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: We present the case for the presence of complex organic molecules, such as amino acids and nucleobases, formed by abiotic processes on the surface and in near-subsurface regions of Pluto. Pluto's surface is tinted with a range of non-ice substances with colors ranging from light yellow to red to dark brown; the colors match those of laboratory organic residues called tholins. Tholins are broadly characterized as complex, macromolecular organic solids consisting of a network of aromatic structures connected by aliphatic bridging units (e.g., Imanaka et al.,2004; Materese et al.,2014, 2015). The synthesis of tholins in planetary atmospheres and in surface ices has been explored in numerous laboratory experiments, and both gas- and solid-phase varieties are found on Pluto. A third variety of tholins, exposed at a site of tectonic surface fracturing called Virgil Fossae, appears to have come from a reservoir in the subsurface. Eruptions of tholin-laden liquid H2O from a subsurface aqueous repository appear to have covered portions of Virgil Fossae and its surroundings with a uniquely colored deposit (D.P. Cruikshank, personal communication) that is geographically correlated with an exposure of H2O ice that includes spectroscopically detected NH3 (C.M. Dalle Ore, personal communication). The subsurface organic material could have been derived from presolar or solar nebula processes, or might have formed in situ. Photolysis and radiolysis of a mixture of ices relevant to Pluto's surface composition (N2, CH4, CO) have produced strongly colored, complex organics with a significant aromatic content having a high degree of nitrogen substitution similar to the aromatic heterocycles pyrimidine and purine (Materese et al.,2014, 2015; Cruikshank et al.,2016). Experiments with pyrimidines and purines frozen in H2O-NH3 ice resulted in the formation of numerous nucleobases, including the biologically relevant guanine, cytosine, adenine, uracil, and thymine (Materese et al.,2017). The red material associated with the H2O ice may contain nucleobases resulting from energetic processing on Pluto's surface or in the interior. Some other Kuiper Belt objects also exhibit red colors similar to those found on Pluto and may therefore carry similar inventories of complex organic materials. The widespread and ubiquitous nature of similarly complex organic materials observed in a variety of astronomical settings drives the need for additional laboratory and modeling efforts to explain the origin and evolution of organic molecules. Pluto observations reveal complex organics on a small body that remains close to its place of origin in the outermost regions of the Solar System.

Description: No abstract available

Description: Spacecraft surface charging during geomagnetically disturbed times is one of the most important causes of satellite anomalies. Predicting the surface charging environment is one prevalent task of the geospace environment models. Therefore, the Geospace Environment Modeling (GEM) Focus Group "Inner Magnetosphere Crossenergy/Population Interactions" initiated a communitywide challenge study to assess the capability of several inner magnetosphere ring current models in determining surface charging environment for the Van Allen Probes orbits during the 17 March 2013 storm event. The integrated electron flux between 10 and 50 keV is used as the metrics. Various skill scores are applied to quantitatively measure the modeling performance against observations. Results indicate that no model consistently perform the best in all of the skill scores or for both satellites. We find that from these simulations the ring current model with observational flux boundary condition and Weimer electric potential driver generally reproduces the most realistic flux level around the spacecraft. A simple and weaker VollandStern electric field is not capable of effectively transporting the same plasma at the boundary toward the Earth. On the other hand, if the ring current model solves the electric field selfconsistently and obtains similar strength and pattern in the equatorial plane as the Weimer model, the boundary condition plays another crucial role in determining the electron flux level in the inner region. When the boundary flux spectra based on magnetohydrodynamics (MHD) model/empirical model deviate from the shape or magnitude of the observed distribution function, the simulation produces poor skill scores along Van Allen Probes orbits.

Description: No abstract available

Description: No abstract available

Description: No abstract available

Description: What: Thermal moonquakes are small amplitude events that are produced by diurnal temperature changes. Why: Finding the locations of thermal moonquakes will lead to information about lunar surface processes. Where: Apollo 17 Lunar Seismic Profiling Experiment (LSPE) is able to locate thermal moonquake unlike Apollo 12-16. The primary science goal was an active source experiment to study the detailed structure of the lunar crust using 8 explosive packages (EPs). The secondary science goal was to passively listen for lunar seismic activity.

Description: No abstract available

Description: The Mars Science Laboratory Curiosity rover arrived at Mars in August 2012 with a primary goal of characterizing the habitability of ancient and modern environments. Curiosity landed in Gale crater to study a sequence of ~3.5 Ga old sedimentary rocks that, based on orbital visible/near-infrared reflectance spectra, contain secondary minerals that suggest deposition and/or alteration in liquid water. The sedimentary sequence that comprises the lower slopes of Mount Sharp within Gale crater may preserve a dramatic shift on early Mars from a relatively warm and wet climate to a cold and dry climate based on a transition from smectite-bearing strata to sulfate-bearing strata. The rover is equipped with cameras and geochemical and mineralogical instruments to examine the sedimentology and identify compositional changes within the stratigraphy. These observations provide information about variations in depositional and diagenetic environments over time. The Chemistry and Mineralogy (CheMin) instrument is one of two internal laboratories on Curiosity and includes a transmission X-ray diffractometer (XRD) and X-ray fluorescence (XRF) spectrometer with a Co-K source. CheMin measures loose sediment samples scooped from the surface and drilled rock powders. The XRD provides quantitative mineralogy of scooped and drilled samples to a detection limit of ~1 wt.%. Curiosity has traversed 〉20 km since landing and has primarily been exploring the site of a predominantly ancient lake environment fed by groundwater and streams emanating from the crater rim. Results from CheMin demonstrate an incredible diversity in the mineralogy of fluvio-lacustrine rocks that signify variations in source rock composition, sediment transport mechanisms, and depositional and diagenetic fluid chemistry. Abundant trioctahedral smectite and magnetite at the base of the section may have formed from low-salinity pore waters with a circumneutral pH within lake sediments. A transition to dioctahedral smectite, hematite, and Ca-sulfate going up section suggests a change to more saline and oxidative aqueous conditions within the lake waters themselves and/or within diagenetic fluids. The primary minerals detected in fluvio-lacustrine samples by CheMin also suggest diversity in the igneous source regions for the sediments, where abundant pyroxene and plagioclase in most samples suggest a basaltic protolith, but sanidine and pyroxene in one sample may have been sourced from a potassic trachyte, and tridymite and sanidine in another sample may have been transported from a rhyolitic source. Crystal chemistry of major phases in each sample have been calculated from refined unit-cell parameters, providing further constraints on aqueous alteration processes and igneous protoliths for the sediments. Perhaps one of the biggest mysteries revealed by the CheMin instrument is the high abundance of X-ray amorphous materials (15 to 73 wt.%) in all samples measured to date. X-ray amorphous materials were detected by CheMin based on the observation of broad humps in XRD patterns. How these materials formed, their composition, and why they persist near the martian surface remain a topic of debate. The sedimentology and composition of the rocks analyzed by Curiosity demonstrate that habitable environments persisted intermittently on the surface or in the subsurface of Gale crater for perhaps more than a billion years.

Description: The Habitable Exoplanet Observatory Mission (HabEx) will image and spectroscopically characterize planetary systems in the habitable zone around nearby sun-like stars. Additionally, HabEx will perform a broad range of general astrophysics science enabled by 100 to 2500 nm spectral range and 3 x 3 arc-minute FOV. Critical to achieving the HabEx science goals is a large, ultra-stable telescope. The baseline HabEx telescope is a 4-m off-axis unobscured three-mirror-anastigmatic design with diffraction limited performance at 400 nm and wavefront stability of picometers per mK. These specifications are driven by science requirements. STOP (structural thermal optical performance) analysis predicts that the baseline telescopes opto-mechanical design meets its specified performance tolerances.

