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  • 1
    Publication Date: 2010-02-26
    Description: The class of exotic Jupiter-mass planets that orbit very close to their parent stars were not explicitly expected before their discovery. The recently discovered transiting planet WASP-12b has a mass M = 1.4 +/- 0.1 Jupiter masses (M(J)), a mean orbital distance of only 3.1 stellar radii (meaning it is subject to intense tidal forces), and a period of 1.1 days. Its radius 1.79 +/- 0.09R(J) is unexpectedly large and its orbital eccentricity 0.049 +/- 0.015 is even more surprising because such close orbits are usually quickly circularized. Here we report an analysis of its properties, which reveals that the planet is losing mass to its host star at a rate of about 10(-7)M(J) per year. The planet's surface is distorted by the star's gravity and the light curve produced by its prolate shape will differ by about ten per cent from that of a spherical planet. We conclude that dissipation of the star's tidal perturbation in the planet's convective envelope provides the energy source for its large volume. We predict up to 10 mJy CO band-head (2.292 mum) emission from a tenuous disk around the host star, made up of tidally stripped planetary gas. It may also contain a detectable resonant super-Earth, as a hypothetical perturber that continually stirs up WASP-12b's eccentricity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Li, Shu-Lin -- Miller, N -- Lin, Douglas N C -- Fortney, Jonathan J -- England -- Nature. 2010 Feb 25;463(7284):1054-6. doi: 10.1038/nature08715.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20182506" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 2
    Publication Date: 2011-09-17
    Description: We report the detection of a planet whose orbit surrounds a pair of low-mass stars. Data from the Kepler spacecraft reveal transits of the planet across both stars, in addition to the mutual eclipses of the stars, giving precise constraints on the absolute dimensions of all three bodies. The planet is comparable to Saturn in mass and size and is on a nearly circular 229-day orbit around its two parent stars. The eclipsing stars are 20 and 69% as massive as the Sun and have an eccentric 41-day orbit. The motions of all three bodies are confined to within 0.5 degrees of a single plane, suggesting that the planet formed within a circumbinary disk.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Doyle, Laurance R -- Carter, Joshua A -- Fabrycky, Daniel C -- Slawson, Robert W -- Howell, Steve B -- Winn, Joshua N -- Orosz, Jerome A -- Prsa, Andrej -- Welsh, William F -- Quinn, Samuel N -- Latham, David -- Torres, Guillermo -- Buchhave, Lars A -- Marcy, Geoffrey W -- Fortney, Jonathan J -- Shporer, Avi -- Ford, Eric B -- Lissauer, Jack J -- Ragozzine, Darin -- Rucker, Michael -- Batalha, Natalie -- Jenkins, Jon M -- Borucki, William J -- Koch, David -- Middour, Christopher K -- Hall, Jennifer R -- McCauliff, Sean -- Fanelli, Michael N -- Quintana, Elisa V -- Holman, Matthew J -- Caldwell, Douglas A -- Still, Martin -- Stefanik, Robert P -- Brown, Warren R -- Esquerdo, Gilbert A -- Tang, Sumin -- Furesz, Gabor -- Geary, John C -- Berlind, Perry -- Calkins, Michael L -- Short, Donald R -- Steffen, Jason H -- Sasselov, Dimitar -- Dunham, Edward W -- Cochran, William D -- Boss, Alan -- Haas, Michael R -- Buzasi, Derek -- Fischer, Debra -- New York, N.Y. -- Science. 2011 Sep 16;333(6049):1602-6. doi: 10.1126/science.1210923.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Carl Sagan Center for the Study of Life in the Universe, SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA. ldoyle@seti.org〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21921192" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 3
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    American Association for the Advancement of Science (AAAS)
    Publication Date: 2004-09-09
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fortney, Jonathan J -- New York, N.Y. -- Science. 2004 Sep 3;305(5689):1414-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Systems Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA. jfortney@arc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15353790" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Evolution, Planetary ; Gravitation ; *Helium ; *Hydrogen ; *Jupiter ; Mathematics ; Models, Structural ; Pressure ; *Saturn ; Spacecraft ; Temperature
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
    Publication Date: 2013-11-01
