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  • 1
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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Astronomy. Taking the pulse of a massive star (2003)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2003-06-21
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kawaler, Steven D -- New York, N.Y. -- Science. 2003 Jun 20;300(5627):1885-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA. sdk@iastate.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12817130" 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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    Hot super-Earths stripped by their host stars (2016)
    Springer Nature
    Details
    Publication Date: 2016-04-13
    Description: Article Theory predicts a deficit of super-Earth sized planets, which orbit close to their host star. Here, Lundkvist et al . use data from the NASA Kepler mission to show that this deficit is also seen in observations, thereby providing new insight into exoplanetary systems. Nature Communications doi: 10.1038/ncomms11201 Authors: M. S. Lundkvist, H. Kjeldsen, S. Albrecht, G. R. Davies, S. Basu, D. Huber, A. B. Justesen, C. Karoff, V. Silva Aguirre, V. Van Eylen, C. Vang, T. Arentoft, T. Barclay, T. R. Bedding, T. L. Campante, W. J. Chaplin, J. Christensen-Dalsgaard, Y. P. Elsworth, R. L. Gilliland, R. Handberg, S. Hekker, S. D. Kawaler, M. N. Lund, T. S. Metcalfe, A. Miglio, J. F. Rowe, D. Stello, B. Tingley, T. R. White
    Electronic ISSN: 2041-1723
    Topics: Biology , Chemistry and Pharmacology , Natural Sciences in General , Physics
    Published by Springer Nature
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  • 4
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    A sub-Mercury-sized exoplanet (2013)
    Nature Publishing Group (NPG)
    Details
    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
    Published by Nature Publishing Group (NPG)
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  • 5
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    A compact system of small planets around a former red-giant star (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-12-24
    Description: Planets that orbit their parent star at less than about one astronomical unit (1 AU is the Earth-Sun distance) are expected to be engulfed when the star becomes a red giant. Previous observations have revealed the existence of post-red-giant host stars with giant planets orbiting as close as 0.116 AU or with brown dwarf companions in tight orbits, showing that these bodies can survive engulfment. What has remained unclear is whether planets can be dragged deeper into the red-giant envelope without being disrupted and whether the evolution of the parent star itself could be affected. Here we report the presence of two nearly Earth-sized bodies orbiting the post-red-giant, hot B subdwarf star KIC 05807616 at distances of 0.0060 and 0.0076 AU, with orbital periods of 5.7625 and 8.2293 hours, respectively. These bodies probably survived deep immersion in the former red-giant envelope. They may be the dense cores of evaporated giant planets that were transported closer to the star during the engulfment and triggered the mass loss necessary for the formation of the hot B subdwarf, which might also explain how some stars of this type did not form in binary systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Charpinet, S -- Fontaine, G -- Brassard, P -- Green, E M -- Van Grootel, V -- Randall, S K -- Silvotti, R -- Baran, A S -- Ostensen, R H -- Kawaler, S D -- Telting, J H -- England -- Nature. 2011 Dec 21;480(7378):496-9. doi: 10.1038/nature10631.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Universite de Toulouse, UPS-OMP, IRAP, F-31400 Toulouse, France. stephane.charpinet@ast.obs-mip.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22193103" 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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    Ensemble asteroseismology of solar-type stars with the NASA Kepler mission (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-04-09