Description: In recent years, several commercial companies have proposed telecommunications constellations consisting of hundreds to thousands of 100-to-300-kg class spacecraft in low Earth orbit (LEO, the region below 2000-km altitude). If deployed, such large constellations (LCs) will dramatically change the landscape of satellite operations in LEO. From the large number of spacecraft and large amount of mass involved, it is clear that the deployment, operations, and frequent de-orbit and replenishment of the proposed LCs could significantly contribute to the existing orbital debris problem. To better understand the nature of the problem, the NASA Orbital Debris Program Office (ODPO) recently completed a parametric study on LCs. The objective was to quantify the potential negative debris-generation effects from LCs to the LEO environment and provide recommendations for mitigation measures. The tool used for the LC study was the ODPOs LEO-to-GEO Environment Debris (LEGEND) numerical simulation model, which has been used for various mitigation and remediation studies in the past. For the LC study, more than 300 scenarios based on different user-specified assumptions and parameters were defined. Selected results from key scenarios are summarized in this paper.

Description: The Astromaterials Acquisition and Curation Office at NASA Johnson Space Center (henceforth AACO) is responsible for receiving and curating all of NASAs extraterrestrial samples, current and future (as per NASA Policy Directive (NPD) 7100.10E Curation of Extraterrestrial Materials). As such, the AACO coordinates sample capture, containment, and transportation to the curation facility as well as documents, preserves, prepares, and distributes all of the samples within NASAs astromaterial collections for research, education, and public outreach. Since the lunar rock and soil samples returned during the Apollo Program, NASAs first Class V Restricted Earth Return Missions, the AACO curates six other astromaterials collections. Lessons learned from each collection and respective missions (e.g. Apollo, Genesis, Stardust) as well as advancements in science and technology have informed the AACOs plan for acquiring and curating Martian samples. Given the nature of the collection, a mobile and modular facility is recommended. The two broad requirements a Mars sample facility must maintain are: 1) the ability to contain the samples to protect the public from exposure of an unknown unknown biological agent and 2) ensure the scientific integrity of the samples are maintained (while maximizing scientific outcome). Although Apollo samples were eventually deemed safe and released to the scientific community for evaluation, there is no guarantee that this will be the case for Martian samples. Therefore, the facility in which the samples will be contained and investigated must be modular and able to accommodate an array of instrumentation that could be highly variable depending on the initial scientific outcomes. Furthermore, in order to facilitate proper sample capture and containment upon landing as well as sample distribution to other laboratories with proper containment, a mobile facility is a valuable investment.

Description: The surfaces of airless bodies, such as 101955 Bennu, are vulnerable to micrometeoroids, high-energy particles, and solar wind particles. As a result, material on the surface of these bodies experience physical and chemical changes that are collectively known as space weathering. Space weathering processes result in the production of sub-micronsized particles called submicroscopic particles. There are two types of submicroscopic particles, nanophase (〈33 nm in size) and microphase particles (〉33 nm in size). Studies of lunar samples show that nanophase particles occur within the glassy rims that surround grains and agglutinates. In contrast, microphase iron particles occur only within agglutinates. Another important difference between these two particles is that nanophase and microphase particles affect visible to near-infrared reflectance spectra differently. From lunar samples, the presence of nanophase particles in a regolith causes the regoliths reflectance spectrum to darken and redden, whereas the presence of microphase particles in a regolith causes it to only darken. In addition, the reflectance spectra of submicroscopic particle-bearing regolith exhibit weakened absorptions and spectral features. Lantz et al. (2018) found that these particles also affect spectral curvature [8]. By taking advantage of these spectral characteristics, with global spectral data, it is possible to model the nanophase and microphase particle abundances across a planetary surface resulting in the production of global space weathering maps.

Description: The chondrule regions generally regarded to be most susceptible to aqueous alteration are mesostasis and Fe-Ni metal nodules. In CMs, studies of mesostasis have successfully placed contraints into their asteroidal histories. Unlike CM mesostasis, only a few studies of CR mesostasis are currently available [e.g. 1-4]. Here we study the effects aqueous alteration can have on the texture, composition, and mineralogy of CR chondrule mesostasis from 9 Antarctic CR chondrites: EET 92062,5, EET 96259,13, GRA 95229,77, GRO 95577,61 LAP 02342,44, LAP 04516,4, LAP 04720,16 and MIL 07525,7 and MIL 090001,2, generously provided by the U.S. Antarctic Meteorite Collection. To our knowledge, this is the first detailed TEM and compositional study of differences between chondrule setting in CR mesostasis. Based on these data, we place constraints on the degree to which these CRs record aqueous alteration.

Description: The Astromaterials Curation Division at NASAs Johnson Space Center houses seven sample collections stored in separate clean rooms to avoid cross-contamination. Prior to receiving new sample collections from carbon rich asteroids, we instituted a monitoring program to characterize the microbial ecology of these labs and to understand how organisms could interact with and potentially contaminate current and future collections. Methods: Beginning in Oct. 2017 we sampled the Meteorite (ISO 7 equivalent) and Pristine Lunar (ISO 5 equivalent) labs on a monthly basis. Surface samples were collected using dry swabs. Air samples were collected using an impactor style air sampler. Cultivable organisms were identified and characterized. Aliquots of each sample were also preserved for DNA sequencing. For each sampling event recovery rate was calculated as the percentage of samples showing microbial growth1. Fungal colonies were selected for amino acid extraction and analysis via Ultra- Performance Liquid Chromatography with Fluorescence Detection and Mass Spectrometry.

Description: Exploration Mission 2 (EM-2) will be NASAs first manned flight on the Space Launch System (SLS) and Orion Spacecraft. The mission has been changed from an SLS Block 1B configuration to Block 1. This change has necessitated a reexamination of the flight profile to determine what changes must be made in order to accommodate the reduced launch vehicle performance on the Block 1. Launch availability and orbital debris risk will be traded to find the best flight profile for both SLS and Orion.

Description: The Astromaterials Research and Exploration Science Division at JSC is responsible for the curation of extraterrestrial samples from NASA's past, present and future sample return missions. These samples provide data that help scientists better understand the history and evolution of our Solar System. Our mission is to preserve, protect, and distribute samples for research by the present and future scientific community.

Description: No abstract available

Description: Data from LRO has formed a corner-stone in our understanding of many fundamental aspects of lunar geology. However, as LRO approaches its 10th year of lunar discovery, key questions about volcanic, tectonic, and interior processes and composition still re-main.

Description: NASA's Space Communications and Navigation (SCaN) program is creating an operational optical communications network to complement its current radio frequency (RF) networks. NASA is currently planning for a new optical communications relay node in geostationary (GEO) orbit to be commissioned in 2025, developed by NASA's Goddard Space Flight Center (GSFC), as evolved from Goddard's Laser Communications Relay Demonstration (LCRD) GEO relay payload that will launch in 2019. The Next Generation optical relay node will serve as an initial element in a larger optical networking constellation that will consist of Government and commercial, and international relays. NASA's nodes will aggregate traffic at data rates of up to 10 Gigabits per second (Gbps) from users on the Earth's surface and up through suborbital, LEO, MEO, GEO, cislunar and even out to Earth-Sun Lagrange (1.25 Mkm) distances. Users that require low-latency will be serviced with an onboard complementary Ka-band downlink service. The next generation network will deploy 〉 100 Gbps space-to-ground links and also optical crosslinks between nodes to allow for user traffic backhaul to minimize ground station location constraints.

Description: Oral presentation will discuss the history of the ISS, ongoing research in space, and the plans for Gateway.

Description: The goal of the Mars Science Laboratory (MSL), Curiosity Rover mission is to determine if Gale Crater, Mars ever had a habitable environment and to search for evidence of extinct microbial life. Gale Crater is ~155 km wide with a layered central mound (~5 km high). The Curiosity rover has traversed ~20 km from the crater floor up 350 m to the lower slopes of the central mound for over 2200 Martian solar days (sols). Curiosity's instruments have evaluated the geochemistry and mineralogy of regolith fines, eolian sediments, and sedimentary rocks to assess Gale Crater's aqueous alteration history. Results indicate that Gale Crater surface material have experienced a complex authigenetic/diagenetic history involving fluids with varying pH, redox, and salt composition. The inferred geochemical conditions were favorable for microbial habitability and if life ever existed, there was likely sufficient organic C to support a small microbial population.

