abstract available

Description: No abstract available

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Description: We obtained high-resolution (lambda divided by delta times lambda equals approximately 25,000) pre-perihelion spectra of Comet C/2013 V5 (Oukaimeden) using NIRSPEC at Keck II on UT 2014 September 5-6, and CSHELL (Cryogenic Echelle Spectrograph) at the NASA-Infrared Telescope Facility on September 11-13, altogether spanning a range in heliocentric distance R (sub h) equals 0.789-0.698 astronomical units. We report water production rates, and production rates and abundance ratios relative to co-measured H2O for eight trace molecules: CO, H2CO, CH3OH, CH4, C2H2, C2H6, HCN, and NH3. Our measured water production rates from NIRSPEC ( Near Infra-Red Spectrograph) and CSHELL observations remained relatively constant and were close to those from SOHO (Solar and Heliospheric Observatory) / Solar Wind Anisotropies observations that encompassed our dates, suggesting H2O production dominated by release directly from or within approximately 2000 kilometers of the nucleus. All trace volatiles were depleted relative to their respective median abundances among comets, excepting NH3, which was consistent with its median abundance. Most surprising were pronounced increases in abundance ratios for CH3OH (by 51 percent relative to simultaneously measured H2O) and especially C2H6 (by 87 percent) between September 5 and 6. On September 5, C2H6 was severely depleted, consistent with its lowest abundance yet measured for any comet. It also tracked the spatial profile of H2O, suggesting C2H6 was associated with a polar ice phase dominating gas production. On September 6, C2H6 was only moderately depleted and was spatially distinct from H2O, suggesting both polar- and nonpolar-dominated ice phases contributed to the activity then. Our results are consistent with a nonhomogeneous volatile composition for C/2013V5, implying differential processing of its constituent ices.

Description: Sulfur has been observed to be severely depleted in dense clouds leading to uncertainty in the molecules that contain it and the chemistry behind their evolution. Here, we aim to shed light on the sulfur chemistry in young stellar objects (YSOs) by using high-resolution infrared spectroscopy of absorption by the 3 rovibrational band of SO2 obtained with the Echelon-Cross-Echelle Spectrograph on the Stratospheric Observatory for Infrared Astronomy. Using local thermodynamic equilibrium models we derive physical parameters for the SO2 gas in the massive YSO MonR2 IRS3. This yields a SO2/H abundance lower limit of 5.6 0.5 10(exp -7), or 〉4% of the cosmic sulfur budget, and an intrinsic line width (Doppler parameter) of b 〈 3.20 km s(exp -1). The small line widths and high temperature (Tex = 234 15 K) locate the gas in a relatively quiescent region near the YSO, presumably in the hot core where ices have evaporated. This sublimation unlocks a volatile sulfur reservoir (e.g., sulfur allotropes as detected abundantly in comet 67P/ChuryumovGerasimenko), which is followed by SO2 formation by warm, dense gas-phase chemistry. The narrowness of the lines makes formation of SO2 from sulfur sputtered off grains in shocks less likely toward MonR2 IRS3.

Description: We present simultaneous optical and radar observations of meteors observed over the Arecibo radar in Puerto Rico. These observations were obtained during ~24 h of radar time over 3 different nights in May 2012. The radar was operating in a dual-frequency mode at 430 MHz (UHF) and 46.8 MHz (VHF). The optical observations were made at 41 frames per second with an Andor Electron Multiplying CCD camera with a field of view of ~6, enabling the determination of accurate horizontal meteor velocities and optical light curves. There are varying detection sensitivities of the 3 different techniques (2 radar, 1 optical). The UHF radar is the most sensitive, resulting in a total of 8710 detected meteors during that period, while the VHF radar is significantly less sensitive resulting in only 278 detected meteors. The optical observations are the least sensitive, resulting in a total of 178 detections. Of all of these meteors, only 19 were simultaneously detected by the 3 instruments. This paper focuses on the analysis of these 19 common events. The meteoroid masses determined from the optical light curves were found to be in the range of 20 g to 1.2 mg and did not correlate with the maximum Signal-to-Noise Ratio (SNR) of either radar. In addition, the UHF radar detected 5 out of these 19 meteors with far side-lobes, beyond the main-beam and first side-lobe. This indicates that a significant fraction of events detected by the UHF radar could be in far side lobes and therefore have significantly underestimated Radar Cross Sections (RCS), given the smaller backscattered powers received in the side lobes.

