Kepler's first rocky planet: Kepler-10b

Batalha, Natalie M. and Borucki, William J. and Bryson, Stephen T. and Buchhave, Lars A. and Caldwell, Douglas A. and Christensen-Dalsgaard, Jorgen and Ciardi, David and Dunham, Edward W. and Fressin, Francois and Gautier, Thomas N. and Gilliland, Ronald L. and Haas, Michael R. and Howell, Steve B. and Jenkins, Jon M. and Kjeldsen, Hans and Koch, David G. and Latham, David W. and Lissauer, Jack J. and Marcy, Geoffrey W. and Rowe, Jason F. and Sasselov, Dimitar D. and Seager, Sara and Steffen, Jason H. and Torres, Guillermo and Basri, Gibor S. and Brown, Timothy M. and Charbonneau, David and Christiansen, Jessie and Clarke, Bruce and Cochran, William D. and Dupree, Andrea and Fabrycky, Daniel C. and Fischer, Debra and Ford, Eric B. and Fortney, Jonathan and Girouard, Forrest R. and Holman, Matthew J. and Johnson, John and Isaacson, Howard and Klaus, Todd C. and MacHalek, Pavel and Moorehead, Althea V. and Morehead, Robert C. and Ragozzine, Darin and Tenenbaum, Peter and Twicken, Joseph and Quinn, Samuel and Van Cleve, Jeffrey and Walkowicz, Lucianne M. and Welsh, William F. and DeVore, Edna and Gould, Alan (2011) Kepler's first rocky planet: Kepler-10b. The Astrophysical Journal, 729 (1). pp. 27-47. ISSN 0004-637X

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Abstract

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 9ppm 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 4.5Gyr) but otherwise Sun-like main-sequence star with T eff = 5627 44K, 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+1.17 -1.29 M ⊕, R P = 1.416+0.033 -0.036 R ⊕, and ρP = 8.8+2.1 -2.9gcm-3. Kepler-10b is the smallest transiting exoplanet discovered to date.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Access to published version in accordance with the copyright policy of the publisher.
Faculty / Department / School: No Faculty
Date Deposited: 13 Jun 2017 01:24
Last Modified: 27 Jun 2017 05:00
Uncontrolled Keywords: planetary systems; photometric; spectroscopic;
Fields of Research : 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Socio-Economic Objective: E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Identification Number or DOI: 10.1088/0004-637X/729/1/27
URI: http://eprints.usq.edu.au/id/eprint/32174

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