Description: No abstract available

Description: Hydrogen in nominally anhydrous minerals (NAMs) in meteorites provides insight to mantle sources of indigenous water on differentiated bodies: e.g. Peslier et al. 2017 [1], including Mars [2-4]. However, all meteorite samples, including Martian shergottites, record impact events as fractures, deformation, silicate darkening, shock melt veins and pockets, etc. The effect of shock on hydrogen in NAMs is poorly constrained, and must be understood prior to using these data to infer planetary indigenous water. Here we present water contents and D/H ratios (calculated as dD, i.e. the variation of the D/H ratio relative to a standard, in this case sea water "SMOW") in pyroxene, olivine and maskelynite in the olivine-phyric shergottite Larkman Nunatak 06319 (LAR 06319) as a function of proximity to impact melt. While the results suggest impact may have a role in fractionating H isotopes, the magmatic signature of H2O in Mars can be preserved in some pyroxene.

Description: Water, in the form of structurally bound hydrogen in the crystal lattice of nominally anhydrous minerals (NAMs), strongly influences many important physical processes on terrestrial planets and planetary objects. Water enhances the rates of plastic deformation and controls the degree of partial melting in silicate rocks, which influences the generation of melt and therefore the nature of planetary volcanism. Water has also been experimentally demonstrated to influence the nature of lattice preferred orientation in deformed aggregates, and thus may be important in the interpretation of seismic anisotropy data collected from planetary bodies, such as from the current InSight mission on Mars. Therefore, much attention has been focused on characterizing the distribution and concentration of water in the planets and rocky bodies of our solar system.

Description: Exploration Mission 2 (EM-2) will be NASAs first manned flight on the Space Launch System (SLS) and Orion Spacecraft. The mission has been changed from an SLS Block 1B configuration to Block 1. This change has necessitated a reexamination of the flight profile to determine what changes must be made in order to accommodate the reduced launch vehicle performance on the Block 1. Launch availability and orbital debris risk will be traded to find the best flight profile for both SLS and Orion.

Description: The NASA Curiosity rover has encountered both ancient and modern dune deposits within Gale crater. The modern dunes are actively migrating across the surface within the Bagnold Dune field of which Curiosity conducted analysis campaigns at two different localities. Variations in mafic-felsic mineral abundances between these two sites have been related to the aeolian mineral sorting regime for basaltic environments identified on the Earth which become preferentially enriched in olivine relative to plagioclase feldspar with increasing distance from the source. This aeolian mineral sorting regime for basaltic minerals has also been inferred for Mars from orbital data. The aim of this study is to investigate whether this aeolian mafic-felsic mineral sorting trend has left a geochemical signature in the ancient dune deposits preserved within the Stimson formation. The Stimson formation unconformably overlies the Murray formation and consists of thickly laminated, cross-bedded sandstone. Stimson outcrops have a variable thickness up to 5 meters covering a total area of 17 square kilometers. A dry, aeolian origin was determined for this sandstone due to the high sphericity and roundness of the grains, uniform bimodal grain size distribution (250-710 microns), and 1-meter-thick cross-beds. Identifying the geochemical signature of mineral sorting can provide insights about the paleo-net sediment transport direction of the dunes and prevailing wind direction at the time of deposition.

Description: The Sample Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) rover has been essential in understanding volatile-bearing phases in Gale Crater materials. SAMs evolved gas analysis mass spectrometry (EGA-MS) has detected H2O, CO2, O2, H2, SO2, H2S, HCl, NO, and other trace gases, including organic fragments, in many samples. The identity and evolution temperature of evolved gases can support CheMin instrument mineral detection and place constraints on trace volatile-bearing phases or phases difficult to characterize with X-ray diffraction (e.g., amorphous phases). For the past ~500 sols, MSL has been exploring the Vera Rubin Ridge (VRR), which exhibits a striking hematite signature in orbital remote sensing data, in order to understand the depositional and diagenetic history recorded in the rocks and how it relates to the underlying Murray Formation. Four rock samples were drilled, one from the Blunts Point Member (Duluth, DU), one from the Pettegrrove Point Member (Stoer, ST), and two from the Jura Member. The Jura Member displays differences in color, summarized as grey and red, and a key goal was to constrain the cause of this color difference and the associated implications for depositional or post-depositional conditions. To investigate, a grey (Highfield, HF) and a red (Rock Hall, RH) Jura sample were drilled. Here we will give an overview of results from SAM EGA-MS analyses of VRR materials, with some comparisons to analyses of samples of the underlying Murray.

Description: No abstract available

Description: The Astromaterials Acquisition and Curation Office at the Johnson Space Center is the past, present, and future home of all of NASAs astromaterials sample collections. The primary goals of the curation office are to maintain the long-term integrity of the samples and ensure that the samples are distributed for scientific study in a fair, timely, and responsible manner, thus maximizing the return on each sample. Part of the curation process is planning for the future. To this end, we perform fundamental research in advanced curation initiatives to better prepared for future sample return missions. Advanced Curation is tasked with developing procedures, technology, and data sets necessary for curating new sample collections, or getting new results from existing sample collections. As part of these advanced curation efforts, we have installed and are operating a Nikon XTH 320 X-ray Computed Tomography(XCT) system in the JSC curation office with four interchangeable X-ray sources, a large-area detector, and a heavy-duty stage. These instrument characteristics allow us exceptional flexibility to analyze a wide range of sample sizes, from sub-mm soil particles to rocks 〉10 cm in diameter. The penetrative nature of the XCT scans allows for astromaterials samples to be analyzed within sealed low-density containers (e.g., Teflon bags), preserving the pristinity of the samples. We have begun scanning of the Apollo and Antarctic Meteorite sample suites in order to non-destructively map out lithic clasts (and other features) within the samples. The data from these scans will be made available to scientists via the JSC curation website and the Astromaterials Curation Newsletter. We anticipate sample requests from these new lithic clasts identified in these old samples. We also anticipate that XCT analyses like these would be useful for future sample return missions, like the OSIRIS REx mission, as well as future sample return missions.

Description: In magmatic systems, the availabil- ity of excess oxygen that can react with multivalent elements such as Fe and S to change their charge (oxi- dation of Fe2+ to Fe3+ or reduction of S6+ to S2-) is characterized by a parameter called the oxygen fugacity (O2). The O2 controls the availability of these ions and consequently the mineralsand the chemistry of those mineralsthat crystallize from a melt. Mineral mode and chemistry control how magmas evolve, and given that O2 varies by many orders of magnitude on different planets [2], understanding the O2 of a mag- ma is critical to relating observations about a magma to the body on which it forms. The mineral apatite was long thought to only incor- porate S6+ in a coupled substitution for P5+, but recently natural apatites with S2- were identified in lunar mare basalts that crystallized at low O2 [3]. This suggests that apatite can be used as a monitor of O2 assuming that one can 1) measure S6+/S (S6+ over total sulfur), and 2) determine some partitioning relationship be- tween apatite and melt for S6+ and S2-. The most common method for measuring S6+/S is X-ray Absorption Near-Edge Spectroscopy (XANES), but given the limited access to synchrotron facilities, it is wise to explore the potential of other methods for measuring S6+/S. One such possible method relies upon the shift in energy of the sulfur K- peak on the electron microprobe. However, apatite is subject to well-documented beam damage [4, 5], so it is neces- sary to evaluate under what conditions can reliable S6+ ethod.

