ALBERT

Description: Anorthite, the Ca-rich end-member of plagioclase feldspar, is a dominant mineral component of the Lunar highlands. Plagioclase feldspar is also found in comets, meteorites and stony asteroids. It is therefore expected to contribute to the population of interplanetary (and circumplanetary) dust grains within the solar system. After coating micron- and submicron-sized grains of Anorthite with a conductive layer of Platinum, the mineral was successfully accelerated to hypervelocity speeds in the Max Planck Institut für Kernphysik's Van de Graaff accelerator. We present impact ionization mass spectra generated following the impacts of anorthite grains with a prototype mass spectrometer (the Large Area Mass Analyser, LAMA) designed for use in space, and discuss the behavior of the spectra with increasing impact energy. Correlation analysis is used to identify the compositions and sources of cations present in the spectra, enabling the identification of several molecular cations (e.g., CaAlO2, CaSiO2, Ca2AlO3/CaAlSi2O2) which identify anorthite as the progenitor bulk grain material.

Description: The Stardust spacecraft collected thousands of particles from comet 81P/Wild 2 and returned them to Earth for laboratory study. The preliminary examination of these samples shows that the nonvolatile portion of the comet is an unequilibrated assortment of materials that have both presolar and solar system origin. The comet contains an abundance of silicate grains that are much larger than predictions of interstellar grain models, and many of these are high-temperature minerals that appear to have formed in the inner regions of the solar nebula. Their presence in a comet proves that the formation of the solar system included mixing on the grandest scales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Brownlee, Don -- Tsou, Peter -- Aleon, Jerome -- Alexander, Conel M O'd -- Araki, Tohru -- Bajt, Sasa -- Baratta, Giuseppe A -- Bastien, Ron -- Bland, Phil -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brearley, Adrian -- Brenker, F -- Brennan, Sean -- Bridges, John C -- Browning, Nigel D -- Brucato, John R -- Bullock, E -- Burchell, Mark J -- Busemann, Henner -- Butterworth, Anna -- Chaussidon, Marc -- Cheuvront, Allan -- Chi, Miaofang -- Cintala, Mark J -- Clark, B C -- Clemett, Simon J -- Cody, George -- Colangeli, Luigi -- Cooper, George -- Cordier, Patrick -- Daghlian, C -- Dai, Zurong -- D'Hendecourt, Louis -- Djouadi, Zahia -- Dominguez, Gerardo -- Duxbury, Tom -- Dworkin, Jason P -- Ebel, Denton S -- Economou, Thanasis E -- Fakra, Sirine -- Fairey, Sam A J -- Fallon, Stewart -- Ferrini, Gianluca -- Ferroir, T -- Fleckenstein, Holger -- Floss, Christine -- Flynn, George -- Franchi, Ian A -- Fries, Marc -- Gainsforth, Z -- Gallien, J-P -- Genge, Matt -- Gilles, Mary K -- Gillet, Philipe -- Gilmour, Jamie -- Glavin, Daniel P -- Gounelle, Matthieu -- Grady, Monica M -- Graham, Giles A -- Grant, P G -- Green, Simon F -- Grossemy, Faustine -- Grossman, Lawrence -- Grossman, Jeffrey N -- Guan, Yunbin -- Hagiya, Kenji -- Harvey, Ralph -- Heck, Philipp -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Hutcheon, Ian D -- Ignatyev, Konstantin -- Ishii, Hope -- Ito, Motoo -- Jacob, Damien -- Jacobsen, Chris -- Jacobsen, Stein -- Jones, Steven -- Joswiak, David -- Jurewicz, Amy -- Kearsley, Anton T -- Keller, Lindsay P -- Khodja, H -- Kilcoyne, A L David -- Kissel, Jochen -- Krot, Alexander -- Langenhorst, Falko -- Lanzirotti, Antonio -- Le, Loan -- Leshin, Laurie A -- Leitner, J -- Lemelle, L -- Leroux, Hugues -- Liu, Ming-Chang -- Luening, K -- Lyon, Ian -- Macpherson, Glen -- Marcus, Matthew A -- Marhas, Kuljeet -- Marty, Bernard -- Matrajt, Graciela -- McKeegan, Kevin -- Meibom, Anders -- Mennella, Vito -- Messenger, Keiko -- Messenger, Scott -- Mikouchi, Takashi -- Mostefaoui, Smail -- Nakamura, Tomoki -- Nakano, T -- Newville, M -- Nittler, Larry