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  • 1
    Publication Date: 2000-09-23
    Description: We report major element composition ratios for regions of the asteroid 433 Eros imaged during two solar flares and quiet sun conditions during the period of May to July 2000. Low aluminum abundances for all regions argue against global differentiation of Eros. Magnesium/silicon, aluminum/silicon, calcium/silicon, and iron/silicon ratios are best interpreted as a relatively primitive, chondritic composition. Marked depletions in sulfur and possible aluminum and calcium depletions, relative to ordinary chondrites, may represent signatures of limited partial melting or impact volatilization.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Trombka -- Squyres -- Bruckner -- Boynton -- Reedy -- McCoy -- Gorenstein -- Evans -- Arnold -- Starr -- Nittler -- Murphy -- Mikheeva I -- McNutt Jr -- McClanahan -- McCartney -- Goldsten -- Gold -- Floyd -- Clark -- Burbine -- Bhangoo -- Bailey -- Petaev -- New York, N.Y. -- Science. 2000 Sep 22;289(5487):2101-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Goddard Space Flight Center, Code 691, Greenbelt, MD 20771, USA. Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. Max-Planck-Institut fur Chemie, Postfach 3060, D-55020 Mainz, Germany. Department of Planetary Science, Spac.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11000107" target="_blank"〉PubMed〈/a〉
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  • 2
    Publication Date: 2006-12-16
    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〉
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  • 3
    Publication Date: 2006-05-06
    Description: Organic matter in extraterrestrial materials has isotopic anomalies in hydrogen and nitrogen that suggest an origin in the presolar molecular cloud or perhaps in the protoplanetary disk. Interplanetary dust particles are generally regarded as the most primitive solar system matter available, in part because until recently they exhibited the most extreme isotope anomalies. However, we show that hydrogen and nitrogen isotopic compositions in carbonaceous chondrite organic matter reach and even exceed those found in interplanetary dust particles. Hence, both meteorites (originating from the asteroid belt) and interplanetary dust particles (possibly from comets) preserve primitive organics that were a component of the original building blocks of the solar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Busemann, Henner -- Young, Andrea F -- Alexander, Conel M O'd -- Hoppe, Peter -- Mukhopadhyay, Sujoy -- Nittler, Larry R -- New York, N.Y. -- Science. 2006 May 5;312(5774):727-30.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015, USA. busemann@dtm.ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16675696" target="_blank"〉PubMed〈/a〉
    Keywords: *Cosmic Dust ; Deuterium/*analysis ; Evolution, Planetary ; *Meteoroids ; Nitrogen Isotopes/*analysis ; Organic Chemicals/*analysis ; *Solar System ; Temperature
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  • 4
    Publication Date: 2006-12-16
    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〉
    Keywords: Carbon/analysis ; Cosmic Dust/analysis ; Deuterium/analysis ; *Meteoroids ; Nitrogen/analysis ; Nitrogen Isotopes/analysis ; Organic Chemicals/*analysis ; Oxygen/analysis ; Polycyclic Hydrocarbons, Aromatic/analysis ; Spacecraft
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  • 5
    Publication Date: 2008-07-05
    Description: Observations by MESSENGER show that Mercury's magnetosphere is immersed in a comet-like cloud of planetary ions. The most abundant, Na+, is broadly distributed but exhibits flux maxima in the magnetosheath, where the local plasma flow speed is high, and near the spacecraft's closest approach, where atmospheric density should peak. The magnetic field showed reconnection signatures in the form of flux transfer events, azimuthal rotations consistent with Kelvin-Helmholtz waves along the magnetopause, and extensive ultralow-frequency wave activity. Two outbound current sheet boundaries were observed, across which the magnetic field decreased in a manner suggestive of a double magnetopause. The separation of these current layers, comparable to the gyro-radius of a Na+ pickup ion entering the magnetosphere after being accelerated in the magnetosheath, may indicate a planetary ion boundary layer.