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  • 1
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    Kepler planet-detection mission: introduction and first results (2010)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2010-01-09
    Description: The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet's surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets (approximately 0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Borucki, William J -- Koch, David -- Basri, Gibor -- Batalha, Natalie -- Brown, Timothy -- Caldwell, Douglas -- Caldwell, John -- Christensen-Dalsgaard, Jorgen -- Cochran, William D -- DeVore, Edna -- Dunham, Edward W -- Dupree, Andrea K -- Gautier, Thomas N 3rd -- Geary, John C -- Gilliland, Ronald -- Gould, Alan -- Howell, Steve B -- Jenkins, Jon M -- Kondo, Yoji -- Latham, David W -- Marcy, Geoffrey W -- Meibom, Soren -- Kjeldsen, Hans -- Lissauer, Jack J -- Monet, David G -- Morrison, David -- Sasselov, Dimitar -- Tarter, Jill -- Boss, Alan -- Brownlee, Don -- Owen, Toby -- Buzasi, Derek -- Charbonneau, David -- Doyle, Laurance -- Fortney, Jonathan -- Ford, Eric B -- Holman, Matthew J -- Seager, Sara -- Steffen, Jason H -- Welsh, William F -- Rowe, Jason -- Anderson, Howard -- Buchhave, Lars -- Ciardi, David -- Walkowicz, Lucianne -- Sherry, William -- Horch, Elliott -- Isaacson, Howard -- Everett, Mark E -- Fischer, Debra -- Torres, Guillermo -- Johnson, John Asher -- Endl, Michael -- MacQueen, Phillip -- Bryson, Stephen T -- Dotson, Jessie -- Haas, Michael -- Kolodziejczak, Jeffrey -- Van Cleve, Jeffrey -- Chandrasekaran, Hema -- Twicken, Joseph D -- Quintana, Elisa V -- Clarke, Bruce D -- Allen, Christopher -- Li, Jie -- Wu, Haley -- Tenenbaum, Peter -- Verner, Ekaterina -- Bruhweiler, Frederick -- Barnes, Jason -- Prsa, Andrej -- New York, N.Y. -- Science. 2010 Feb 19;327(5968):977-80. doi: 10.1126/science.1185402. Epub 2010 Jan 7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, CA 94035, USA. William.J.Borucki@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20056856" target="_blank"〉PubMed〈/a〉
    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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  • 2
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    Kepler-16: a transiting circumbinary planet (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    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
    Electronic ISSN: 1095-9203
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  • 3
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    PTF 11kx: a type Ia supernova with a symbiotic nova progenitor (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-08-28
    Description: There is a consensus that type Ia supernovae (SNe Ia) arise from the thermonuclear explosion of white dwarf stars that accrete matter from a binary companion. However, direct observation of SN Ia progenitors is lacking, and the precise nature of the binary companion remains uncertain. A temporal series of high-resolution optical spectra of the SN Ia PTF 11kx reveals a complex circumstellar environment that provides an unprecedentedly detailed view of the progenitor system. Multiple shells of circumstellar material are detected, and the SN ejecta are seen to interact with circumstellar material starting 59 days after the explosion. These features are best described by a symbiotic nova progenitor, similar to RS Ophiuchi.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Dilday, B -- Howell, D A -- Cenko, S B -- Silverman, J M -- Nugent, P E -- Sullivan, M -- Ben-Ami, S -- Bildsten, L -- Bolte, M -- Endl, M -- Filippenko, A V -- Gnat, O -- Horesh, A -- Hsiao, E -- Kasliwal, M M -- Kirkman, D -- Maguire, K -- Marcy, G W -- Moore, K -- Pan, Y -- Parrent, J T -- Podsiadlowski, P -- Quimby, R M -- Sternberg, A -- Suzuki, N -- Tytler, D R -- Xu, D -- Bloom, J S -- Gal-Yam, A -- Hook, I M -- Kulkarni, S R -- Law, N M -- Ofek, E O -- Polishook, D -- Poznanski, D -- New York, N.Y. -- Science. 2012 Aug 24;337(6097):942-5. doi: 10.1126/science.1219164.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117, USA. bdilday@lcogt.net〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22923575" 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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  • 4
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    Kepler-47: a transiting circumbinary multiplanet system (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-08-31
