ALBERT

Description: Airborne and ground-based measurements during the CalNex (California Research at the Nexus of Air Quality and Climate Change) field study in May/June 2010 show a weekend effect in ozone in the South Coast Air Basin (SoCAB) consistent with previous observations. The well-known and much-studied weekend ozone effect has been attributed to weekend reductions in nitrogen oxide (NOx = NO + NO2) emissions, which affect ozone levels via two processes: (1) reduced ozone loss by titration and (2) enhanced photochemical production of ozone due to an increased ratio of non-methane volatile organic compounds (VOCs) to NOx. In accord with previous assessments, the 2010 airborne and ground-based data show an average decrease in NOx of 46 ± 11% and 34 ± 4%, respectively, and an average increase in VOC/NOx ratio of 48 ± 8% and 43 ± 22%, respectively, on weekends. This work extends current understanding of the weekend ozone effect in the SoCAB by identifying its major causes and quantifying their relative importance from the available CalNex data. Increased weekend production of a VOC-NOx oxidation product, peroxyacetyl nitrate, compared to a radical termination product, nitric acid, indicates a significant contribution from increased photochemical production on weekends. Weekday-to-weekend differences in the products of NOx oxidation show 45 ± 13% and 42 ± 12% more extensive photochemical processing and, when compared with odd oxygen (Ox = O3 + NO2), 51 ± 14% and 22 ± 17% greater ozone production efficiency on weekends in the airborne and ground-based data, respectively, indicating that both contribute to higher weekend ozone levels in the SoCAB.

Description: Infrared spectral properties of silicate grains in interplanetary dust particles (IDPs) were compared with those of astronomical silicates. The approximately 10-micrometer silicon-oxygen stretch bands of IDPs containing enstatite (MgSiO3), forsterite (Mg2SiO4), and glass with embedded metal and sulfides (GEMS) exhibit fine structure and bandwidths similar to those of solar system comets and some pre-main sequence Herbig Ae/Be stars. Some GEMS exhibit a broad, featureless silicon-oxygen stretch band similar to those observed in interstellar molecular clouds and young stellar objects. These GEMS provide a spectral match to astronomical "amorphous" silicates, one of the fundamental building blocks from which the solar system is presumed to have formed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bradley, J P -- Keller, L P -- Snow, T P -- Hanner, M S -- Flynn, G J -- Gezo, J C -- Clemett, S J -- Brownlee, D E -- Bowey, J E -- New York, N.Y. -- Science. 1999 Sep 10;285(5434):1716-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉MVA Inc., Norcross, GA 30093, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10481004" target="_blank"〉PubMed〈/a〉

Description: Organics found in comet 81P/Wild 2 samples show a heterogeneous and unequilibrated distribution in abundance and composition. Some organics are similar, but not identical, to those in interplanetary dust particles and carbonaceous meteorites. A class of aromatic-poor organic material is also present. The organics are rich in oxygen and nitrogen compared with meteoritic organics. Aromatic compounds are present, but the samples tend to be relatively poorer in aromatics than are meteorites and interplanetary dust particles. The presence of deuterium and nitrogen-15 excesses suggest that some organics have an interstellar/protostellar heritage. Although the variable extent of modification of these materials by impact capture is not yet fully constrained, a diverse suite of organic compounds is present and identifiable within the returned samples.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sandford, Scott A -- Aleon, Jerome -- Alexander, Conel M O'd -- Araki, Tohru -- Bajt, Sasa -- Baratta, Giuseppe A -- Borg, Janet -- Bradley, John P -- Brownlee, Donald E -- Brucato, John R -- Burchell, Mark J -- Busemann, Henner -- Butterworth, Anna -- Clemett, Simon J -- Cody, George -- Colangeli, Luigi -- Cooper, George -- D'Hendecourt, Louis -- Djouadi, Zahia -- Dworkin, Jason P -- Ferrini, Gianluca -- Fleckenstein, Holger -- Flynn, George J -- Franchi, Ian A -- Fries, Marc -- Gilles, Mary K -- Glavin, Daniel P -- Gounelle, Matthieu -- Grossemy, Faustine -- Jacobsen, Chris -- Keller, Lindsay P -- Kilcoyne, A L David -- Leitner, Jan -- Matrajt, Graciela -- Meibom, Anders -- Mennella, Vito -- Mostefaoui, Smail -- Nittler, Larry R -- Palumbo, Maria E -- Papanastassiou, Dimitri A -- Robert, Francois -- Rotundi, Alessandra -- Snead, Christopher J -- Spencer, Maegan K -- Stadermann, Frank J -- Steele, Andrew -- Stephan, Thomas -- Tsou, Peter -- Tyliszczak, Tolek -- Westphal, Andrew J -- Wirick, Sue -- Wopenka, Brigitte -- Yabuta, Hikaru -- Zare, Richard N -- Zolensky, Michael E -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1720-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astrophysics Branch, NASA-Ames Research Center, Moffett Field, CA 94035, USA. ssandford@mail.arc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170291" target="_blank"〉PubMed〈/a〉

