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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    HD 181068: a red giant in a triply eclipsing compact hierarchical triple system (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-04-09
    Description: Hierarchical triple systems comprise a close binary and a more distant component. They are important for testing theories of star formation and of stellar evolution in the presence of nearby companions. We obtained 218 days of Kepler photometry of HD 181068 (magnitude of 7.1), supplemented by ground-based spectroscopy and interferometry, which show it to be a hierarchical triple with two types of mutual eclipses. The primary is a red giant that is in a 45-day orbit with a pair of red dwarfs in a close 0.9-day orbit. The red giant shows evidence for tidally induced oscillations that are driven by the orbital motion of the close pair. HD 181068 is an ideal target for studies of dynamical evolution and testing tidal friction theories in hierarchical triple systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Derekas, A -- Kiss, L L -- Borkovits, T -- Huber, D -- Lehmann, H -- Southworth, J -- Bedding, T R -- Balam, D -- Hartmann, M -- Hrudkova, M -- Ireland, M J -- Kovacs, J -- Mezo, Gy -- Moor, A -- Niemczura, E -- Sarty, G E -- Szabo, Gy M -- Szabo, R -- Telting, J H -- Tkachenko, A -- Uytterhoeven, K -- Benko, J M -- Bryson, S T -- Maestro, V -- Simon, A E -- Stello, D -- Schaefer, G -- Aerts, C -- ten Brummelaar, T A -- De Cat, P -- McAlister, H A -- Maceroni, C -- Merand, A -- Still, M -- Sturmann, J -- Sturmann, L -- Turner, N -- Tuthill, P G -- Christensen-Dalsgaard, J -- Gilliland, R L -- Kjeldsen, H -- Quintana, E V -- Tenenbaum, P -- Twicken, J D -- New York, N.Y. -- Science. 2011 Apr 8;332(6026):216-8. doi: 10.1126/science.1201762.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Eotvos University, Budapest, Hungary. derekas@konkoly.hu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21474755" 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
    Published by American Association for the Advancement of Science (AAAS)
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  • 3
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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 4
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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
    Published by Nature Publishing Group (NPG)
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  • 5
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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
    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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  • 6
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    A sub-Mercury-sized exoplanet (2013)
    Nature Publishing Group (NPG)
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    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〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 7
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    A closely packed system of low-mass, low-density planets transiting Kepler-11 (2011)
    Nature Publishing Group (NPG)
    Details
    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〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 8
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    The same frequency of planets inside and outside open clusters of stars (2013)
    Nature Publishing Group (NPG)
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    Publication Date: 2013-06-28
    Description: Most stars and their planets form in open clusters. Over 95 per cent of such clusters have stellar densities too low (less than a hundred stars per cubic parsec) to withstand internal and external dynamical stresses and fall apart within a few hundred million years. Older open clusters have survived by virtue of being richer and denser in stars (1,000 to 10,000 per cubic parsec) when they formed. Such clusters represent a stellar environment very different from the birthplace of the Sun and other planet-hosting field stars. So far more than 800 planets have been found around Sun-like stars in the field. The field planets are usually the size of Neptune or smaller. In contrast, only four planets have been found orbiting stars in open clusters, all with masses similar to or greater than that of Jupiter. Here we report observations of the transits of two Sun-like stars by planets smaller than Neptune in the billion-year-old open cluster NGC6811. This demonstrates that small planets can form and survive in a dense cluster environment, and implies that the frequency and properties of planets in open clusters are consistent with those of planets around field stars in the Galaxy.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Meibom, Soren -- Torres, Guillermo -- Fressin, Francois -- Latham, David W -- Rowe, Jason F -- Ciardi, David R -- Bryson, Steven T -- Rogers, Leslie A -- Henze, Christopher E -- Janes, Kenneth -- Barnes, Sydney A -- Marcy, Geoffrey W -- Isaacson, Howard -- Fischer, Debra A -- Howell, Steve B -- Horch, Elliott P -- Jenkins, Jon M -- Schuler, Simon C -- Crepp, Justin -- England -- Nature. 2013 Jul 4;499(7456):55-8. doi: 10.1038/nature12279. Epub 2013 Jun 26.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA. smeibom@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23803764" 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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    PREDICTING THE DETECTABILITY OF OSCILLATIONS IN SOLAR-TYPE STARS OBSERVED BYKEPLER (2011)
    Institute of Physics
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    Publication Date: 2011-04-14
    Print ISSN: 0004-637X
    Electronic ISSN: 1538-4357
    Topics: Physics
    Published by Institute of Physics
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  • 10
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    DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FORθCYG, THE BRIGHTEST STAR OBSERVED BY THEKEPLERMISSION (2016)
    Institute of Physics
    Details
    Publication Date: 2016-10-21
    Print ISSN: 0004-637X
    Electronic ISSN: 1538-4357
    Topics: Physics
    Published by Institute of Physics
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