    Description: In addition to its search for extrasolar planets, the NASA Kepler mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solar-type stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius, and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Chaplin, W J -- Kjeldsen, H -- Christensen-Dalsgaard, J -- Basu, S -- Miglio, A -- Appourchaux, T -- Bedding, T R -- Elsworth, Y -- Garcia, R A -- Gilliland, R L -- Girardi, L -- Houdek, G -- Karoff, C -- Kawaler, S D -- Metcalfe, T S -- Molenda-Zakowicz, J -- Monteiro, M J P F G -- Thompson, M J -- Verner, G A -- Ballot, J -- Bonanno, A -- Brandao, I M -- Broomhall, A-M -- Bruntt, H -- Campante, T L -- Corsaro, E -- Creevey, O L -- Dogan, G -- Esch, L -- Gai, N -- Gaulme, P -- Hale, S J -- Handberg, R -- Hekker, S -- Huber, D -- Jimenez, A -- Mathur, S -- Mazumdar, A -- Mosser, B -- New, R -- Pinsonneault, M H -- Pricopi, D -- Quirion, P-O -- Regulo, C -- Salabert, D -- Serenelli, A M -- Silva Aguirre, V -- Sousa, S G -- Stello, D -- Stevens, I R -- Suran, M D -- Uytterhoeven, K -- White, T R -- Borucki, W J -- Brown, T M -- Jenkins, J M -- Kinemuchi, K -- Van Cleve, J -- Klaus, T C -- New York, N.Y. -- Science. 2011 Apr 8;332(6026):213-6. doi: 10.1126/science.1201827.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK. w.j.chaplin@bham.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21474754" 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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  • 7
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    Kepler detected gravity-mode period spacings in a red giant star (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-03-19
    Description: Stellar interiors are inaccessible through direct observations. For this reason, helioseismologists made use of the Sun's acoustic oscillation modes to tune models of its structure. The quest to detect modes that probe the solar core has been ongoing for decades. We report the detection of mixed modes penetrating all the way to the core of an evolved star from 320 days of observations with the Kepler satellite. The period spacings of these mixed modes are directly dependent on the density gradient between the core region and the convective envelope.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Beck, P G -- Bedding, T R -- Mosser, B -- Stello, D -- Garcia, R A -- Kallinger, T -- Hekker, S -- Elsworth, Y -- Frandsen, S -- Carrier, F -- De Ridder, J -- Aerts, C -- White, T R -- Huber, D -- Dupret, M-A -- Montalban, J -- Miglio, A -- Noels, A -- Chaplin, W J -- Kjeldsen, H -- Christensen-Dalsgaard, J -- Gilliland, R L -- Brown, T M -- Kawaler, S D -- Mathur, S -- Jenkins, J M -- New York, N.Y. -- Science. 2011 Apr 8;332(6026):205. doi: 10.1126/science.1201939. Epub 2011 Mar 17.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, 3001 Leuven, Belgium. paul.beck@ster.kuleuven.be〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21415318" 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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  • 8
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    Kepler-36: a pair of planets with neighboring orbits and dissimilar densities (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    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〉
    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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  • 9
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    Insights into internal effects of common-envelope evolution using the extended Kepler mission (2015)
    Oxford University Press
    Details
    Publication Date: 2015-06-10
    Description: We present an analysis of the binary and physical parameters of a unique pulsating white dwarf with a main-sequence companion, SDSS J1136+0409, observed for more than 77 d during the first pointing of the extended Kepler mission: K2 Campaign 1. Using new ground-based spectroscopy, we show that this post-common-envelope binary has an orbital period of 6.89760103(60) h, which is also seen in the photometry as a result of Doppler beaming and ellipsoidal variations of the secondary. We spectroscopically refine the temperature of the white dwarf to 12 330 ± 260 K and its mass to 0.601 ± 0.036 M . We detect seven independent pulsation modes in the K2 light curve. A preliminary asteroseismic solution is in reasonable agreement with the spectroscopic atmospheric parameters. Three of the pulsation modes are clearly rotationally split multiplets, which we use to demonstrate that the white dwarf is not synchronously rotating with the orbital period but has a rotation period of 2.49 ± 0.53 h. This is faster than any known isolated white dwarf, but slower than almost all white dwarfs measured in non-magnetic cataclysmic variables, the likely future state of this binary.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    Observations of the Pulsating White Dwarf G 185–32 (2003)
    EDP Sciences
    Details
    Publication Date: 2003-12-18
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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