dc.contributor.author | Batalha, Natalie M. | |
dc.contributor.author | Borucki, William J. | |
dc.contributor.author | Bryson, Stephen T. | |
dc.contributor.author | Buchhave, Lars A. | |
dc.contributor.author | Caldwell, Douglas A. | |
dc.contributor.author | Christensen-Dalsgaard, Jørgen | |
dc.contributor.author | Ciardi, David | |
dc.contributor.author | Dunham, Edward W. | |
dc.contributor.author | Fressin, Francois | |
dc.contributor.author | Gautier, Thomas N. | |
dc.contributor.author | Gilliland, Ronald L. | |
dc.contributor.author | Haas, Michael R. | |
dc.contributor.author | Howell, Steve B. | |
dc.contributor.author | Jenkins, Jon M. | |
dc.contributor.author | Kjeldsen, Hans | |
dc.contributor.author | Koch, David G. | |
dc.contributor.author | Latham, David W. | |
dc.contributor.author | Lissauer, Jack J. | |
dc.contributor.author | Marcy, Geoffrey W. | |
dc.contributor.author | Rowe, Jason F. | |
dc.contributor.author | Sasselov, Dimitar D. | |
dc.contributor.author | Seager, Sara | |
dc.contributor.author | Steffen, Jason H. | |
dc.contributor.author | Torres, Guillermo | |
dc.contributor.author | Basri, Gibor S. | |
dc.contributor.author | Brown, Timothy M. | |
dc.contributor.author | Charbonneau, David | |
dc.contributor.author | Christiansen, Jessie | |
dc.contributor.author | Clarke, Bruce | |
dc.contributor.author | Cochran, William D. | |
dc.contributor.author | Dupree, Andrea | |
dc.contributor.author | Fabrycky, Daniel C. | |
dc.contributor.author | Fischer, Debra | |
dc.contributor.author | Ford, Eric B. | |
dc.contributor.author | Fortney, Jonathan | |
dc.contributor.author | Girouard, Forrest R. | |
dc.contributor.author | Holman, Matthew J. | |
dc.contributor.author | Johnson, John | |
dc.contributor.author | Isaacson, Howard | |
dc.contributor.author | Klaus, Todd C. | |
dc.contributor.author | Machalek, Pavel | |
dc.contributor.author | Moorehead, Althea V. | |
dc.contributor.author | Morehead, Robert C. | |
dc.contributor.author | Ragozzine, Darin | |
dc.contributor.author | Tenenbaum, Peter | |
dc.contributor.author | Twicken, Joseph | |
dc.contributor.author | Quinn, Samuel | |
dc.contributor.author | VanCleve, Jeffrey | |
dc.contributor.author | Walkowicz, Lucianne M. | |
dc.contributor.author | Welsh, William F. | |
dc.contributor.author | Devore, Edna | |
dc.contributor.author | Gould, Alan | |
dc.date.accessioned | 2019-09-24T17:25:11Z | |
dc.date.issued | 2011 | |
dc.identifier.citation | Batalha, Natalie M., William J. Borucki, Stephen T. Bryson, Lars A. Buchhave, Douglas A. Caldwell, Jørgen Christensen-Dalsgaard, David Ciardi, et al. 2011. “KEPLER’S FIRST ROCKY PLANET: KEPLER-10b.” The Astrophysical Journal 729 (1): 27. https://doi.org/10.1088/0004-637x/729/1/27. | |
dc.identifier.issn | 0004-637X | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.uri | http://nrs.harvard.edu/urn-3:HUL.InstRepos:41397410 | * |
dc.description.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(-0.00082)(+0.00060) + N * 0.837495(-0.000005)(+0.000004) days and (2) a 376 +/- 9 ppm dimming lasting 6.86 +/- 0.07 hr with ephemeris T [BJD] = 2454971.6761(-0.0023)(+0.0020) + N * 45.29485(-0.00076)(+0.00065) 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-star = 0.895 +/- 0.060M(circle dot), and R-star = 1.056 +/- 0.021R(circle dot). 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(-1.29)(+1.17) M-circle plus, R-P = 1.416(-0.036)(+0.033) R-circle plus, and rho P = 8.8(-2.9)(+2.1) g cm(-3). Kepler-10b is the smallest transiting exoplanet discovered to date. | |
dc.language.iso | en_US | |
dc.publisher | American Astronomical Society | |
dash.license | LAA | |
dc.title | Kepler 's First Rocky Planet: Kepler-10b | |
dc.type | Journal Article | |
dc.description.version | Version of Record | |
dc.relation.journal | The Astrophysical Journal | |
dash.depositing.author | Charbonneau, David::a0e3ca75d3fb8511f2f554ed69428108::600 | |
dc.date.available | 2019-09-24T17:25:11Z | |
dash.workflow.comments | 1Science Serial ID 98817 | |
dc.identifier.doi | 10.1088/0004-637X/729/1/27 | |
dash.source.volume | 729;1 | |
dash.source.page | 27 | |