Description: No abstract available

Description: Seismic data, inclusive of velocities and attenuation, can be utilized to elucidate the physical state of planetary interiors]. However, numerous micromechanical factors have been either experimentally demonstrated, or theoretically considered, to affect the propagation and dissipation of seismic energy within crystalline solids - including, but not limited to, changes in grain size, temperature, melt fraction, pressure and dislocation density. Thus, observed variations in seismic wave speeds and attenuation may be used to ultimately map variations in physical properties, such as those listed above, within planetary bodies. But, in order to complete a successful inversion of seismic data into representations of physical properties, a first requirement is to obtain a fundamental laboratory based understanding of how each of these possible factors individually influences seismic waves. Here we conduct an experimental study with the initial objective to further understand one of the most commonly invoked, yet least studied, mechanisms that could alter intrinsic seismic wave attenuation: water content (occurring as chemically-bound hydroxyl). The historical basis for determining the effect of water on seismic properties was established predominantly through analogy with large-strain creep experiments conducted on olivine under water-saturated conditions. While these deformation experiments routinely demonstrate a weakening of olivine in the presence of water, they represent a fundamentally different deformation regime in comparison to the microstrains experienced due to a passing seismic wave. Thus, in order to directly assess the effects of water on seismic properties, small-strain experiments are required. Substantially modified seismic properties in the presence of water have been observed previously at low strains and low frequencies, but only in a single exploratory study conducted under water-saturated conditions. Thus, to properly test the theoretical predictions we conducted a systematic study of the seismic properties of olivine using low-frequency torsional oscillation on aggregates containing varying concentrations of bound hydroxyl, for the first time at under saturated conditions.

Description: Impact cratering is an important geological process that occurs on every rocky body in the solar system. It alters the texture and mineralogy of rocks via shock metamorphism. The peak shock pressures experienced by a rock are traditionally evaluated using qualitative optical methods however, quantitative methods do exist. One such method was developed by Uchizono et al., who used X-ray Diffraction (XRD) to measure lattice strain () in several artificially shocked olivine grains using XRD peak broadening as a function of tan , where is the diffraction angle. They plotted the values against the known peak shock pressures experienced by the olivine grains. Using this calibration curve, the precise shock pressure experienced by a grain of olivine can be determined using its measured value. Another method was developed by McCausland et al. and Izawa et al., who used in situ XRD to measure strain-related mosaicity (SRM) of olivine in several ordinary chondrites and enstatite in enstatite chondrites, respectively. They plotted these results against the shock stage estimates for these meteorites. Using these plots, meteorites can be assigned to shock stage bins by measuring the SRM of olivine and/or enstatite. Both methods are useful for evaluating shock metamorphism, however, they have limitations. Uchizono et al.s calibration curve has been successfully applied to martian meteorites, however it can only be applied to olivine-bearing rocks. McCausland et al.s and Izawa et al.s SRM method is uncalibrated and is limited to binning meteorites by shock stage. This work aims to expand on both methods by creating calibration curves for clinopyroxene (CPX): one for , similar to Uchizono et al.s calibration curve for olivine, and one for SRM. This will extend the application of shock calibration methods to a greater variety of rock types. Preliminary results are presented herein.

Description: No abstract available

Description: No abstract available

Description: Space weathering alters the surfaces of airless planetary bodies via irradiation from the solar wind and micrometeorite impacts. These processes modify the microstructure, chemical composition, and spectral properties of surface materials, typically resulting in the reddening (increasing reflectance with increasing wavelength), darkening (reducing albedo), and attenuation of characteristic absorption features in reflectance spectra. In lunar samples, these changes in optical properties are driven by the production of reduced nanophase Fe particles (npFe). Our understanding of space weathering has largely been based on data from the Moon and, more recently, near-Earth S-type asteroids. However, the environment at Mercury is significantly different, with the surface experiencing intense solar wind irradiation and higher velocity micrometeorite impacts. Additionally, the composition of Mercurys surface varies significantly from that of the Moon, including a component with very low albedo known as low reflectance material (LRM) which is enriched with up to 4 wt.% carbon over the local mean. Our understanding of how carbon phases, including graphite, are altered as a result of these processes is limited.

Description: In a negative-polarity coronal hole, magnetic flux emergence, seen by the Solar Dynamics Observatory's {SDO) Helioseismic Magnetic lmager (HMI), begins at approximately 19:00 UT on March 3, 2016. The emerged magnetic field produced sunspots, which NOAA numbered 12514 two days later. The emerging magnetic field is largely bipolar with the opposite-polarity fluxes spreading apart overall, but there is simultaneously some convergence and cancellation of opposite-polarity flux at the polarity inversion line (PIL) inside the emerging bipole. In the first fifteen hours after emergence onset, three obvious eruptions occur, observed in the coronal EUV images from SDO's Atmospheric Imaging Assembly (AIA). The first two erupt from separate segments of the external PIL between the emerging positve-polarity flux and the extant surrounding negative-polarity flux, with the exploding magnetic field being prepared and triggered by flux cancellation at the external PIL. The emerging bipole shows obvious overall left-handed shear and/or twist in its magnetic field. The focus of th is poster is the third and largest eruption, which comes from inside the emerging bipole and blows it open to produce a CME observed by SOHO/LASCO. That eruption is preceded by flux cancellation at the emerging bipole's interior PIL, cancellation that plausibly builds a sheared and twisted flux rope above the interior PIL and finally triggers the blow-out eruption of the flux rope via photospheric-convectiondriven slow tether-cutting reconnection of the legs of the sheared core field, low above the interior PIL, as proposed by van Ballegooijen & Martens (1989) and Moore & Roumeliotis (1992). The production of this eruption is a (perhaps rare) counterexample to solar eruptions that result from external collisional shearing between opposite polarities from two distinct emerging and/or emerged bipoles (Chintzoglou et al. 2019).

Description: We present data from ground-based, vacuum-chamber tests demonstrating the ability to modulate the output of a plasma source capable of producing a low-Earth orbit (LEO) type plasma. We obtained plasma oscillations up to 2.5 kHz impingent on stationary test equipment, which corresponds to meter-level ionospheric structures in LEO. This plasma source is, therefore, suitable for developing scientific instruments that measure the LEO plasma environment, in situ, with meter-level spatial resolution. Measurements were made using a fixed-bias collector and an electrometer sampling at 40 kHz. A mechanical aperture was established at the output of the plasma source via two concentric grids. The outer grid was free to rotate in the azimuthal direction with respect to the fixed inner grid. An identical, alternating hole pattern in the two grids resulted in a variable aperture that cycles through 90 open/close cycles per revolution. The frequency of the plasma oscillations is limited by the mechanism used to spin the grids and the bearing assembly on which the grids rotate. Higher frequencies are obtainable by upgrading the drive mechanism, allowing the possibility of centimeter-level spatial resolution.

Description: No abstract available

Description: Determining the biological impact of spaceflight through novel approaches is essential to reduce the health risks to astronauts for long-term space missions. The current established health risks due to spaceflight are only reflecting known symptomatic and physiologic responses and do not reflect early onset of other potential diseases. There are many unknown variables which still need to be identified to fully understand the health impacts due to the environmental factors in space. One method to uncover potential novel biological mechanisms responsible for health risks in astronauts is by utilizing NASA's GeneLab Data Systems (genelab.nasa.gov). GeneLab is public repository that hosts multiple omics datasets generated from space biology experiments that include experiments flown in space, simulated cosmic radiation.

Description: No abstract available

Description: The dramatic flow of data from the Kepler and K2 missions opens the opportunity to significantly improve our knowledge of stellar interiors, surface dynamics, and structure. However, interpretation of these observations is a challenging task because it depends on tiny effects that can be studied only with advanced first-principles modeling. We present results of 3D time-dependent radiative hydrodynamic simulations of stellar outer convection zones and atmospheres taking into account chemical composition, radiative transfer, turbulence effects, and a realistic equation of state for main sequence stars. We will discuss properties of convective structure and dynamics, convective overshoot, effects of magnetic fields and rotation, as well as the potential influence of turbulent surface dynamics on high-precision RV measurements.

