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  • 1
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    The mass of the Mars-sized exoplanet Kepler-138 b from transit timing (2015)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2015-06-19
    Description: Extrasolar planets that pass in front of their host star (transit) cause a temporary decrease in the apparent brightness of the star, providing a direct measure of the planet's size and orbital period. In some systems with multiple transiting planets, the times of the transits are measurably affected by the gravitational interactions between neighbouring planets. In favourable cases, the departures from Keplerian orbits (that is, unaffected by gravitational effects) implied by the observed transit times permit the planetary masses to be measured, which is key to determining their bulk densities. Characterizing rocky planets is particularly difficult, because they are generally smaller and less massive than gaseous planets. Therefore, few exoplanets near the size of Earth have had their masses measured. Here we report the sizes and masses of three planets orbiting Kepler-138, a star much fainter and cooler than the Sun. We determine that the mass of the Mars-sized inner planet, Kepler-138 b, is 0.066(+0.059)(-0.037) Earth masses. Its density is 2.6(+2.4)(-1.5) grams per cubic centimetre. The middle and outer planets are both slightly larger than Earth. The middle planet's density (6.2(+5.8)(-3.4) grams per cubic centimetre) is similar to that of Earth, and the outer planet is less than half as dense at 2.1(+2.2)(-1.2) grams per cubic centimetre, implying that it contains a greater portion of low-density components such as water and hydrogen.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jontof-Hutter, Daniel -- Rowe, Jason F -- Lissauer, Jack J -- Fabrycky, Daniel C -- Ford, Eric B -- England -- Nature. 2015 Jun 18;522(7556):321-3. doi: 10.1038/nature14494.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉1] Department of Astronomy, Pennsylvania State University, Davey Laboratory, University Park, Pennsylvania 16802, USA [2] NASA Ames Research Center, Moffett Field, California 94035, USA. ; 1] NASA Ames Research Center, Moffett Field, California 94035, USA [2] SETI Institute, 189 North Bernardo Avenue, Mountain View, California 94043, USA. ; NASA Ames Research Center, Moffett Field, California 94035, USA. ; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA. ; Department of Astronomy, Pennsylvania State University, Davey Laboratory, University Park, Pennsylvania 16802, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26085271" 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
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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
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 3
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    Kepler-47: a transiting circumbinary multiplanet system (2012)
    American Association for the Advancement of Science (AAAS)
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    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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  • 4
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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
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  • 5
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    Two Earth-sized planets orbiting Kepler-20 (2011)
    Nature Publishing Group (NPG)
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    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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  • 6
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    Transiting circumbinary planets Kepler-34 b and Kepler-35 b (2012)
    Nature Publishing Group (NPG)
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    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
    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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    Alignment of the stellar spin with the orbits of a three-planet system (2012)
    Nature Publishing Group (NPG)
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    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
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    A closely packed system of low-mass, low-density planets transiting Kepler-11 (2011)
    Nature Publishing Group (NPG)
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    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
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  • 9
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    Kepler-9: a system of multiple planets transiting a Sun-like star, confirmed by timing variations (2010)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2010-08-28
    Description: The Kepler spacecraft is monitoring more than 150,000 stars for evidence of planets transiting those stars. We report the detection of two Saturn-size planets that transit the same Sun-like star, based on 7 months of Kepler observations. Their 19.2- and 38.9-day periods are presently increasing and decreasing at respective average rates of 4 and 39 minutes per orbit; in addition, the transit times of the inner body display an alternating variation of smaller amplitude. These signatures are characteristic of gravitational interaction of two planets near a 2:1 orbital resonance. Six radial-velocity observations show that these two planets are the most massive objects orbiting close to the star and substantially improve the estimates of their masses. After removing the signal of the two confirmed giant planets, we identified an additional transiting super-Earth-size planet candidate with a period of 1.6 days.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Holman, Matthew J -- Fabrycky, Daniel C -- Ragozzine, Darin -- Ford, Eric B -- Steffen, Jason H -- Welsh, William F -- Lissauer, Jack J -- Latham, David W -- Marcy, Geoffrey W -- Walkowicz, Lucianne M -- Batalha, Natalie M -- Jenkins, Jon M -- Rowe, Jason F -- Cochran, William D -- Fressin, Francois -- Torres, Guillermo -- Buchhave, Lars A -- Sasselov, Dimitar D -- Borucki, William J -- Koch, David G -- Basri, Gibor -- Brown, Timothy M -- Caldwell, Douglas A -- Charbonneau, David -- Dunham, Edward W -- Gautier, Thomas N 3rd -- Geary, John C -- Gilliland, Ronald L -- Haas, Michael R -- Howell, Steve B -- Ciardi, David R -- Endl, Michael -- Fischer, Debra -- Furesz, Gabor -- Hartman, Joel D -- Isaacson, Howard -- Johnson, John A -- MacQueen, Phillip J -- Moorhead, Althea V -- Morehead, Robert C -- Orosz, Jerome A -- New York, N.Y. -- Science. 2010 Oct 1;330(6000):51-4. doi: 10.1126/science.1195778. Epub 2010 Aug 26.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. mholman@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20798283" target="_blank"〉PubMed〈/a〉
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  • 10
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    KOI-126: a triply eclipsing hierarchical triple with two low-mass stars (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-01-13
    Description: The Kepler spacecraft has been monitoring the light from 150,000 stars in its primary quest to detect transiting exoplanets. Here, we report on the detection of an eclipsing stellar hierarchical triple, identified in the Kepler photometry. KOI-126 [A, (B, C)], is composed of a low-mass binary [masses M(B) = 0.2413 +/- 0.0030 solar mass (M(middle dot in circle)), M(C) = 0.2127 +/- 0.0026 M(middle dot in circle); radii R(B) = 0.2543 +/- 0.0014 solar radius (R(middle dot in circle)), R(C) = 0.2318 +/- 0.0013 R(middle dot in circle); orbital period P(1) = 1.76713 +/- 0.00019 days] on an eccentric orbit about a third star (mass M(A) = 1.347 +/- 0.032 M(middle dot in circle); radius R(A) = 2.0254 +/- 0.0098 R(middle dot in circle); period of orbit around the low-mass binary P(2) = 33.9214 +/- 0.0013 days; eccentricity of that orbit e(2) = 0.3043 +/- 0.0024). The low-mass pair probe the poorly sampled fully convective stellar domain offering a crucial benchmark for theoretical stellar models.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Carter, Joshua A -- Fabrycky, Daniel C -- Ragozzine, Darin -- Holman, Matthew J -- Quinn, Samuel N -- Latham, David W -- Buchhave, Lars A -- Van Cleve, Jeffrey -- Cochran, William D -- Cote, Miles T -- Endl, Michael -- Ford, Eric B -- Haas, Michael R -- Jenkins, Jon M -- Koch, David G -- Li, Jie -- Lissauer, Jack J -- MacQueen, Phillip J -- Middour, Christopher K -- Orosz, Jerome A -- Rowe, Jason F -- Steffen, Jason H -- Welsh, William F -- New York, N.Y. -- Science. 2011 Feb 4;331(6017):562-5. doi: 10.1126/science.1201274. Epub 2011 Jan 11.〈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/21224439" target="_blank"〉PubMed〈/a〉
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