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Kepler's First Rocky Planet: Kepler-10b

Batalha, Natalie M. and Ciardi, David and Johnson, John (2011) Kepler's First Rocky Planet: Kepler-10b. Astrophysical Journal, 729 (1). Art. No. 27. ISSN 0004-637X.

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NASA's Kepler Mission uses transit photometry to determine the frequency of Earth-size planets in or near the habitable zone of Sun-like stars. The mission reached a milestone toward meeting that goal: the discovery of its first rocky planet, Kepler-10b. Two distinct sets of transit events were detected: (1) a 152 ± 4 ppm dimming lasting 1.811 ± 0.024 hr with ephemeris T [BJD] = 2454964.57375^(+0.00060)_(–0.00082) + N * 0.837495^(+0.000004)_(–0.000005) days and (2) a 376 ± 9 ppm dimming lasting 6.86 ± 0.07 hr with ephemeris T [BJD] = 2454971.6761^(+0.0020)_(–0.0023) + N * 45.29485^(+0.00065) _(–0.00076) days. Statistical tests on the photometric and pixel flux time series established the viability of the planet candidates triggering ground-based follow-up observations. Forty precision Doppler measurements were used to confirm that the short-period transit event is due to a planetary companion. The parent star is bright enough for asteroseismic analysis. Photometry was collected at 1 minute cadence for >4 months from which we detected 19 distinct pulsation frequencies. Modeling the frequencies resulted in precise knowledge of the fundamental stellar properties. Kepler-10 is a relatively old (11.9 ± 4.5 Gyr) but otherwise Sun-like main-sequence star with T_(eff) = 5627 ± 44 K, M_⋆ = 0.895 ± 0.060 M_⊙ , and R_⋆ = 1.056 ± 0.021 R_⊙. Physical models simultaneously fit to the transit light curves and the precision Doppler measurements yielded tight constraints on the properties of Kepler-10b that speak to its rocky composition: M_P = 4.56^9+1.17)_(–1.29) M_⊕, R_P = 1.416^(+0.033)_(–0.036) R_⊕, and ρ_P = 8.8^(+2.1)_(–2.9) g cm^(–3). Kepler-10b is the smallest transiting exoplanet discovered to date.

Item Type:Article
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Ciardi, David0000-0002-5741-3047
Additional Information:© 2011 American Astronomical Society. Received 2010 November 10; accepted 2010 November 25; published 2011 February 7. Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology. The authors thank Carly Chubak for computing the barycentric radial velocity of Kepler-10. J.C.D. acknowledges support from The National Center for Atmospheric Research which is sponsored by the National Science Foundation. Funding for this Discovery mission is provided by NASA’s Science Mission Directorate.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Subject Keywords:planetary systems – stars: individual (Kepler-10, KIC 11904151, 2MASS 19024305+5014286) – techniques: photometric – techniques: spectroscopic
Issue or Number:1
Classification Code:PACS: 97.82.-j, 95.10.Gi, 97.10.Sj, 97.20.Jg
Record Number:CaltechAUTHORS:20110314-105719990
Persistent URL:
Official Citation:Natalie M. Batalha et al. 2011 ApJ 729 27 doi: 10.1088/0004-637X/729/1/27
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22854
Deposited By: Benjamin Perez
Deposited On:15 Mar 2011 15:22
Last Modified:03 Oct 2019 02:41

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