    Description: We report the detection of Kepler-47, a system consisting of two planets orbiting around an eclipsing pair of stars. The inner and outer planets have radii 3.0 and 4.6 times that of Earth, respectively. The binary star consists of a Sun-like star and a companion roughly one-third its size, orbiting each other every 7.45 days. With an orbital period of 49.5 days, 18 transits of the inner planet have been observed, allowing a detailed characterization of its orbit and those of the stars. The outer planet's orbital period is 303.2 days, and although the planet is not Earth-like, it resides within the classical "habitable zone," where liquid water could exist on an Earth-like planet. With its two known planets, Kepler-47 establishes that close binary stars can host complete planetary systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Orosz, Jerome A -- Welsh, William F -- Carter, Joshua A -- Fabrycky, Daniel C -- Cochran, William D -- Endl, Michael -- Ford, Eric B -- Haghighipour, Nader -- MacQueen, Phillip J -- Mazeh, Tsevi -- Sanchis-Ojeda, Roberto -- Short, Donald R -- Torres, Guillermo -- Agol, Eric -- Buchhave, Lars A -- Doyle, Laurance R -- Isaacson, Howard -- Lissauer, Jack J -- Marcy, Geoffrey W -- Shporer, Avi -- Windmiller, Gur -- Barclay, Thomas -- Boss, Alan P -- Clarke, Bruce D -- Fortney, Jonathan -- Geary, John C -- Holman, Matthew J -- Huber, Daniel -- Jenkins, Jon M -- Kinemuchi, Karen -- Kruse, Ethan -- Ragozzine, Darin -- Sasselov, Dimitar -- Still, Martin -- Tenenbaum, Peter -- Uddin, Kamal -- Winn, Joshua N -- Koch, David G -- Borucki, William J -- New York, N.Y. -- Science. 2012 Sep 21;337(6101):1511-4. Epub 2012 Aug 28.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, CA 92182, USA. orosz@sciences.sdsu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22933522" target="_blank"〉PubMed〈/a〉
    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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  • 5
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    Stellar spin-orbit misalignment in a multiplanet system (2013)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2013-10-19
    Description: Stars hosting hot Jupiters are often observed to have high obliquities, whereas stars with multiple coplanar planets have been seen to have low obliquities. This has been interpreted as evidence that hot-Jupiter formation is linked to dynamical disruption, as opposed to planet migration through a protoplanetary disk. We used asteroseismology to measure a large obliquity for Kepler-56, a red giant star hosting two transiting coplanar planets. These observations show that spin-orbit misalignments are not confined to hot-Jupiter systems. Misalignments in a broader class of systems had been predicted as a consequence of torques from wide-orbiting companions, and indeed radial velocity measurements revealed a third companion in a wide orbit in the Kepler-56 system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Huber, Daniel -- Carter, Joshua A -- Barbieri, Mauro -- Miglio, Andrea -- Deck, Katherine M -- Fabrycky, Daniel C -- Montet, Benjamin T -- Buchhave, Lars A -- Chaplin, William J -- Hekker, Saskia -- Montalban, Josefina -- Sanchis-Ojeda, Roberto -- Basu, Sarbani -- Bedding, Timothy R -- Campante, Tiago L -- Christensen-Dalsgaard, Jorgen -- Elsworth, Yvonne P -- Stello, Dennis -- Arentoft, Torben -- Ford, Eric B -- Gilliland, Ronald L -- Handberg, Rasmus -- Howard, Andrew W -- Isaacson, Howard -- Johnson, John Asher -- Karoff, Christoffer -- Kawaler, Steven D -- Kjeldsen, Hans -- Latham, David W -- Lund, Mikkel N -- Lundkvist, Mia -- Marcy, Geoffrey W -- Metcalfe, Travis S -- Silva Aguirre, Victor -- Winn, Joshua N -- New York, N.Y. -- Science. 2013 Oct 18;342(6156):331-4. doi: 10.1126/science.1242066.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24136961" target="_blank"〉PubMed〈/a〉
    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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  • 6
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    Kepler-62: a five-planet system with planets of 1.4 and 1.6 Earth radii in the habitable zone (2013)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2013-04-20