R -- Ohnishi, Ichiro -- Ohsumi, Kazumasa -- Okudaira, Kyoko -- Papanastassiou, Dimitri A -- Palma, Russ -- Palumbo, Maria E -- Pepin, Robert O -- Perkins, David -- Perronnet, Murielle -- Pianetta, P -- Rao, William -- Rietmeijer, Frans J M -- Robert, Francois -- Rost, D -- Rotundi, Alessandra -- Ryan, Robert -- Sandford, Scott A -- Schwandt, Craig S -- See, Thomas H -- Schlutter, Dennis -- Sheffield-Parker, J -- Simionovici, Alexandre -- Simon, Steven -- Sitnitsky, I -- Snead, Christopher J -- Spencer, Maegan K -- Stadermann, Frank J -- Steele, Andrew -- Stephan, Thomas -- Stroud, Rhonda -- Susini, Jean -- Sutton, S R -- Suzuki, Y -- Taheri, Mitra -- Taylor, Susan -- Teslich, Nick -- Tomeoka, Kazu -- Tomioka, Naotaka -- Toppani, Alice -- Trigo-Rodriguez, Josep M -- Troadec, David -- Tsuchiyama, Akira -- Tuzzolino, Anthony J -- Tyliszczak, Tolek -- Uesugi, K -- Velbel, Michael -- Vellenga, Joe -- Vicenzi, E -- Vincze, L -- Warren, Jack -- Weber, Iris -- Weisberg, Mike -- Westphal, Andrew J -- Wirick, Sue -- Wooden, Diane -- Wopenka, Brigitte -- Wozniakiewicz, Penelope -- Wright, Ian -- Yabuta, Hikaru -- Yano, Hajime -- Young, Edward D -- Zare, Richard N -- Zega, Thomas -- Ziegler, Karen -- Zimmerman, Laurent -- Zinner, Ernst -- Zolensky, Michael -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1711-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Washington, Seattle, WA 98195, USA. brownlee@astro.washington.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170289" 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: Images taken by the Stardust mission during its flyby of 81P/Wild 2 show the comet to be a 5-kilometer oblate body covered with remarkable topographic features, including unusual circular features that appear to be impact craters. The presence of high-angle slopes shows that the surface is cohesive and self-supporting. The comet does not appear to be a rubble pile, and its rounded shape is not directly consistent with the comet being a fragment of a larger body. The surface is active and yet it retains ancient terrain. Wild 2 appears to be in the early stages of its degradation phase as a small volatile-rich body in the inner solar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Brownlee, Donald E -- Horz, Friedrich -- Newburn, Ray L -- Zolensky, Michael -- Duxbury, Thomas C -- Sandford, Scott -- Sekanina, Zdenek -- Tsou, Peter -- Hanner, Martha S -- Clark, Benton C -- Green, Simon F -- Kissel, Jochen -- New York, N.Y. -- Science. 2004 Jun 18;304(5678):1764-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Washington, Seattle, WA 98195, USA. brownlee@astro.washington.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15205524" target="_blank"〉PubMed〈/a〉

Description: We present measurements of the dust particle flux and mass distribution from the Stardust Dust Flux Monitor Instrument (DFMI) throughout the flyby of comet 81P/Wild 2. In the particle mass regime from 10(-14) to 10(-7) kilograms, the spacecraft encountered regions of intense swarms of particles, together with bursts of activity corresponding to clouds of particles only a few hundred meters across. This fine-scale structure can be explained by particle fragmentation. We estimate that 2800 +/- 500 particles of diameter 15 micrometers or larger impacted the aerogel collectors, the largest being approximately 6 x 10(-7) kilograms, which dominates the total collected mass.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Tuzzolino, Anthony J -- Economou, Thanasis E -- Clark, Ben C -- Tsou, Peter -- Brownlee, Donald E -- Green, Simon F -- McDonnell, J A M -- McBride, Neil -- Colwell, Melusine T S H -- New York, N.Y. -- Science. 2004 Jun 18;304(5678):1776-80.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, 933 East 56th Street, Chicago, IL 60637, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15205527" target="_blank"〉PubMed〈/a〉