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Slavin, James A -- Acuna, Mario H -- Anderson, Brian J -- Baker, Daniel N -- Benna, Mehdi -- Gloeckler, George -- Gold, Robert E -- Ho, George C -- Killen, Rosemary M -- Korth, Haje -- Krimigis, Stamatios M -- McNutt, Ralph L Jr -- Nittler, Larry R -- Raines, Jim M -- Schriver, David -- Solomon, Sean C -- Starr, Richard D -- Travnicek, Pavel -- Zurbuchen, Thomas H -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):85-9. doi: 10.1126/science.1159040.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. james.a.slavin@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599776" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2011-10-01
    Description: X-ray fluorescence spectra obtained by the MESSENGER spacecraft orbiting Mercury indicate that the planet's surface differs in composition from those of other terrestrial planets. Relatively high Mg/Si and low Al/Si and Ca/Si ratios rule out a lunarlike feldspar-rich crust. The sulfur abundance is at least 10 times higher than that of the silicate portion of Earth or the Moon, and this observation, together with a low surface Fe abundance, supports the view that Mercury formed from highly reduced precursor materials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particles. Low Fe and Ti abundances do not support the proposal that opaque oxides of these elements contribute substantially to Mercury's low and variable surface reflectance.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nittler, Larry R -- Starr, Richard D -- Weider, Shoshana Z -- McCoy, Timothy J -- Boynton, William V -- Ebel, Denton S -- Ernst, Carolyn M -- Evans, Larry G -- Goldsten, John O -- Hamara, David K -- Lawrence, David J -- McNutt, Ralph L Jr -- Schlemm, Charles E 2nd -- Solomon, Sean C -- Sprague, Ann L -- New York, N.Y. -- Science. 2011 Sep 30;333(6051):1847-50. doi: 10.1126/science.1211567.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. lnittler@ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21960623" target="_blank"〉PubMed〈/a〉
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  • 7
    Publication Date: 2011-10-01
    Description: The MESSENGER Gamma-Ray Spectrometer measured the average surface abundances of the radioactive elements potassium (K, 1150 +/- 220 parts per million), thorium (Th, 220 +/- 60 parts per billion), and uranium (U, 90 +/- 20 parts per billion) in Mercury's northern hemisphere. The abundance of the moderately volatile element K, relative to Th and U, is inconsistent with physical models for the formation of Mercury requiring extreme heating of the planet or its precursor materials, and supports formation from volatile-containing material comparable to chondritic meteorites. Abundances of K, Th, and U indicate that internal heat production has declined substantially since Mercury's formation, consistent with widespread volcanism shortly after the end of late heavy bombardment 3.8 billion years ago and limited, isolated volcanic activity since.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Peplowski, Patrick N -- Evans, Larry G -- Hauck, Steven A 2nd -- McCoy, Timothy J -- Boynton, William V -- Gillis-Davis, Jeffery J -- Ebel, Denton S -- Goldsten, John O -- Hamara, David K -- Lawrence, David J -- McNutt, Ralph L Jr -- Nittler, Larry R -- Solomon, Sean C -- Rhodes, Edgar A -- Sprague, Ann L -- Starr, Richard D -- Stockstill-Cahill, Karen R -- New York, N.Y. -- Science. 2011 Sep 30;333(6051):1850-2. doi: 10.1126/science.1211576.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. patrick.peplowski@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21960624" target="_blank"〉PubMed〈/a〉
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  • 8
    Publication Date: 2011-06-11