Description: When faced with the question of designing an asteroid deflection mission or with the decision of launching it, significant uncertainties are present in the asteroids physical properties, and its orbit solution. The success of the deflection mission relies heavily on these aspects. For example, a heavier than expected asteroid will reduce the imparted deflection DV. So will a larger porosity value by reducing the beta factor [1]. Here, we present a new capability that estimates asteroid impact risk under consideration of these uncertainties. The new method samples the uncertainty space along multiple dimensions, performs a predetermined deflection, propagates the deflected samples to the Earth, models the impact damage, and estimates the overall risk outcome. The work builds on the Probabilistic Asteroid Impact Risk (PAIR) assessment tool [2] by including orbital uncertainty and deflection capabilities. We demonstrate this risk estimation approach for threatening asteroids using the example of the fictitious impactor 2019 PDC. Such analysis provides a quantitative basis for the work of decision makers and disaster managers. It may further find application in areas such as mitigation mission planning where projected post-mitigation risk can be compared to premitigation levels as a means of cost-benefit analysis formitigation options.

Description: No abstract available

Description: Fine-grained, spinel-rich Ca-Al-rich inclusions (FGIs) in carbonaceous chondrites consist of numerous layered nodules having cores of spinel, hibonite, and/or perovskite surrounded by multiple thin layers of melilite, anorthite, diopside, and/or olivine. They are interpreted as aggregates of direct high-temperature condensates from an 16O-rich nebular gas that escaped significant melting. However, FGIs are very complex objects composed of intimate intergrowths of fine-grained refractory phases and show extremely large variations in mineralogy, modal abundance, and textures. Thus, detailed FIB/TEM analyses of FGIs are required to fully characterize their micro-to-nanometer scale textures, mineralogy, and chemical compositions and hence elucidate their formation processes and conditions in the early solar nebula. Here, we present our on-going study of pristine FGIs from the reduced CV3 chondrites Efremovka and Thiel Mountains (TIL) 07003 and 07007 that have minimal evidence for secondary parent body alteration.

Description: thermally-metamorphosed ordinary chondrite regolith breccias (Monahans 1998, hereafter simply Monahans ( 5) and Zag (H3-6)) contain fluid inclusion-bearing halite (NaCl) crystals dated to be ~4.5 billion years old. Thus, compositional data on fluid inclusions in these halites will reveal unique information regarding the origin and activity of aqueous fluids in the early solar system, and especially their interactions with organic mate- rial. Our initial analyses of solid inclusions in Monahans halite has shown the presence of olivine, high- and low- Ca pyroxene, feldspars, magnetite, sulfides, phyllosilicates, zeolites, metal, phosphates and abundant organics. We age of carbon, carbonates and organics in these residues, and low but significant amino acids concentrations in Monahans and Zag halite.

Description: The CM chondrites are generally complex impact breccias, in which lithic clasts and mineral fragments showing various degrees of aqueous alteration and possibly originating from different parent bodies are mixed together. The occurrence of CM-like clasts in other chondritic and achondritic meteorite breccias is also well-documented, however, reports on the occurrence of foreign clasts in CM chondrites are rare. In this study, we reinvestigated the white clast in the Murchison CM chondrite and demonstrate that the clast is not related to R chondrites as earlier suggested. In addition to the classification we discuss the origin and the history of its formation by studying several aspects like mineralogy, bulk chemistry, Rare Earth Elements (REE), oxygen isotopes, and the soluble organic compounds.

Description: No abstract available

Description: No abstract available

Description: For highly eccentric orbits such as that of the Magnetospheric Multiscale (MMS)mission, with apogee radius now 29.34 Earth radii, the third-body effects of Sun andMoon are the major perturbations. One key consequence is an oscillation in MMSperigee altitude, on an approximately 6 year cycle. This variation has already requiredperigee-raise maneuvers to avoid an untimely reentry. There is also a long-termevolution in the orientation of the MMS orbit, with period roughly twice as long. Thiseffect may potentially be useful for MMS science studies, as it can bring the spacecraftinto new regions of the magnetosphere.

Description: Fourteen CO3 chondrites have been recovered in the Dominion Range (DOM) dense collection area of the Transantarctic Mtns by ANSMET teams during the 2008-09, 2010-11, and 2014-15 seasons [1-3]. DOM 08006, one of the largest masses, has been studied extensively and is recognized to be a very primitive unmetamor-phosed sample of great value to planetary science [4]. Studies of pre-solar grains, organics, chondrules, inclusions, and matrix have revealed a rich scientific treasure helping to constrain the conditions in the early solar system (e.g., [4-8]). Many of the masses paired with this sample are significant, yet the pairing has been called into question due to the finding that DOM 08004 seems less primitive than DOM 08006 [5]. Because of the significant masses involved, and the great scientific value of DOM 08006, we have undertaken a detailed assessment of the pairing using field relations, macroscopic observations, petrography, and olivine compositions.

Description: No abstract available

Description: No abstract available

Description: No abstract available

Description: Oxygen fugacity and water content are crucial parameters for many chemical and physical properties of the Earth's mantle, for example bearing on fluid type, melting initiation, and deformation. However, the exact behaviour of Fe3+ and H during melting and metasomatism is still under debate. Here, the Fe3+/Fe ratio (Mssbauer and EMP) and water content (FTIR) of peridotite minerals are examined in mantle xenoliths from Kilbourne Hole (KH), NM, and Dish Hill (DH), CA (USA). These spinel peridotites have compositions consistent with partial melting with variable degrees of metasomatism (undetectable to cryptic to modal). Pyroxenites also allow to examine melt-rock reactions. Bulk-rock Fe2O3 content of the KH peridotites correlates with indices of melting (positive with bulk-rock Al2O3 and Cpx Yb contents, and negative with spinel Cr#) confirming that Fe3+ behaves as an incompatible element during melting. Correlations of the Fe3+/Fe ratio of minerals with these indices, however, indicates that Fe3+ is incompatible in Cpx but compatible in Opx and spinel during melting. Water contents in olivine, Cpx and Opx from most KH peridotites can be explained by partial melting and correlate negatively with the Fe3+/Fe ratio of spinel and Opx but positively with that of Cpx. This indicates partial control of Fe3+ on the incorporation of H in pyroxene, but not related to a redox equilibrium in Cpx. The higher Fe3+/Fe ratio of spinel in the metasomatized KH and DH peridotites, and in the pyroxenites confirms that oxidation characterizes modal metasomatism. Metasomatism, however, is not necessarily accompanied by water addition.

Description: Energy coupling between the solar wind and the Earth's magnetosphere can affect the electron population in the outer radiation belt. However, the precise role of different internal and external mechanisms that leads to changes of the relativistic electron population is not entirely known. This paper describes how ultralow frequency (ULF) wave activity during the passage of Alfvenic solar wind streams contributes to the global recovery of the relativistic electron population in the outer radiation belt. To investigate the contribution of the ULF waves, we searched the Van Allen Probes data for a period in which we can clearly distinguish the enhancement of electron uxes from the background. We found that the global recovery that started on 22 September 2014, which coincides with the corotating interaction region preceding a highspeed stream and the occurrence of persistent substorm activity, provides an excellent scenario to explore the contribution of ULF waves. To support our analyses, we employed ground and spacebased observational data and global magnetohydrodynamic simulations and calculated the ULF wave radial diffusion coefcients employing an empirical model. Observations show a gradual increase of electron uxes in the outer radiation belt and a concomitant enhancement of ULF activity that spreads from higher to lower Lshells. Magnetohydrodynamic simulation results agree with observed ULF wave activity in the magnetotail, which leads to both fast and Alfven modes in the magnetospheric nightside sector. The observations agree with the empirical model and are conrmed by phase space density calculations for this global recovery period.