    Description: We present the detection of five planets--Kepler-62b, c, d, e, and f--of size 1.31, 0.54, 1.95, 1.61 and 1.41 Earth radii (R plus sign in circle), orbiting a K2V star at periods of 5.7, 12.4, 18.2, 122.4, and 267.3 days, respectively. The outermost planets, Kepler-62e and -62f, are super-Earth-size (1.25 R plus sign in circle 〈 planet radius 〈/= 2.0 R plus sign in circle) planets in the habitable zone of their host star, respectively receiving 1.2 +/- 0.2 times and 0.41 +/- 0.05 times the solar flux at Earth's orbit. Theoretical models of Kepler-62e and -62f for a stellar age of ~7 billion years suggest that both planets could be solid, either with a rocky composition or composed of mostly solid water in their bulk.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Borucki, William J -- Agol, Eric -- Fressin, Francois -- Kaltenegger, Lisa -- Rowe, Jason -- Isaacson, Howard -- Fischer, Debra -- Batalha, Natalie -- Lissauer, Jack J -- Marcy, Geoffrey W -- Fabrycky, Daniel -- Desert, Jean-Michel -- Bryson, Stephen T -- Barclay, Thomas -- Bastien, Fabienne -- Boss, Alan -- Brugamyer, Erik -- Buchhave, Lars A -- Burke, Chris -- Caldwell, Douglas A -- Carter, Josh -- Charbonneau, David -- Crepp, Justin R -- Christensen-Dalsgaard, Jorgen -- Christiansen, Jessie L -- Ciardi, David -- Cochran, William D -- DeVore, Edna -- Doyle, Laurance -- Dupree, Andrea K -- Endl, Michael -- Everett, Mark E -- Ford, Eric B -- Fortney, Jonathan -- Gautier, Thomas N 3rd -- Geary, John C -- Gould, Alan -- Haas, Michael -- Henze, Christopher -- Howard, Andrew W -- Howell, Steve B -- Huber, Daniel -- Jenkins, Jon M -- Kjeldsen, Hans -- Kolbl, Rea -- Kolodziejczak, Jeffery -- Latham, David W -- Lee, Brian L -- Lopez, Eric -- Mullally, Fergal -- Orosz, Jerome A -- Prsa, Andrej -- Quintana, Elisa V -- Sanchis-Ojeda, Roberto -- Sasselov, Dimitar -- Seader, Shawn -- Shporer, Avi -- Steffen, Jason H -- Still, Martin -- Tenenbaum, Peter -- Thompson, Susan E -- Torres, Guillermo -- Twicken, Joseph D -- Welsh, William F -- Winn, Joshua N -- New York, N.Y. -- Science. 2013 May 3;340(6132):587-90. doi: 10.1126/science.1234702. Epub 2013 Apr 18.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, CA 94035, USA. william.j.borucki@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23599262" target="_blank"〉PubMed〈/a〉
    Keywords: Exobiology ; Extraterrestrial Environment ; Models, Theoretical ; *Planets ; Stars, Celestial ; *Water
    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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  • 7
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    Supernova SN 2011fe from an exploding carbon-oxygen white dwarf star (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-12-16
    Description: Type Ia supernovae have been used empirically as 'standard candles' to demonstrate the acceleration of the expansion of the Universe even though fundamental details, such as the nature of their progenitor systems and how the stars explode, remain a mystery. There is consensus that a white dwarf star explodes after accreting matter in a binary system, but the secondary body could be anything from a main-sequence star to a red giant, or even another white dwarf. This uncertainty stems from the fact that no recent type Ia supernova has been discovered close enough to Earth to detect the stars before explosion. Here we report early observations of supernova SN 2011fe in the galaxy M101 at a distance from Earth of 6.4 megaparsecs. We find that the exploding star was probably a carbon-oxygen white dwarf, and from the lack of an early shock we conclude that the companion was probably a main-sequence star. Early spectroscopy shows high-velocity oxygen that slows rapidly, on a timescale of hours, and extensive mixing of newly synthesized intermediate-mass elements in the outermost layers of the supernova. A companion paper uses pre-explosion images to rule out luminous red giants and most helium stars as companions to the progenitor.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nugent, Peter E -- Sullivan, Mark -- Cenko, S Bradley -- Thomas, Rollin C -- Kasen, Daniel -- Howell, D Andrew -- Bersier, David -- Bloom, Joshua S -- Kulkarni, S R -- Kandrashoff, Michael T -- Filippenko, Alexei V -- Silverman, Jeffrey M -- Marcy, Geoffrey W -- Howard, Andrew W -- Isaacson, Howard T -- Maguire, Kate -- Suzuki, Nao -- Tarlton, James E -- Pan, Yen-Chen -- Bildsten, Lars -- Fulton, Benjamin J -- Parrent, Jerod T -- Sand, David -- Podsiadlowski, Philipp -- Bianco, Federica B -- Dilday, Benjamin -- Graham, Melissa L -- Lyman, Joe -- James, Phil -- Kasliwal, Mansi M -- Law, Nicholas M -- Quimby, Robert M -- Hook, Isobel M -- Walker, Emma S -- Mazzali, Paolo -- Pian, Elena -- Ofek, Eran O -- Gal-Yam, Avishay -- Poznanski, Dovi -- England -- Nature. 2011 Dec 14;480(7377):344-7. doi: 10.1038/nature10644.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA. penugent@lbl.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22170680" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 8