Description: We interpret the nucleus properties and jet activity from the Stardust spacecraft imaging and the onboard dust monitoring system data. Triangulation of 20 jets shows that 2 emanate from the nucleus dark side and 16 emanate from sources that are on slopes where the Sun's elevation is greater than predicted from the fitted triaxial ellipsoid. Seven sources, including five in the Mayo depression, coincide with relatively bright surface spots. Fitting the imaged jets, the spikelike temporal distribution of dust impacts indicates that the spacecraft crossed thin, densely populated sheets of particulate ejecta extending from small sources on the rotating nucleus, consistent with an emission cone model.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sekanina, Zdenek -- Brownlee, Donald E -- Economou, Thanasis E -- Tuzzolino, Anthony J -- Green, Simon F -- New York, N.Y. -- Science. 2004 Jun 18;304(5678):1769-74.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA. zs@sek.jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15205525" target="_blank"〉PubMed〈/a〉

Description: During Cassini's approach to Saturn, the Cosmic Dust Analyser (CDA) discovered streams of tiny (less than 20 nanometers) high-velocity (approximately 100 kilometers per second) dust particles escaping from the saturnian system. A fraction of these impactors originated from the outskirts of Saturn's dense A ring. The CDA time-of-flight mass spectrometer recorded 584 mass spectra from the stream particles. The particles consist predominantly of oxygen, silicon, and iron, with some evidence of water ice, ammonium, and perhaps carbon. The stream particles primarily consist of silicate materials, and this implies that the particles are impurities from the icy ring material rather than the ice particles themselves.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kempf, Sascha -- Srama, Ralf -- Postberg, Frank -- Burton, Marcia -- Green, Simon F -- Helfert, Stefan -- Hillier, Jon K -- McBride, Neil -- McDonnell, J Anthony M -- Moragas-Klostermeyer, Georg -- Roy, Mou -- Grun, Eberhard -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1274-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany. Sascha.Kempf@mpi-hd.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731446" target="_blank"〉PubMed〈/a〉

Description: Particles emanating from comet 81P/Wild 2 collided with the Stardust spacecraft at 6.1 kilometers per second, producing hypervelocity impact features on the collector surfaces that were returned to Earth. The morphologies of these surprisingly diverse features were created by particles varying from dense mineral grains to loosely bound, polymineralic aggregates ranging from tens of nanometers to hundreds of micrometers in size. The cumulative size distribution of Wild 2 dust is shallower than that of comet Halley, yet steeper than that of comet Grigg-Skjellerup.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Horz, Friedrich -- Bastien, Ron -- Borg, Janet -- Bradley, John P -- Bridges, John C -- Brownlee, Donald E -- Burchell, Mark J -- Chi, Miaofang -- Cintala, Mark J -- Dai, Zu Rong -- Djouadi, Zahia -- Dominguez, Gerardo -- Economou, Thanasis E -- Fairey, Sam A J -- Floss, Christine -- Franchi, Ian A -- Graham, Giles A -- Green, Simon F -- Heck, Philipp -- Hoppe, Peter -- Huth, Joachim -- Ishii, Hope -- Kearsley, Anton T -- Kissel, Jochen -- Leitner, Jan -- Leroux, Hugues -- Marhas, Kuljeet -- Messenger, Keiko -- Schwandt, Craig S -- See, Thomas H -- Snead, Christopher -- Stadermann, Frank J 1st -- Stephan, Thomas -- Stroud, Rhonda -- Teslich, Nick -- Trigo-Rodriguez, Josep M -- Tuzzolino, A J -- Troadec, David -- Tsou, Peter -- Warren, Jack -- Westphal, Andrew -- Wozniakiewicz, Penelope -- Wright, Ian -- Zinner, Ernst -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1716-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA. friedrich.p.horz@jsc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170290" target="_blank"〉PubMed〈/a〉

