Kepler-68: Three Planets, One With a Density Between That of Earth and Ice Giants
View/ Open
Author
Gilliland, Ronald L.
Marcy, Geoffrey W.
Rowe, Jason F.
Rogers, Leslie
Fressin, Francois
Lopez, Eric D.
Buchhave, Lars A.
Christensen-Dalsgaard, Jørgen
Désert, Jean-Michel
Henze, Christopher E.
Isaacson, Howard
Jenkins, Jon M.
Lissauer, Jack J.
Chaplin, William J.
Basu, Sarbani
Metcalfe, Travis S.
Elsworth, Yvonne
Handberg, Rasmus
Hekker, Saskia
Huber, Daniel
Karoff, Christoffer
Kjeldsen, Hans
Lund, Mikkel N.
Lundkvist, Mia
Miglio, Andrea
Ford, Eric B.
Fortney, Jonathan J.
Haas, Michael R.
Howard, Andrew W.
Howell, Steve B.
Ragozzine, Darin
Thompson, Susan E.
Note: Order does not necessarily reflect citation order of authors.
Published Version
https://doi.org/10.1088/0004-637X/766/1/40Metadata
Show full item recordCitation
Gilliland, Ronald L., Geoffrey W. Marcy, Jason F. Rowe, Leslie Rogers, Guillermo Torres, Francois Fressin, Eric D. Lopez, et al. 2013. Kepler-68: Three Planets, One With a Density Between That of Earth and Ice Giants. The Astrophysical Journal 766, no. 1: 40. doi:10.1088/0004-637x/766/1/40.Abstract
NASA's Kepler Mission has revealed two transiting planets orbiting Kepler-68. Follow-up Doppler measurements have established the mass of the innermost planet and revealed a third Jovian-mass planet orbiting beyond the two transiting planets. Kepler-68b, in a 5.4 day orbit, has $M_{\rm P}=8.3^{+2.2}_{-2.4}$ M ⊕, $R_{\rm P}=2.31^{+0.06}_{-0.09}$ R ⊕, and $\rho _{\rm P}=3.32^{+0.86}_{-0.98}$ g cm–3, giving Kepler-68b a density intermediate between that of the ice giants and Earth. Kepler-68c is Earth-sized, with a radius $R_{\rm P}=0.953^{+0.037}_{-0.042}$ R ⊕ and transits on a 9.6 day orbit; validation of Kepler-68c posed unique challenges. Kepler-68d has an orbital period of 580 ± 15 days and a minimum mass of M Psin i = 0.947 ± 0.035MJ . Power spectra of the Kepler photometry at one minute cadence exhibit a rich and strong set of asteroseismic pulsation modes enabling detailed analysis of the stellar interior. Spectroscopy of the star coupled with asteroseismic modeling of the multiple pulsation modes yield precise measurements of stellar properties, notably T eff = 5793 ± 74 K, M sstarf = 1.079 ± 0.051 M ☉, R sstarf = 1.243 ± 0.019 R ☉, and ρsstarf = 0.7903 ± 0.0054 g cm–3, all measured with fractional uncertainties of only a few percent. Models of Kepler-68b suggest that it is likely composed of rock and water, or has a H and He envelope to yield its density ~3 g cm–3.Other Sources
https://arxiv.org/pdf/1302.2596.pdfTerms 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:29990211
Collections
- FAS Scholarly Articles [18256]
Contact administrator regarding this item (to report mistakes or request changes)