| Literature DB >> 23599262 |
William J Borucki1, Eric Agol, Francois Fressin, Lisa Kaltenegger, Jason Rowe, Howard Isaacson, Debra Fischer, Natalie Batalha, Jack J Lissauer, Geoffrey W Marcy, Daniel Fabrycky, Jean-Michel Désert, Stephen T Bryson, Thomas Barclay, Fabienne Bastien, Alan Boss, Erik Brugamyer, Lars A Buchhave, Chris Burke, Douglas A Caldwell, Josh Carter, David Charbonneau, Justin R Crepp, Jørgen Christensen-Dalsgaard, Jessie L Christiansen, David Ciardi, William D Cochran, Edna DeVore, Laurance Doyle, Andrea K Dupree, Michael Endl, Mark E Everett, Eric B Ford, Jonathan Fortney, Thomas N Gautier, John C Geary, Alan Gould, Michael Haas, Christopher Henze, Andrew W Howard, Steve B Howell, Daniel Huber, Jon M Jenkins, Hans Kjeldsen, Rea Kolbl, Jeffery Kolodziejczak, David W Latham, Brian L Lee, Eric Lopez, Fergal Mullally, Jerome A Orosz, Andrej Prsa, Elisa V Quintana, Roberto Sanchis-Ojeda, Dimitar Sasselov, Shawn Seader, Avi Shporer, Jason H Steffen, Martin Still, Peter Tenenbaum, Susan E Thompson, Guillermo Torres, Joseph D Twicken, William F Welsh, Joshua N Winn.
Abstract
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⊕), 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⊕ < planet radius ≤ 2.0 R⊕) 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.Entities:
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Year: 2013 PMID： 23599262 DOI： 10.1126/science.1234702
Source DB: PubMed Journal: Science ISSN： 0036-8075 Impact factor: 47.728