    Description: The complex suite of organic materials in carbonaceous chondrite meteorites probably originally formed in the interstellar medium and/or the solar protoplanetary disk, but was subsequently modified in the meteorites' asteroidal parent bodies. The mechanisms of formation and modification are still very poorly understood. We carried out a systematic study of variations in the mineralogy, petrology, and soluble and insoluble organic matter in distinct fragments of the Tagish Lake meteorite. The variations correlate with indicators of parent body aqueous alteration. At least some molecules of prebiotic importance formed during the alteration.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Herd, Christopher D K -- Blinova, Alexandra -- Simkus, Danielle N -- Huang, Yongsong -- Tarozo, Rafael -- Alexander, Conel M O'D -- Gyngard, Frank -- Nittler, Larry R -- Cody, George D -- Fogel, Marilyn L -- Kebukawa, Yoko -- Kilcoyne, A L David -- Hilts, Robert W -- Slater, Greg F -- Glavin, Daniel P -- Dworkin, Jason P -- Callahan, Michael P -- Elsila, Jamie E -- De Gregorio, Bradley T -- Stroud, Rhonda M -- New York, N.Y. -- Science. 2011 Jun 10;332(6035):1304-7. doi: 10.1126/science.1203290.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Alberta T6G 2E3, Canada. herd@ualberta.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21659601" target="_blank"〉PubMed〈/a〉
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  • 9
    Publication Date: 2012-07-17
    Description: Determining the source(s) of hydrogen, carbon, and nitrogen accreted by Earth is important for understanding the origins of water and life and for constraining dynamical processes that operated during planet formation. Chondritic meteorites are asteroidal fragments that retain records of the first few million years of solar system history. The deuterium/hydrogen (D/H) values of water in carbonaceous chondrites are distinct from those in comets and Saturn's moon Enceladus, implying that they formed in a different region of the solar system, contrary to predictions of recent dynamical models. The D/H values of water in carbonaceous chondrites also argue against an influx of water ice from the outer solar system, which has been invoked to explain the nonsolar oxygen isotopic composition of the inner solar system. The bulk hydrogen and nitrogen isotopic compositions of CI chondrites suggest that they were the principal source of Earth's volatiles.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Alexander, C M O'D -- Bowden, R -- Fogel, M L -- Howard, K T -- Herd, C D K -- Nittler, L R -- New York, N.Y. -- Science. 2012 Aug 10;337(6095):721-3. doi: 10.1126/science.1223474. Epub 2012 Jul 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015, USA. alexander@dtm.ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22798405" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon/*analysis ; Carbon Isotopes/analysis ; Deuterium/analysis ; *Earth (Planet) ; Evolution, Planetary ; Hydrogen/*analysis ; Ice ; *Minor Planets ; Nitrogen/*analysis ; Nitrogen Isotopes/analysis ; Oxygen Isotopes/analysis ; *Planets ; Water
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  • 10
    Publication Date: 2012-12-01
    Description: Measurements by the Neutron Spectrometer on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft show decreases in the flux of epithermal and fast neutrons from Mercury's north polar region that are consistent with the presence of water ice in permanently shadowed regions. The neutron data indicate that Mercury's radar-bright polar deposits contain, on average, a hydrogen-rich layer more than tens of centimeters thick beneath a surficial layer 10 to 30 cm thick that is less rich in hydrogen. Combined neutron and radar data are best matched if the buried layer consists of nearly pure water ice. The upper layer contains less than 25 weight % water-equivalent hydrogen. The total mass of water at Mercury's poles is inferred to be 2 x 10(16) to 10(18) grams and is consistent with delivery by comets or volatile-rich asteroids.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lawrence, David J -- Feldman, William C -- Goldsten, John O -- Maurice, Sylvestre -- Peplowski, Patrick N -- Anderson, Brian J -- Bazell, David -- McNutt, Ralph L Jr -- Nittler, Larry R -- Prettyman, Thomas H -- Rodgers, Douglas J -- Solomon, Sean C -- Weider, Shoshana Z -- New York, N.Y. -- Science. 2013 Jan 18;339(6117):292-6. doi: 10.1126/science.1229953. Epub 2012 Nov 29.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. david.j.lawrence@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23196909" target="_blank"〉PubMed〈/a〉
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