Description: We measured the elemental compositions of material from 23 particles in aerogel and from residue in seven craters in aluminum foil that was collected during passage of the Stardust spacecraft through the coma of comet 81P/Wild 2. These particles are chemically heterogeneous at the largest size scale analyzed ( approximately 180 ng). The mean elemental composition of this Wild 2 material is consistent with the CI meteorite composition, which is thought to represent the bulk composition of the solar system, for the elements Mg, Si, Mn, Fe, and Ni to 35%, and for Ca and Ti to 60%. The elements Cu, Zn, and Ga appear enriched in this Wild 2 material, which suggests that the CI meteorites may not represent the solar system composition for these moderately volatile minor elements.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flynn, George J -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brenker, Frank E -- Brennan, Sean -- Bridges, John -- Brownlee, Don E -- Bullock, Emma S -- Burghammer, Manfred -- Clark, Benton C -- Dai, Zu Rong -- Daghlian, Charles P -- Djouadi, Zahia -- Fakra, Sirine -- Ferroir, Tristan -- Floss, Christine -- Franchi, Ian A -- Gainsforth, Zack -- Gallien, Jean-Paul -- Gillet, Philippe -- Grant, Patrick G -- Graham, Giles A -- Green, Simon F -- Grossemy, Faustine -- Heck, Philipp R -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Ignatyev, Konstantin -- Ishii, Hope A -- Janssens, Koen -- Joswiak, David -- Kearsley, Anton T -- Khodja, Hicham -- Lanzirotti, Antonio -- Leitner, Jan -- Lemelle, Laurence -- Leroux, Hugues -- Luening, Katharina -- Macpherson, Glenn J -- Marhas, Kuljeet K -- Marcus, Matthew A -- Matrajt, Graciela -- Nakamura, Tomoki -- Nakamura-Messenger, Keiko -- Nakano, Tsukasa -- Newville, Matthew -- Papanastassiou, Dimitri A -- Pianetta, Piero -- Rao, William -- Riekel, Christian -- Rietmeijer, Frans J M -- Rost, Detlef -- Schwandt, Craig S -- See, Thomas H -- Sheffield-Parker, Julie -- Simionovici, Alexandre -- Sitnitsky, Ilona -- Snead, Christopher J -- Stadermann, Frank J -- Stephan, Thomas -- Stroud, Rhonda M -- Susini, Jean -- Suzuki, Yoshio -- Sutton, Stephen R -- Taylor, Susan -- Teslich, Nick -- Troadec, D -- Tsou, Peter -- Tsuchiyama, Akira -- Uesugi, Kentaro -- Vekemans, Bart -- Vicenzi, Edward P -- Vincze, Laszlo -- Westphal, Andrew J -- Wozniakiewicz, Penelope -- Zinner, Ernst -- Zolensky, Michael E -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1731-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, State University of New York at Plattsburgh, 101 Broad Street, Plattsburgh, NY 12901, USA. george.flynn@plattsburgh.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170294" target="_blank"〉PubMed〈/a〉

