Two Earth-sized planets orbiting Kepler-20
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Author
Fressin, Francois
Rowe, Jason F.
Rogers, Leslie A.
Ballard, Sarah
Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Buchhave, Lars A.
Ciardi, David R.
Désert, Jean-Michel
Dressing, Courtney D.
Fabrycky, Daniel C.
Ford, Eric B.
Gautier III, Thomas N.
Henze, Christopher E.
Howard, Andrew
Howell, Steve B.
Jenkins, Jon M.
Koch, David G.
Lissauer, Jack J.
Marcy, Geoffrey W.
Quinn, Samuel N.
Ragozzine, Darin
Seager, Sara
Barclay, Thomas
Mullally, Fergal
Seader, Shawn E.
Still, Martin
Twicken, Joseph D.
Thompson, Susan E.
Uddin, Kamal
Note: Order does not necessarily reflect citation order of authors.
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https://doi.org/10.1038/nature10780Metadata
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Fressin, Francois, Guillermo Torres, Jason F. Rowe, David Charbonneau, Leslie A. Rogers, Sarah Ballard, Natalie M. Batalha, et al. 2011. Two Earth-Sized Planets Orbiting Kepler-20. Nature 482, no. 7384: 195–198. doi:10.1038/nature10780. http://dx.doi.org/10.1038/nature10780.Abstract
Since the discovery of the first extrasolar giant planets around Sun-like stars1,2, 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 discovered3 has a radius 1.42 times that of the Earth’s radius (R⊕), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03R⊕) and the other smaller than the Earth (0.87R⊕), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets4 . 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.Other Sources
https://arxiv.org/abs/1112.4550Terms of Use
This article is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#OAPCitable link to this page
http://nrs.harvard.edu/urn-3:HUL.InstRepos:29990191
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