    Description: Planets with sizes between that of Earth (with radius R Earth symbol) and Neptune (about 4R Earth symbol) are now known to be common around Sun-like stars. Most such planets have been discovered through the transit technique, by which the planet's size can be determined from the fraction of starlight blocked by the planet as it passes in front of its star. Measuring the planet's mass--and hence its density, which is a clue to its composition--is more difficult. Planets of size 2-4R Earth symbol have proved to have a wide range of densities, implying a diversity of compositions, but these measurements did not extend to planets as small as Earth. Here we report Doppler spectroscopic measurements of the mass of the Earth-sized planet Kepler-78b, which orbits its host star every 8.5 hours (ref. 6). Given a radius of 1.20 +/- 0.09 R Earth symbol and a mass of 1.69 +/- 0.41 R Earth symbol, the planet's mean density of 5.3 +/- 1.8 g cm(-3) is similar to Earth's, suggesting a composition of rock and iron.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Howard, Andrew W -- Sanchis-Ojeda, Roberto -- Marcy, Geoffrey W -- Johnson, John Asher -- Winn, Joshua N -- Isaacson, Howard -- Fischer, Debra A -- Fulton, Benjamin J -- Sinukoff, Evan -- Fortney, Jonathan J -- England -- Nature. 2013 Nov 21;503(7476):381-4. doi: 10.1038/nature12767. Epub 2013 Oct 30.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24172898" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 5
    Publication Date: 2013-02-22
    Description: Since the discovery of the first exoplanets, it has been known that other planetary systems can look quite unlike our own. Until fairly recently, we have been able to probe only the upper range of the planet size distribution, and, since last year, to detect planets that are the size of Earth or somewhat smaller. Hitherto, no planets have been found that are smaller than those we see in the Solar System. Here we report a planet significantly smaller than Mercury. This tiny planet is the innermost of three that orbit the Sun-like host star, which we have designated Kepler-37. Owing to its extremely small size, similar to that of the Moon, and highly irradiated surface, the planet, Kepler-37b, is probably rocky with no atmosphere or water, similar to Mercury.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Barclay, Thomas -- Rowe, Jason F -- Lissauer, Jack J -- Huber, Daniel -- Fressin, Francois -- Howell, Steve B -- Bryson, Stephen T -- Chaplin, William J -- Desert, Jean-Michel -- Lopez, Eric D -- Marcy, Geoffrey W -- Mullally, Fergal -- Ragozzine, Darin -- Torres, Guillermo -- Adams, Elisabeth R -- Agol, Eric -- Barrado, David -- Basu, Sarbani -- Bedding, Timothy R -- Buchhave, Lars A -- Charbonneau, David -- Christiansen, Jessie L -- Christensen-Dalsgaard, Jorgen -- Ciardi, David -- Cochran, William D -- Dupree, Andrea K -- Elsworth, Yvonne -- Everett, Mark -- Fischer, Debra A -- Ford, Eric B -- Fortney, Jonathan J -- Geary, John C -- Haas, Michael R -- Handberg, Rasmus -- Hekker, Saskia -- Henze, Christopher E -- Horch, Elliott -- Howard, Andrew W -- Hunter, Roger C -- Isaacson, Howard -- Jenkins, Jon M -- Karoff, Christoffer -- Kawaler, Steven D -- Kjeldsen, Hans -- Klaus, Todd C -- Latham, David W -- Li, Jie -- Lillo-Box, Jorge -- Lund, Mikkel N -- Lundkvist, Mia -- Metcalfe, Travis S -- Miglio, Andrea -- Morris, Robert L -- Quintana, Elisa V -- Stello, Dennis -- Smith, Jeffrey C -- Still, Martin -- Thompson, Susan E -- England -- Nature. 2013 Feb 28;494(7438):452-4. doi: 10.1038/nature11914. Epub 2013 Feb 20.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, California 94035, USA. thomas.barclay@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23426260" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2012-01-13
    Description: Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars (binaries). Although long anticipated, the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than approximately 1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Welsh, William F -- Orosz, Jerome A -- Carter, Joshua A -- Fabrycky, Daniel C -- Ford, Eric B -- Lissauer, Jack J -- Prsa, Andrej -- Quinn, Samuel N -- Ragozzine, Darin -- Short, Donald R -- Torres, Guillermo -- Winn, Joshua N -- Doyle, Laurance R -- Barclay, Thomas -- Batalha, Natalie -- Bloemen, Steven -- Brugamyer, Erik -- Buchhave, Lars A -- Caldwell, Caroline -- Caldwell, Douglas A -- Christiansen, Jessie L -- Ciardi, David R -- Cochran, William D -- Endl, Michael -- Fortney, Jonathan J -- Gautier, Thomas N 3rd -- Gilliland, Ronald L -- Haas, Michael R -- Hall, Jennifer R -- Holman, Matthew J -- Howard, Andrew W -- Howell, Steve B -- Isaacson, Howard -- Jenkins, Jon M -- Klaus, Todd C -- Latham, David W -- Li, Jie -- Marcy, Geoffrey W -- Mazeh, Tsevi -- Quintana, Elisa V -- Robertson, Paul -- Shporer, Avi -- Steffen, Jason H -- Windmiller, Gur -- Koch, David G -- Borucki, William J -- England -- Nature. 2012 Jan 11;481(7382):475-9. doi: 10.1038/nature10768.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, California 92182, USA. wfw@sciences.sdsu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22237021" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment/chemistry ; *Planets ; Space Flight ; Spacecraft ; Stars, Celestial