Description: Critical measurements for understanding accretion and the dust/gas ratio in the solar nebula, where planets were forming 4.5 billion years ago, are being obtained by the GIADA (Grain Impact Analyser and Dust Accumulator) experiment on the European Space Agency's Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko. Between 3.6 and 3.4 astronomical units inbound, GIADA and OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) detected 35 outflowing grains of mass 10(-10) to 10(-7) kilograms, and 48 grains of mass 10(-5) to 10(-2) kilograms, respectively. Combined with gas data from the MIRO (Microwave Instrument for the Rosetta Orbiter) and ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instruments, we find a dust/gas mass ratio of 4 +/- 2 averaged over the sunlit nucleus surface. A cloud of larger grains also encircles the nucleus in bound orbits from the previous perihelion. The largest orbiting clumps are meter-sized, confirming the dust/gas ratio of 3 inferred at perihelion from models of dust comae and trails.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Rotundi, Alessandra -- Sierks, Holger -- Della Corte, Vincenzo -- Fulle, Marco -- Gutierrez, Pedro J -- Lara, Luisa -- Barbieri, Cesare -- Lamy, Philippe L -- Rodrigo, Rafael -- Koschny, Detlef -- Rickman, Hans -- Keller, Horst Uwe -- Lopez-Moreno, Jose J -- Accolla, Mario -- Agarwal, Jessica -- A'Hearn, Michael F -- Altobelli, Nicolas -- Angrilli, Francesco -- Barucci, M Antonietta -- Bertaux, Jean-Loup -- Bertini, Ivano -- Bodewits, Dennis -- Bussoletti, Ezio -- Colangeli, Luigi -- Cosi, Massimo -- Cremonese, Gabriele -- Crifo, Jean-Francois -- Da Deppo, Vania -- Davidsson, Bjorn -- Debei, Stefano -- De Cecco, Mariolino -- Esposito, Francesca -- Ferrari, Marco -- Fornasier, Sonia -- Giovane, Frank -- Gustafson, Bo -- Green, Simon F -- Groussin, Olivier -- Grun, Eberhard -- Guttler, Carsten -- Herranz, Miguel L -- Hviid, Stubbe F -- Ip, Wing -- Ivanovski, Stavro -- Jeronimo, Jose M -- Jorda, Laurent -- Knollenberg, Joerg -- Kramm, Rainer -- Kuhrt, Ekkehard -- Kuppers, Michael -- Lazzarin, Monica -- Leese, Mark R -- Lopez-Jimenez, Antonio C -- Lucarelli, Francesca -- Lowry, Stephen C -- Marzari, Francesco -- Epifani, Elena Mazzotta -- McDonnell, J Anthony M -- Mennella, Vito -- Michalik, Harald -- Molina, Antonio -- Morales, Rafael -- Moreno, Fernando -- Mottola, Stefano -- Naletto, Giampiero -- Oklay, Nilda -- Ortiz, Jose L -- Palomba, Ernesto -- Palumbo, Pasquale -- Perrin, Jean-Marie -- Rodriguez, Julio -- Sabau, Lola -- Snodgrass, Colin -- Sordini, Roberto -- Thomas, Nicolas -- Tubiana, Cecilia -- Vincent, Jean-Baptiste -- Weissman, Paul -- Wenzel, Klaus-Peter -- Zakharov, Vladimir -- Zarnecki, John C -- New York, N.Y. -- Science. 2015 Jan 23;347(6220):aaa3905. doi: 10.1126/science.aaa3905.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Universita degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy. rotundi@uniparthenope.it. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Gottingen, Germany. ; Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. ; Osservatorio Astronomico, INAF, Via Tiepolo 11, 34143 Trieste, Italy. ; Instituto de Astrofisica de Andalucia, Consejo Superior de Investigaciones Cientificas (CSIC), P.O. Box 3008, 18080 Granada, Spain. ; Department of Physics and Astronomy, Padova University, Vicolo dell'Osservatorio 3, 35122 Padova, Italy. ; Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS and Aix-Marseille Universite, 13388 Marseille, France. ; Centro de Astrobiologia (Instituto Nacional de Tecnica Aerospacial-CSIC), 28691 Villanueva de la Canada, Madrid, Spain. International Space Science Institute, Hallerstrasse 6, CH-3012 Bern, Switzerland. ; Scientific Support Office, European Space Agency, 2201 Noordwijk, Netherlands. ; Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden. Polish Academy