Description: No abstract available

Description: No abstract available

Description: No abstract available

Description: The Habitable Exoplanet Observatory (HabEx) is one of four mission concepts under study for the 2020 Astrophysics Decadal Survey. Its goal is to directly image and spectroscopically characterize planetary systems in the habitable zone around nearby sun-like stars. Additionally, HabEx will perform a broad range of general astrophysics science enabled by 115 to 2500 nm spectral range and 3 x 3 arc-minute FOV. Critical to achieving the HabEx science goals is a large, ultra-stable UV/Optical/Near-IR (UVOIR) telescope. The baseline HabEx telescope is 4-meter off-axis unobscured, diffraction limited at 400 nm with wavefront stability on the order of a few 10s of picometers. The technology readiness level (TRL) to manufacture and test the HabEx baseline primary mirror is assessed to be at TRL-6 for all but two TRL-4 technologies: 1) non-destructive process to quantify CTE homogeneity of a 4-m mirror substrate with a spatial sampling of at least 100 x 100 to better than +/- 1 ppb/K; and, 2) process to quantify self-weight gravity deflection to better than 4-nm rms over a 100 x 100 spatial sampling. This paper reviews the technology needs to manufacture the HabEx primary mirror, assesses their TRL and proposes a roadmap to mature the two remaining technologies to TRL-6.

Description: No abstract available

Description: This study develops a vision-based detection and classification algorithm to address the challenges of in-situ small orbital debris environment classification including debris observability and instrument requirements for small debris observation. The algorithm operates in near real time and is robust under difficult tasks in moving objects classification such as multiple moving objects, objects with various movement trajectories and speeds, very small or faint objects, and substantial background motion. The performance of the algorithm is optimized and validated using space image data available through simulated environments generated using NASA Marshall Space Flight Centers Dynamic Star Field Simulator of on-board optical sensors and cameras.

Description: By the close of the Cassini mission in 2017 the Composite Infrared Spectrometer had recorded surface brightnesstemperatures on Titan for 13 yr (almost half a Titan year). We mapped temperatures in latitude from pole to pole inseven time segments from northern mid-winter to northern summer solstice. At the beginning of the mission thewarmest temperatures were centered at 13 S where they peaked at 93.9 K. Temperatures fell off by about 4 Ktoward the north pole and 2 K toward the south pole. As the seasons progressed the warmest temperatures shiftednorthward, tracking the subsolar point, and at northern summer solstice were centered at 24 N. While moving norththe peak temperature decreased by about 1 K, reaching 92.8 K at solstice. At solstice the fall-off toward the northand south poles were 1 K and 3 K, respectively. Thus the temperature range was the same 2 K at the two poles. Ourobserved surface temperatures agree with recent general circulation model results that take account of methanehydrology and imply that hemispherical differences in Titan's topography may play a role in the north?southasymmetry on Titan.

Description: No abstract available

Description: No abstract available

Description: From 2004 to 2017, the Cassini spacecraft orbited Saturn, completing 127 close ybys of its largest moon, Titan. Cassinis Composite Infrared Spectrometer (CIRS), one of 12 instruments carried on board, proled Titan in the thermal infrared (71000 m) throughout the entire 13 yr mission. CIRS observed on both targeted encounters (ybys) and more distant opportunities, collecting 8.4 million spectra from 837 individual Titan observations over 3633 hr. Observations of multiple types were made throughout the mission, building up a vast mosaic picture of Titans atmospheric state across spatial and temporal domains. This paper provides a guide to these observations, describing each type and chronicling its occurrences and global-seasonal coverage. The purpose is to provide a resource for future users of the CIRS data set, as well as those seeking to put existing CIRS publications into the overall context of the mission, and to facilitate future intercomparison of CIRS results with those of other Cassini instruments and ground-based observations.

Description: The Primordial Inflation Explorer (PIXIE) is an Explorer-class mission concept to measure the gravitational-wave signature of primordial inflation through its distinctive imprint on the linear polarization of thecosmic microwave background (CMB). Its optical system couples a polarizing Fourier transform spectrometerto the sky to measure the differential signal between orthogonal linear polarization states from two co-pointedbeams on the sky. The double differential nature of the four-port measurement mitigates beam-related systematic errors common to the two-port systems used in most CMB measurements. Systematic errors coupling unpolarized temperature gradients to a false polarized signal cancel to first order for any individual detector. Thiscommon-mode cancellation is performed optically, prior to detection, and does not depend on the instrumentcalibration. Systematic errors coupling temperature to polarization cancel to second order when comparing signals from independent detectors. We describe the polarized beam patterns for PIXIE and assess the systematicerror for measurements of CMB polarization.

Description: The Miniaturized Electron pRoton Telescope, MERiT, is a lowmass, lowpower, compact instrument using an innovative combination of particle detectors, sensor electronics, and onboard processing. MERiT is flying on the Compact Radiation belt Explorer, CeREs, a 3U CubeSat launched into a low earth orbit of 500km altitude and inclination of 85 on 16 December 2018. The primary and secondary science goals of CeREs are to investigate electron microbursts and to study solar particles. MERiT comprises a stack of solid state detectors (SSD) behind space facing avalanche photo diodes (APDs) surrounded by WAl shielding to reduce sidepenetrating particle background. The APDSSD combination enables measurement of electrons from 5 to 200 keV and 1 to 8 MeV; protons from 200400 keV and 7100 MeV in differential channels with energy resolution E/E30% for both electrons and protons. MERiT measures microbursts with a high time resolution ranging from 4 to 16 ms and solar particles with a cadence of 1 s. MERiT energy channels and cadences are software configurable via algorithms and lookup tables residing on a fieldprogrammable gate array. The lookup tables can be changed via ground commands. MERiT geometry factor is 31 sq.cmsr and optimized to measure microbursts with the instrument viewing the local zenith in orbit. MERiT enables investigation of dynamical processes of radiation belt electron energization and loss, solar electron and proton transport, and their access to the Earth's polar caps. We describe the MERiT sensor design, calibration, operational modes, data products, and science goals.

Description: C II is one of the brightest emission lines from star-forming galaxies and is an excellent tracer for star formation. Recent work measured the C II emission line amplitude for redshifts 2 〈 z 〈 3.2 by cross-correlating Planck High Frequency Instrument emission maps with tracers of overdensity from the Baryon Oscillation Spectroscopic Sky Survey, finding I(CII)=6.6(sup +5.0, sub 4.810(exp 4) Jy/sr at 95per cent confidence level. In this paper, we present a refinement of this earlier work by improving the mask weighting in each of the Planck bands and the precision in the covariance matrix. We report a detection of excess emission in the 545 GHz Planck band separate from the cosmic infrared background (CIB) present in the 353857 GHz Planck bands. This excess is consistent with redshifted C II emission, in which case we report b(CII)I(CII)=2.0(sup +1.2, sub 1.110(exp 5) Jy/sr at 95 per cent confidence level, which strongly favours many collisional excitation models of C II emission. Our detection shows strong evidence for a model with a non-zero C II parameter, though line intensity mapping observations at high spectral resolution will be needed to confirm this result.

Description: The NASA Orbital Debris Program Office (ODPO) studies all aspects of spacecraft end-of-life and orbital debris measurement, modeling, and mitigation. The reentry safety group within the ODPO uses the Object Reentry Survival Analysis Tool (ORSAT) to calculate the casualty risk due to reentry of spacecraft and other types of orbital debris. ORSAT models spacecraft as a collection of fragments that break apart from the parent object at a pre-defined breakup altitude. It then calculates the trajectory and aero-heating of these fragments to determine which fragments are completely destroyed and which survive to the ground and pose a risk to human population. Because of the historically high computational cost of these calculations, many simplifying assumptions have been made in the traditional calculation and analysis process used by the ODPO, some of which have been shown by recent research by the ODPO and others to be incorrect. Improvements to the ORSAT code and advancements in computer technology have vastly decreased the programs processing time, and have allowed the ODPO to develop a capability for large-scale parametric studies and Monte Carlo reentry simulations that can aid in both the initial spacecraft design and provide more detailed and accurate risk analysis to spacecraft operators.