Description: Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream. More than 50 spacecraft debris particles were also identified. The interstellar dust candidates are readily distinguished from debris impacts on the basis of elemental composition and/or impact trajectory. The seven candidate interstellar particles are diverse in elemental composition, crystal structure, and size. The presence of crystalline grains and multiple iron-bearing phases, including sulfide, in some particles indicates that individual interstellar particles diverge from any one representative model of interstellar dust inferred from astronomical observations and theory.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Westphal, Andrew J -- Stroud, Rhonda M -- Bechtel, Hans A -- Brenker, Frank E -- Butterworth, Anna L -- Flynn, George J -- Frank, David R -- Gainsforth, Zack -- Hillier, Jon K -- Postberg, Frank -- Simionovici, Alexandre S -- Sterken, Veerle J -- Nittler, Larry R -- Allen, Carlton -- Anderson, David -- Ansari, Asna -- Bajt, Sasa -- Bastien, Ron K -- Bassim, Nabil -- Bridges, John -- Brownlee, Donald E -- Burchell, Mark -- Burghammer, Manfred -- Changela, Hitesh -- Cloetens, Peter -- Davis, Andrew M -- Doll, Ryan -- Floss, Christine -- Grun, Eberhard -- Heck, Philipp R -- Hoppe, Peter -- Hudson, Bruce -- Huth, Joachim -- Kearsley, Anton -- King, Ashley J -- Lai, Barry -- Leitner, Jan -- Lemelle, Laurence -- Leonard, Ariel -- Leroux, Hugues -- Lettieri, Robert -- Marchant, William -- Ogliore, Ryan -- Ong, Wei Jia -- Price, Mark C -- Sandford, Scott A -- Sans Tresseras, Juan-Angel -- Schmitz, Sylvia -- Schoonjans, Tom -- Schreiber, Kate -- Silversmit, Geert -- Sole, Vicente A -- Srama, Ralf -- Stadermann, Frank -- Stephan, Thomas -- Stodolna, Julien -- Sutton, Stephen -- Trieloff, Mario -- Tsou, Peter -- Tyliszczak, Tolek -- Vekemans, Bart -- Vincze, Laszlo -- Von Korff, Joshua -- Wordsworth, Naomi -- Zevin, Daniel -- Zolensky, Michael E -- 30714 Stardust@home dusters -- New York, N.Y. -- Science. 2014 Aug 15;345(6198):786-91. doi: 10.1126/science.1252496.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA, USA. westphal@ssl.berkeley.edu. ; Materials Science and Technology Division, Naval Research Laboratory, Washington, DC, USA. ; Advanced Light Source, Lawrence Berkeley Laboratory, Berkeley, CA, USA. ; Geoscience Institute, Goethe University Frankfurt, Frankfurt, Germany. ; Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA, USA. ; State University of New York at Plattsburgh, Plattsburgh, NY, USA. ; Jacobs Technology/ESCG, NASA Johnson Space Center (JSC), Houston, TX, USA. ; Institut fur Geowissenschaften, University of Heidelberg, Germany. ; Institut des Sciences de la Terre, Observatoire des Sciences de l'Univers de Grenoble, Grenoble, France. ; Institut fur Raumfahrtsysteme (IRS), University of Stuttgart, Stuttgart, Germany. IGEP, TU Braunschweig, Braunschweig, Germany. Max Planck Institut fur Kernphysik, Heidelberg, Germany. International Space Sciences Institute, Bern, Switzerland. ; Carnegie Institution of Washington, Washington, DC, USA. ; Astromaterials Research and Exploration Science, NASA JSC, Houston, TX, USA. ; Field Museum of Natural History, Chicago, IL, USA. ; Deutsches Elektronen-Synchrotron, Hamburg, Germany. ; Space Research Centre, University of Leicester, Leicester, UK. ; Department of Astronomy, University of Washington, Seattle, WA, USA. ; University of Kent, Canterbury, Kent, UK. ; University of Ghent, Ghent, Belgium. ; University of New Mexico. ; European Synchrotron Radiation Facility (ESRF), Grenoble, France. ; University of Chicago, Chicago, IL, USA. ; Washington University, St. Louis, MO, USA. ; Max-Planck-Institut fur Kernphysik, Heidelberg, Germany. ; International Space Sciences Institute, Bern, Switzerland. ; Max-Planck-Institut fur Chemie, Mainz, Germany. ; 615 William Street, Apt 405, Midland, Ontario, Canada. ; Natural History Museum, London, UK. ; Advanced Photon Source, Argonne National Laboratory, Lemont, IL, USA. ; Ecole Normale Superieure de Lyon, Lyon, France. ; University Lille 1, France. ; University of Hawai'i at Manoa, Honolulu, HI, USA. ; NASA Ames Research Center, Moffett Field, CA, USA. ; IRS, University Stuttgart, Stuttgart, Germany. ; Jet Propulsion Laboratory, Pasadena, CA, USA. ; Wexbury, Farthing Green Lane, Stoke Poges, South Buckinghamshire, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25124433" target="_blank"〉PubMed〈/a〉

Description: Noble gas elemental and isotopic ratios were measured in a group of 13 "chondritic" stratospheric dust particles. Neon and argon are present in "solar" proportions; xenon appears to be dominated by contributions from "planetary" sources. The apparent xenon concentration is higher than that measured in any bulk meteorite, approaching the concentration found in the noble gas-rich, acid-insoluble residues from carbonaceous chondrites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hudson, B -- Flynn, G J -- Fraundorf, P -- Hohenberg, C M -- Shirck, J -- New York, N.Y. -- Science. 1981 Jan 23;211(4480):383-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748271" target="_blank"〉PubMed〈/a〉