of Sciences Space Research Center, Bartycka 18A, PL-00716 Warszawa, Poland. ; Institute for Geophysics and Extraterrestrial Physics, Technische Universitat Braunschweig, Braunschweig 38106, Germany. ; Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Universita degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy. ; Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA. ; European Space Agency (ESA)-European Space Astronomy Center (ESAC), Camino Bajo del Castillo, s/n, 28692 Villanueva de la Canada, Madrid, Spagna. ; Department of Mechanical Engineering, University of Padova, via Venezia 1, 35131 Padova, Italy. ; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Universite Paris 06, Universite Paris-Diderot, 5 place Johannes Janssen, 92195 Meudon, France. ; Laboratoire Atmospheres, Milieux, Observations Spatiales, CNRS/Universite de Versailles Saint-Quentin-en-Yvelines/Institut Pierre-Simon Laplace, 11 boulevard d'Alembert, 78280 Guyancourt, France. ; University of Padova, Centro Interdipartimentale di Studi e Attivita Spaziali (CISAS), via Venezia 15, 35100 Padova, Italy. ; Universita degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy. ; ESA, European Space Research and Technology Centre (ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, Netherlands. ; Selex-ES, Via Albert Einstein, 35, 50013 Campi Bisenzio, Firenze, Italy. ; Osservatorio Astronomico di Padova, INAF, Vicolo dell'Osservatorio 5, 35122 Padova, Italy. ; Consiglio Nazionale delle Ricerche-Istituto di Fotonica e Nanotecnologie-Unita Operativa di Supporto Padova LUXOR, via Trasea 7, 35131 Padova, Italy. ; Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden. ; Universita di Trento, via Mesiano, 77, 38100 Trento, Italy. ; Osservatorio Astronomico di Capodimonte, INAF, Salita Moiariello, 16, 80133 Naples, Italy. ; Virginia Polytechnic Institute and State University, Blacksburg, VA 24061, USA. ; University of Florida, Gainesville, FL 32611, USA. ; Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK. ; Max-Planck-Institut fuer Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany. ; Institute of Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany. ; Institute for Space Science, National Central University, 300 Chung Da Road, 32054 Chung-Li, Taiwan. ; The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK. ; Department of Physics, University of Padova, 35131 Padova, Italy. ; Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK. The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK. Unispacekent, Canterbury CT2 8EF, UK. ; Institut fur Datentechnik und Kommunikationsnetze, 38106 Braunschweig, Germany. ; Departamento de Fisica Aplicada, Universidad de Granada, Facultad de Ciencias, Avenida Severo Ochoa, s/n, 18071 Granada, Spain. ; Department of Information Engineering, Padova University, via Gradenigo 6, 35131 Padova, Italy. ; Laboratoire Atmospheres, Milieux, Observations Spatiales, CNRS/Universite de Versailles Saint-Quentin-en-Yvelines/Institut Pierre-Simon Laplace, 11 boulevard d'Alembert, 78280 Guyancourt, France. Observatoire de Haute Provence OSU Pytheas UMS 2244 CNRS-AMU, 04870 Saint Michel l'Observatoire, France. ; Instituto Nacional de Tecnica Aeroespacial, Carretera de Ajalvir, p.k. 4, 28850 Torrejon de Ardoz, Madrid, Spain. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Gottingen, Germany. Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK. ; Physikalisches Institut, Sidlerstrasse 5, University of Bern, 3012 Bern, Switzerland. ; Planetary Science Section, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA. ; International Space Science Institute, Hallerstrasse 6, CH-3012 Bern, Switzerland. Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25613898" target="_blank"〉PubMed〈/a〉

Description: Author(s): N. Murdoch, B. Rozitis, K. Nordstrom, S. F. Green, P. Michel, T.-L. de Lophem, and W. Losert [Phys. Rev. Lett. 110, 029902] Published Fri Jan 11, 2013