Description: There is a limited amount of hypervelocity impact (HVI) data on pressurized composite overwrapped pressure vessels (COPV). In recent years, NASA has performed HVI tests to characterize impact conditions resulting in either leak or burst of the COPVs representative of spacecraft hardware. This paper reports on the results of 40 tests that have been conducted on several types of COPV configurations, pressurized by inert gas to near the vessels rated maximum expected operating pressure (MEOP). These tests were used to better understand COPV response under HVI conditions and develop ballistic limit equations (BLE) related to these tests.

Description: The statistical debris measurement campaigns conducted by the Haystack Ultrawideband Satellite Imaging Radar on behalf of the NASA Orbital Debris Program Office are used to characterize the long-term behavior of the small, low Earth orbit (LEO) orbital debris environment. Recent analyses have revealed the presence of a persistent LEO small debris cloud, which has no accompanying large component, cataloged by the U.S. Space Surveillance Network. This cloud, at an inclination of approximately 82 and below 1200 km in altitude does, however, correspond to the heavily trafficked region of space that has suffered several known, accidental collisions, e.g., Cosmos 1934 and Cosmos 2251. In this paper, we describe the observed cloud and model it using the NASA Standard Satellite Breakup Model. Key features of the cloud model, including source attribution and debris mass constraints, are presented to enable further observations and characterization.

Description: No abstract available

Description: We used a terrestrial single-station seismometer to quantify the uncertainty of InSight (INterior explorations using Seismic Investigations, Geodesy and Heat Transport) data for determining Martian core size. To mimic Martian seismicity, we formed a catalog using 917 terrestrial earthquakes, from which we randomly selected events. We stacked ScS amplitudes on modeled arrival times and searched for where ScS produced coherent seismic amplitudes. A core detection was defined by a coherent peak with small offset between predicted and user-selected arrival times. Iterating the detection algorithm with varying signal-to-noise (SNR) ranges and quantity of events determined the selection frequency of each model and quantified core depth uncertainty. Increasing the quantity of events reduced core depth uncertainty while increasing the recovery rate, while increasing event SNR had little effect. Including ScS2 multiples increased the recovery rate and reduced core depth uncertainty when we used low quantities of events. The most-frequent core depths varied by back azimuth, suggesting our method is sensitive to the presence of mantle heterogeneities. When we added 1 in source distance errors, core depth uncertainty increased by up to 11 km and recovery rates decreased by 〈5%. Altering epicentral distances by 25% added ~35 km of uncertainty and reduced recovery rates to 〈50% in some cases. From these experiments, we estimate that if InSight can detect five events with high location precision (〈10% epicentral distance errors), that there is at least an 88% chance of core depth recovery using ScS alone with uncertainty in core depth approaching 18 km and decreasing as more events are located.

Description: Existing DOD and NASA satellite breakup models are based on a key laboratory test, the 1992 Satellite Orbital debris Characterization Impact Test, which has supported many applications and matched on-orbit events involving older satellite designs reasonably well over the years. In 2014, the NASA Orbital Debris Program Office, in collaboration with the Air Force Space and Missile Systems Center, The Aerospace Corporation, and the University of Florida, conducted a hypervelocity impact test using a high-fidelity, mock-up satellite, DebriSat, in controlled and instrumented laboratory conditions to update and improve these models. DebriSat is representative of present-day, low Earth orbit satellites, having been constructed with modern spacecraft materials and techniques. The DebriSat fragment ensemble provided a variety of shapes, bulk densities, and dimensions. Fragments down to 2 mm in size are being characterized by their physical and derived properties. The data will inform updates to the current NASA Standard Satellite Breakup Model (SSBM), which was formulated using laboratory and ground-based measurements of on-orbit fragmentation events to describe an average breakup for spacecraft and upper-stage collisions and explosions. Although individual fragment collection and characterization is still ongoing, this paper will present the status of the DebriSat fragment data analysis including cumulative characteristic length and cumulative mass distributions, area-to-mass distributions, and characteristic length versus mass distributions. Additionally, comparisons to the NASA SSBM will be presented.

Description: The Indian spacecraft Microsat-R (International Designator 2019-006A, U.S. Strategic Command [USSTRATCOM] Space Surveillance Network [SSN] catalog number 43947), launched on 24 January 2019, was intentionally destroyed in a test of a ground-based, direct-ascent Anti-Satellite (ASAT) weapon system at 0640 GMT on 27 March 2019. At the time of breakup the 740 kg spacecraft was in an approximately 294 x 265 km altitude, 96.63 orbit. A total of 101 debris have entered the public satellite catalog (through object 2019-006DF), of which 49 fragments remain on-orbit as of 15 July 2019. However, over 400 fragments were initially tracked by SSN sensors and cataloging is complicated by the low altitude of the event and the concomitant rapid orbital decay. A Gabbard plot of this debris cloud is presented in the figure on page 2. A Centaur V Single-Engine Centaur (SEC) rocket variant (International Designator 2018-079B, SSN number 43652) fragmented in early April 2019. At the time of the event the stage was in an approximately 35,092 x 8526 km altitude, 12.2 orbit. This Centaur V upper stage is associated with the launch of the USA 288, or Advanced Extremely High Frequency 4 (AEHF 4), spacecraft from the (U.S.) Air Force Eastern Test Range on 17 October 2018. The cause of the event is unknown. No debris have entered the catalog at this time, but the ODQN will provide updates should they become publicly available.

Description: We present the first observation of Titan with the high resolution Echelon cross-Echelle Spectrograph(EXES) instrument on the Stratospheric Observatory for Infrared Astronomy (SOFIA, Fig. 1). These show clear detection of multiple spectral lines in the R-branch of the acetylene vibrational band at 13 m. These are compared to similar observations with the ground-based sister instrument TEXES (Texas Echelon cross-Echelle Spectrograph) on the IRTF(Infrared Telescope Facility), showing that EXES will have access to an enlarged spectral range as expected, through reduced atmospheric opacity. In future EXES will be used to complement TEXES for spectral line searches on Titan, geared to detect new molecular species, focusing on spectral regions that are inaccessible from the ground.

Description: Gravitational potential data from GRACE are being used to study mass redistribution within and between the atmosphere, hydrosphere, cryosphere, and solid Earth. The GRACE data are made available in a reference frame with its origin at the center of mass of the Earth system (geocenter) while many other geophysical models and data sets refer to a reference frame attached to the Earth's surface. Changes in the offset between these reference frames (geocenter motion) must be accounted for when GRACE data are used to quantify surface mass changes. In this study, we developed a technique for coestimation of geocenter motion and gravitational potential field seamlessly from degree 1 to 90 by simultaneously inverting a set of globallydistributed GPS displacement time series and the temporallyvarying GRACE gravity data. We found that the effect of geocenter motion was evident particularly in the GPS time series of horizontal displacements. Our estimates of geocenter motion are most consistent with the Satellite Laser Ranging (SLR) results within 1 mm in X and Z components and a submillimeter in Y component, when compared to monthly variability averaged over the period of 20032016. The overall magnitude of the degree1 (l = 1) surface mass load is estimated to be ~3 cm in equivalent water height annually migrating southwestward from Europe (DecemberJanuary) to the South Pacific (JuneJuly). Our results also show that dense GPS network data improve water storage recovery in major river basins in the United States and Europe by contributing significantly to the recovery of higherdegree (l ~20) geopotential coefficients.