Description: The Imaging X-ray Polarimetry Explorer (IXPE) will expand the information space for study of cosmic sources, by adding linear polarization to the properties (time, energy, and position) observed in x-ray astronomy. Selected in 2017 January as a NASA Astrophysics Small Explorer (SMEX) mission, IXPE will be launched into an equatorial orbit in 2021. The IXPE mission will provide scientifically meaningful measurements of the x-ray polarization of a few dozen sources in the 2-8 keV band, including polarization maps of several x-ray-bright extended sources and phase-resolved polarimetry of many bright pulsating x-ray sources.

Description: Future NASA concept missions that are currently under study, like the Habitable Exoplanet Imaging Mission (HabEx) and the Large Ultra-violet Optical Infra Red Surveyor (UVOIR), could discover a large diversity of exoplanets. We propose here a classification scheme that distinguishes exoplanets into different categories based on their size and incident stellar flux, for the purpose of providing the expected number of exoplanets observed (yield) with direct imaging missions. The boundaries of this classification can be computed using the known chemical behavior of gases and condensates at different pressures and temperatures in a planetary atmosphere. In this study, we initially focus on condensation curves for sphalerite ZnS, H2O, CO2, and CH4. The order in which these species condense in a planetary atmosphere define the boundaries between different classes of planets. Broadly, the planets are divided into rocky planets (0.5-1.0 solar radius), super-Earths (1.0-1.75 solar radius), sub-Neptunes (1.75-3.5 solar radius), sub-Jovians (3.5-6.0 solar radius), and Jovians (6-14.3 solar radius) based on their planet sizes, and "hot," "warm," and "cold" based on the incident stellar flux. We then calculate planet occurrence rates within these boundaries for different kinds of exoplanets, eta (sub planet) [i.e. exoplanet], using the community coordinated results of NASA's Exoplanet Program Analysis Group's Science Analysis Group-13 (SAG-13). These occurrence rate estimates are in turn used to estimate the expected exoplanet yields for direct imaging missions of different telescope diameters.

Description: The Gaia catalogue second data release and its implications to optical observations of man-made Earth orbiting objects. Abstract and not the Final Paper is attached. The Gaia spacecraft was launched in December 2013 by the European Space Agency to produce a three-dimensional, dynamic map of objects within the Milky Way. Gaia's first year of data was released in September 2016. Common sources from the first data release have been combined with the Tycho-2 catalogue to provide a 5 parameter astrometric solution for approximately 2 million stars. The second Gaia data release is scheduled to come out in April 2018 and is expected to provide astrometry and photometry for more than 1 billion stars, a subset of which with a the full 6 parameter astrometric solution (adding radial velocity) and positional accuracy better than 0.002 arcsec (2 mas). In addition to precise astrometry, a unique opportunity exists with the Gaia catalogue in its production of accurate, broadband photometry using the Gaia G filter. In the past, clear filters have been used by various groups to maximize likelihood of detection of dim man-made objects but these data were very difficult to calibrate. With the second release of the Gaia catalogue, a ground based system utilizing the G band filter will have access to 1.5 billion all-sky calibration sources down to an accuracy of 0.02 magnitudes or better. In this talk, we will discuss the advantages and practicalities of implementing the Gaia filters and catalogue into data pipelines designed for optical observations of man-made objects.

Description: No abstract available

Description: No abstract available

Description: When comparing the dark icy surfaces of outer solar system small bodies and the composition of carbonaceous chondrites derived from dark asteroids we find a significant discrepancy in the assessed amounts of elemental carbon: up to 80% amorphous carbon is used to model the dark surfaces of Kuiper Belt Objects and Centaurs whereas at most 5% of elemental carbon is found in carbonaceous chondrites. If we presume that regimes of comet nuclei formation are analogous to disk regimes where other outer solar system ice-rich bodies formed then we can turn to comet dust to gain insights into the diversity in the concentration and forms of carbon available in the outer disk. Comet dust offers important insights into the diversity in the amounts and forms of carbon that were incorporated into aggregate dust particles in the colder parts of the protoplanetary disk out of which comet nuclei accreted. Comet nuclei are amongst the most primitive bodies because they have remained cold and unequilibrated. Comet dust particles reveal the presence of forms of elemental carbon and of soluble and insoluble organic matter, and in a great diversity of concentrations from very little, e.g., Stardust samples of comet 81P/Wild 2, to 80% by volume for Ultra Carbonaceous Antarctic Micro Meteorites (UCAMMs). Cometary outbursts and/or jet activity also demonstrate variations in the concentration of carbon in the grains at different grain sizes within a single comet. We review the diversity of carbon-bearing dust grains in cometary samples, flyby measurements and deduced from remote-sensing to enrich the discussion about the diversity of carbonaceous matter available in the outer ice-rich disk at the time of comet nuclei formation.