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  • 7
    Publication Date: 2012-07-28
    Description: The Sun's equator and the planets' orbital planes are nearly aligned, which is presumably a consequence of their formation from a single spinning gaseous disk. For exoplanetary systems this well-aligned configuration is not guaranteed: dynamical interactions may tilt planetary orbits, or stars may be misaligned with the protoplanetary disk through chaotic accretion , magnetic interactions or torques from neighbouring stars. Indeed, isolated 'hot Jupiters' are often misaligned and even orbiting retrograde. Here we report an analysis of transits of planets over starspots on the Sun-like star Kepler-30 (ref. 8), and show that the orbits of its three planets are aligned with the stellar equator. Furthermore, the orbits are aligned with one another to within a few degrees. This configuration is similar to that of our Solar System, and contrasts with the isolated hot Jupiters. The orderly alignment seen in the Kepler-30 system suggests that high obliquities are confined to systems that experienced disruptive dynamical interactions. Should this be corroborated by observations of other coplanar multi-planet systems, then star-disk misalignments would be ruled out as the explanation for the high obliquities of hot Jupiters, and dynamical interactions would be implicated as the origin of hot Jupiters.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sanchis-Ojeda, Roberto -- Fabrycky, Daniel C -- Winn, Joshua N -- Barclay, Thomas -- Clarke, Bruce D -- Ford, Eric B -- Fortney, Jonathan J -- Geary, John C -- Holman, Matthew J -- Howard, Andrew W -- Jenkins, Jon M -- Koch, David -- Lissauer, Jack J -- Marcy, Geoffrey W -- Mullally, Fergal -- Ragozzine, Darin -- Seader, Shawn E -- Still, Martin -- Thompson, Susan E -- England -- Nature. 2012 Jul 25;487(7408):449-53. doi: 10.1038/nature11301.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139, USA. rsanchis86@gmail.com〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22836999" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
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  • 8
    Publication Date: 2011-02-05
    Description: When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets observed as multiples has implications for the planarity of planetary systems. But few stars have more than one known transiting planet, and none has more than three. Here we report Kepler spacecraft observations of a single Sun-like star, which we call Kepler-11, that reveal six transiting planets, five with orbital periods between 10 and 47 days and a sixth planet with a longer period. The five inner planets are among the smallest for which mass and size have both been measured, and these measurements imply substantial envelopes of light gases. The degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end of planet formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lissauer, Jack J -- Fabrycky, Daniel C -- Ford, Eric B -- Borucki, William J -- Fressin, Francois -- Marcy, Geoffrey W -- Orosz, Jerome A -- Rowe, Jason F -- Torres, Guillermo -- Welsh, William F -- Batalha, Natalie M -- Bryson, Stephen T -- Buchhave, Lars A -- Caldwell, Douglas A -- Carter, Joshua A -- Charbonneau, David -- Christiansen, Jessie L -- Cochran, William D -- Desert, Jean-Michel -- Dunham, Edward W -- Fanelli, Michael N -- Fortney, Jonathan J -- Gautier, Thomas N 3rd -- Geary, John C -- Gilliland, Ronald L -- Haas, Michael R -- Hall, Jennifer R -- Holman, Matthew J -- Koch, David G -- Latham, David W -- Lopez, Eric -- McCauliff, Sean -- Miller, Neil -- Morehead, Robert C -- Quintana, Elisa V -- Ragozzine, Darin -- Sasselov, Dimitar -- Short, Donald R -- Steffen, Jason H -- England -- Nature. 2011 Feb 3;470(7332):53-8. doi: 10.1038/nature09760.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, California 94035, USA. jack.lissauer@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21293371" target="_blank"〉PubMed〈/a〉
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  • 9
    Publication Date: 2012-06-23