Description: The Flow Boiling and Condensation Experiment (FBCE) to be manifested on the International Space Station (ISS) consists of a fluid system and the associated electronics to provide for conditioning the test fluid (normal-PerFluorohexane or nPFH-C6F14) to the proper thermodynamic state prior to entering a test module, which can be interchangeable based on the science objectives. Two separate test modules have been manufactured for the FBCE, the Flow Boiling Module (FBM), which investigates flow boiling for a subcooled liquid, saturated liquid, or two phase mixture, and the Condensation Module Heat Transfer (CM-HT), which investigates condensation of a flowing saturated or superheated vapor. The test fluid heating is accomplished using the Bulk Heater Module (BHM), which heats the fluid to various states based on the demands of the currently installed test module. ISS Internal Thermal Control System (ITCS) water is utilized to cool the test fluid prior to entering the circulation pump, and is also utilized for cooling for condensation in CM-HT, for cooling of a camera in FBM. An adjustable pressure bellows-type accumulator is used to set the pressure at the inlet of the test section, but does not provide active pressure control during testing. The flow of the test fluid is achieved using a gear pump controlled by a coriolis flow meter, which also provides the flow rate measurement. Flow rates for the ITCS water loops are measured and controlled using coriolis flow meters with directly controlled proportional valves. During execution of FBCE operations, the FBM is scheduled to collect data for three months before being exchanged with CM-HT for another three month data collection run. In this work, we present the development of the flight hardware, the associated challenges experienced during the development such as packaging flight system hardware, and the lessons learned in overcoming the encountered challenges.

Description: This study retrieved estimated altitudes of Martian water-ice clouds through a comparison of observations taken by the Mars Science Laboratory (MSL, Curiosity) rover and the Mars Regional Atmospheric Modelling System (MRAMS). The vertical pointing of a Zenith Movie (ZM) allows many wind velocities and directions to be measured when clouds are observed, however without a lidar onboard the altitude of these clouds cannot be directly determined. By simulating conditions at Gale Crater with MRAMS, wind properties found in ZMs can be correlated with model outputs to estimate cloud altitudes at Gale Crater from the surface for the first time. These results are evaluated to assess any diurnal and seasonal cloud altitude patterns above Gale crater.

Description: Mars' atmosphere typically supports dust aerosol with an effective radius near 1.5 m, varying from ~1 m during low dust times near northern summer solstice to ~2 m during higher dust times in southern spring and summer. After global dust events, size variations outside this range have not previously been observed. We report on imaging and spectral observations by the Curiosity rover through the 2018 global dust event. These observations show that the dust effective radius was seasonally normal prior to the local onset of increased opacity, increased rapidly above 4 m with increasing opacity, remained above 3 m over a period of ~50 Martian solar days, then returned to seasonal values before the opacity did so. This demonstrates lifting and regionalscale transport of a dust population ~3 times the size of typical dust aerosol.

Description: No abstract available

Description: The role of the Science Mission Directorate (SMD) is to enable NASA to achieve its science goals in the context of the nation's science agenda. SMD's strategic decisions regarding future missions and scientific pursuits are guided by agency goals, input from the science community including the recommendations set forth in the National Research Council (NRC) decadal surveys and a commitment to preserve a balanced program across the major science disciplines. Toward this end, each of the four SMD science divisions -- Heliophysics, Earth Science, Planetary Science, and Astrophysics -- develops fundamental science questions upon which to base future research and mission programs.

Description: The aubrites are a unique group of differentiated meteorites that formed on parent bodies with oxygen fugacities (O2) from ~2 to ~6 log units below the iron-wustite buffer. At these highly reduced condi- tions, elements deviate from the geochemical behavior exhibited at terrestrial O2, and may form FeO-poor silicates, Si-bearing metals, and exotic sulfides. Geochemical examinations of aubrites, such as mineral major-element compositions, bulk-rock compositions, O isotopes, and crystallization ages, are crucial to understand their formation and evolution at extreme O2 conditions. In this study, we determine partitioning relationships of elements between bulk silicate, sulfide, and metal phases within aubrites, and compare the results to partition coefficients determined from petrologic experiments run under mercurian conditions. While previous studies have described the petrology and 2D modal abundances of aubrites, this work provides the first 3D view of aubritic mineralogies, which are com- pared to the available 2D data. Constraints of 3D modal abundances will increase the accuracy of computed bulk distribution coefficients; therefore, 3D scans of aubrite samples are imperative. We utilize X-ray computed tomogra- phy (XCT) to non-destructively analyze the distribution and abundances of mineral phases in aubrites and locate composite clasts of sulfide grains for future analysis.

Description: Scientific drilling of the end-Cretaceous, approximately 180 kilometers-diameter Chicxulub crater (Yucatan Peninsula, Mexico) during IODPICDP (Integrated Ocean Drilling Program - International Continental Scientific Drilling Program) Expedition 364 has provided new insights into the formation, shock metamorphism, structural evolution, and thermal history of peak rings in large complex impact craters. An outstanding feature in uplifted granitoid rocks of the Chicxulub peak ring is the preservation of TiO2-II, an orthorhombic high-pressure polymorph of TiO2 with an alpha-PbO2 structure, produced during the impact from rutile and/or anatase at shock pressures of approximately 12.5-17.5 gigapascals. Unlike other mostly micro- and cryptocrystalline occurrences of TiO2-II at terrestrial impact sites, ejecta deposits, and in rare ultra-high pressure metamorphic rocks, TiO2-II at Chicxulub occurs as abundant euhedral crystals greater than or equal to 70 microns in size within aggregates of altered magmatic titanite. This mode of occurrence provides an excellent opportunity to investigate the crystallography and transformation kinetics of the shock-produced high-pressure polymorph using scanning electron microscopic, micro-Raman, electron backscatter diffraction (EBSD), focused ion beam (FIB), as well as transmission-EBSD and transmission electron microscopic (TEM) techniques. Here we present refined microstructural and new crystallographic results for TiO2-II at the Chicxulub crater.

Description: The ambient solar wind conditions in interplanetary space and in the near-Earth environment are determined by activity on the Sun. Steady solar wind streams modulate the propagation behavior of interplanetary coronal mass ejections and are themselves an important driver of recurrent geomagnetic storm activity. The knowledge of the ambient solar wind flows and fields is thus an essential component of successful space weather forecasting. Here, we present an implementation of an operational framework for operating, validating, and optimizing models of the ambient solar wind flow on the example of Carrington Rotation 2077. We reconstruct the global topology of the coronal magnetic field using the potential field source surface model (PFSS) and the Schatten current sheet model (SCS) and discuss three empirical relationships for specifying the solar wind conditions near the Sun, namely the WangSheeley (WS) model, the distance from the coronal hole boundary model (DCHB), and the Wang-SheeleyArge (WSA) model. By adding uncertainty in the latitude about the sub-Earth point, we select an ensemble of initial conditions and map the solutions to Earth by the Heliospheric Upwind eXtrapolation (HUX) model. We assess the forecasting performance from a continuous variable validation and find that the WSA model most accurately predicts the solar wind speed time series (RMSE83 km/s). We note that the process of ensemble forecasting slightly improves the forecasting performance of all solar wind models investigated. We conclude that the implemented framework is well suited for studying the relationship between coronal magnetic fields and the properties of the ambient solar wind flow in the near-Earth environment.

Description: Coronal Mass Ejections (CMEs) are the key drivers of strong to extreme space weather storms at the Earth that can have drastic consequences for technological systems in space and on ground.The ability of a CME to drive geomagnetic disturbances depends crucially on the magnetic structure of the embedded flux rope, which is thus essential to predict. The current capabilities in forecasting in advance(at least half a day before) the geo effectiveness of a given CME is however severely hampered by the lack of remote-sensing measurements of the magnetic field in the corona and adequate tools to predict how CMEs deform, rotate, and deflect during their travel through the coronal and interplanetary space as they interact with the ambient solar wind and other CMEs. These problems can lead not only to over estimation or underestimation of the severity of a storm, but also to forecasting "misses" and "false alarms" that are particularly difficult for the end-users. In this paper, we discuss the current status and future challenges and prospects related to forecasting of the magnetic structure and orientation of CMEs. We focus both on observational- and modeling-based (first principle and semiempirical) approaches and discuss the space- and ground-based observations that would be the most optimal for making accurate space weather predictions. We also cover the gaps in our current understanding related to the formation and eruption of the CME flux rope and physical processes that govern its evolution in the variable ambient solar windbackground that complicate the forecasting.