Description: No abstract available

Description: We have analysed the differences in positions of 9081 matched sources between the GaiaData Release 2 (DR2) and very long baseline interferometry (VLBI) catalogues. The medianposition uncertainty of matched sources in the VLBI catalogue is a factor of two larger thanthe median position uncertainty in Gaia DR2. There are 9 per cent matched sources withstatistically significant offsets between both catalogues. We found that the reported positionalerrors should be rescaled by a factor of 1.3 for VLBI and 1.06 for Gaia and, in addition, the Gaiaerrors should be multiplied by the square root of chi squared per degree of freedom in order tobest fit the normalized position differences to the Rayleigh distribution. We have establishedthat the major contributor to statistically significant position offsets is the presence of opticaljets. Among the sources for which the jet direction was determined, the position offsets areparallel to the jet directions for 62 per cent of the outliers. Among the matched sources withsignificant proper motion, the fraction of objects with proper motion directions parallel tojets is a factor of three greater than on average. Such sources have systematically higher chisquared per degree of freedom. We explain these proper motions as a manifestation of thesource position jitter caused by flares, which we predicted earlier. Therefore, the assumptionthat quasars are fixed points, and thus that differential proper motions determined with respectto quasar photocentres can be regarded as absolute proper motions, should be treated withgreat caution.

Description: We report here on the results of our initial study of a mission to the deep outer regions of our solar system, with the primary mission objective of conducting direct megapixel high-resolution imag- ing and spectroscopy of a potentially habitable exoplanet by exploiting the remarkable optical properties of the SGL. Our main goal was not to study how to get there (although this was also addressed), but rather, to investigate what it takes to operate spacecraft at such enormous distances with the needed precision. Specifically, we studied i) how a space mission to the focal region of the SGL may be used to obtain high-resolution direct imaging and spectroscopy of an exoplanet by detecting, tracking, and studying the Einstein ring around the Sun, and ii) how such information could be used to detect signs of life on another planet.

Description: More than 600 multi-planet systems are known. The vast majority of these systems have been discovered by NASA's Kepler spacecraft, but dozens were found using the Doppler technique, the first multi-exoplanet system was identified through pulsar timing, and the most massive system has been found using imaging. More than one-third of the 4000+ planet candidates found by NASA's Kepler spacecraft are associated with target stars that have more than one planet candidate, and the large number of such Kepler "multis" tells us that flat multiplanet systems like our Solar System are common. Virtually all of Kepler candidate multis are stable, as tested by numerical integrations that assume a physically motivated mass-radius relationship. Statistical studies performed on these candidate systems reveal a great deal about the architecture of planetary systems, including the typical spacing of orbits and flatness. The characteristics of several of the most interesting confirmed multi-exoplanet systems will also be discussed.HR 8799's four massive planets orbit tens of AU from their host star and travel on nearly circular orbits. PSR B1257+12 has three much smaller planets orbiting close to a neutron star. Both represent extremes and show that planet formation is a robust process that produces a diversity of outcomes. Although both exomoons and Trojan (triangle Lagrange point) planets have been searched for, neither has yet been found.

Description: No abstract available

Description: The experience acquired through development, implementation and operation of the Kepler K2 science pipelines can provide lessons learned for the development of science pipelines for other missions such as NASA's Transiting Exoplanet Survey Satellite and ESA's PLATO mission.

Description: No abstract available

Description: Hybrid sensors comprising Shack-Hartmann Wavefront Sensor (S-HWFS) and Zernike Wavefront Sensor (Z-WFS) capabilities are presented. The hybrid sensor includes a Z-WFS optically arranged in-line with a S-HWFS such that the combined wavefront sensor operates across a wide dynamic range and noise conditions. The Z-WFS may include the ability to introduce a dynamic phase shift in both transmissive and reflective modes.