    Description: In the solar system, the planets' compositions vary with orbital distance, with rocky planets in close orbits and lower-density gas giants in wider orbits. The detection of close-in giant planets around other stars was the first clue that this pattern is not universal and that planets' orbits can change substantially after their formation. Here, we report another violation of the orbit-composition pattern: two planets orbiting the same star with orbital distances differing by only 10% and densities differing by a factor of 8. One planet is likely a rocky "super-Earth," whereas the other is more akin to Neptune. These planets are 20 times more closely spaced and have a larger density contrast than any adjacent pair of planets in the solar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Carter, Joshua A -- Agol, Eric -- Chaplin, William J -- Basu, Sarbani -- Bedding, Timothy R -- Buchhave, Lars A -- Christensen-Dalsgaard, Jorgen -- Deck, Katherine M -- Elsworth, Yvonne -- Fabrycky, Daniel C -- Ford, Eric B -- Fortney, Jonathan J -- Hale, Steven J -- Handberg, Rasmus -- Hekker, Saskia -- Holman, Matthew J -- Huber, Daniel -- Karoff, Christopher -- Kawaler, Steven D -- Kjeldsen, Hans -- Lissauer, Jack J -- Lopez, Eric D -- Lund, Mikkel N -- Lundkvist, Mia -- Metcalfe, Travis S -- Miglio, Andrea -- Rogers, Leslie A -- Stello, Dennis -- Borucki, William J -- Bryson, Steve -- Christiansen, Jessie L -- Cochran, William D -- Geary, John C -- Gilliland, Ronald L -- Haas, Michael R -- Hall, Jennifer -- Howard, Andrew W -- Jenkins, Jon M -- Klaus, Todd -- Koch, David G -- Latham, David W -- MacQueen, Phillip J -- Sasselov, Dimitar -- Steffen, Jason H -- Twicken, Joseph D -- Winn, Joshua N -- New York, N.Y. -- Science. 2012 Aug 3;337(6094):556-9. doi: 10.1126/science.1223269. Epub 2012 Jun 21.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. jacarter@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22722249" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
    Publication Date: 2014-10-11
    Description: Exoplanets that orbit close to their host stars are much more highly irradiated than their solar system counterparts. Understanding the thermal structures and appearances of these planets requires investigating how their atmospheres respond to such extreme stellar forcing. We present spectroscopic thermal emission measurements as a function of orbital phase ("phase-curve observations") for the highly irradiated exoplanet WASP-43b spanning three full planet rotations using the Hubble Space Telescope. With these data, we construct a map of the planet's atmospheric thermal structure, from which we find large day-night temperature variations at all measured altitudes and a monotonically decreasing temperature with pressure at all longitudes. We also derive a Bond albedo of 0.18(-0.12)(+0.07) and an altitude dependence in the hot-spot offset relative to the substellar point.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stevenson, Kevin B -- Desert, Jean-Michel -- Line, Michael R -- Bean, Jacob L -- Fortney, Jonathan J -- Showman, Adam P -- Kataria, Tiffany -- Kreidberg, Laura -- McCullough, Peter R -- Henry, Gregory W -- Charbonneau, David -- Burrows, Adam -- Seager, Sara -- Madhusudhan, Nikku -- Williamson, Michael H -- Homeier, Derek -- New York, N.Y. -- Science. 2014 Nov 14;346(6211):838-41. doi: 10.1126/science.1256758. Epub 2014 Oct 9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA. NASA Sagan Fellow. kbs@uchicago.edu. ; CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, 389-UCB, Boulder, CO 80309, USA. ; Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA. ; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA. ; Department of Planetary Sciences and Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USA. ; Space Telescope Science Institute, Baltimore, MD 21218, USA. Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA. ; Center for Excellence in Information Systems, Tennessee State University, Nashville, TN 37209, USA. ; Department of Astronomy, Harvard University, Cambridge, MA 02138, USA. ; Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA. ; Department of Earth, Atmospheric, and Planetary Sciences, Department of Physics, Massachusetts Institute of Technology, 54-1718, 77 Massachusetts Avenue, Cambridge, MA 02139, USA. ; Institute of Astronomy, University of Cambridge, Cambridge CB3 OHA, UK. ; Centre de Recherche Astrophysique de Lyon, UMR 5574, CNRS, Universite de Lyon, Ecole Normale Superieure de Lyon, 46 Allee d'Italie, F-69364 Lyon Cedex 07, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25301972" target="_blank"〉PubMed〈/a〉
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