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    Two Earth-sized planets orbiting Kepler-20 (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-12-22
    Description: Since the discovery of the first extrasolar giant planets around Sun-like stars, evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered has a radius 1.42 times that of the Earth's radius (R( plus sign in circle)), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03R( plus sign in circle)) and the other smaller than the Earth (0.87R( plus sign in circle)), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets. The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fressin, Francois -- Torres, Guillermo -- Rowe, Jason F -- Charbonneau, David -- Rogers, Leslie A -- Ballard, Sarah -- Batalha, Natalie M -- Borucki, William J -- Bryson, Stephen T -- Buchhave, Lars A -- Ciardi, David R -- Desert, Jean-Michel -- Dressing, Courtney D -- Fabrycky, Daniel C -- Ford, Eric B -- Gautier, Thomas N 3rd -- Henze, Christopher E -- Holman, Matthew J -- Howard, Andrew -- Howell, Steve B -- Jenkins, Jon M -- Koch, David G -- Latham, David W -- Lissauer, Jack J -- Marcy, Geoffrey W -- Quinn, Samuel N -- Ragozzine, Darin -- Sasselov, Dimitar D -- Seager, Sara -- Barclay, Thomas -- Mullally, Fergal -- Seader, Shawn E -- Still, Martin -- Twicken, Joseph D -- Thompson, Susan E -- Uddin, Kamal -- England -- Nature. 2011 Dec 20;482(7384):195-8. doi: 10.1038/nature10780.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA. ffressin@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22186831" 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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  • 9
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    An abundance of small exoplanets around stars with a wide range of metallicities (2012)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2012-06-23
    Description: The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a 'fossil' record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets, supporting the model that planets form by accumulation of dust and ice particles. Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets. However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission, including objects that are comparable in size to the terrestrial planets in the Solar System. We find that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. This observation suggests that terrestrial planets may be widespread in the disk of the Galaxy, with no special requirement of enhanced metallicity for their formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Buchhave, Lars A -- Latham, David W -- Johansen, Anders -- Bizzarro, Martin -- Torres, Guillermo -- Rowe, Jason F -- Batalha, Natalie M -- Borucki, William J -- Brugamyer, Erik -- Caldwell, Caroline -- Bryson, Stephen T -- Ciardi, David R -- Cochran, William D -- Endl, Michael -- Esquerdo, Gilbert A -- Ford, Eric B -- Geary, John C -- Gilliland, Ronald L -- Hansen, Terese -- Isaacson, Howard -- Laird, John B -- Lucas, Philip W -- Marcy, Geoffrey W -- Morse, Jon A -- Robertson, Paul -- Shporer, Avi -- Stefanik, Robert P -- Still, Martin -- Quinn, Samuel N -- England -- Nature. 2012 Jun 13;486(7403):375-7. doi: 10.1038/nature11121.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark. buchhave@astro.ku.dk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22722196" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
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  • 10
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    A rocky composition for an Earth-sized exoplanet (2013)
    Nature Publishing Group (NPG)
    Details
    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
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    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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