KEPLER'S FIRST ROCKY PLANET: KEPLER-10b

被引：415

作者：

Batalha, Natalie M. ^{[1
]}

Borucki, William J.

Bryson, Stephen T.

Buchhave, Lars A. ^{[3
]}

Caldwell, Douglas A. ^{[2
]}

Christensen-Dalsgaard, Jorgen ^{[4
,5
]}

Ciardi, David ^{[6
]}

Dunham, Edward W. ^{[7
]}

Fressin, Francois ^{[3
]}

Gautier, Thomas N., III ^{[8
]}

Gilliland, Ronald L. ^{[9
]}

Haas, Michael R.

Howell, Steve B. ^{[10
]}

Jenkins, Jon M. ^{[2
]}

Kjeldsen, Hans ^{[4
]}

Koch, David G.

Latham, David W. ^{[3
]}

Lissauer, Jack J.

Marcy, Geoffrey W. ^{[11
]}

Rowe, Jason F.

Sasselov, Dimitar D. ^{[3
]}

Seager, Sara ^{[12
]}

Steffen, Jason H. ^{[13
]}

Torres, Guillermo ^{[3
]}

Basri, Gibor S. ^{[11
]}

Brown, Timothy M. ^{[14
]}

Charbonneau, David ^{[3
]}

Christiansen, Jessie

Clarke, Bruce ^{[2
]}

Cochran, William D. ^{[15
]}

Dupree, Andrea ^{[3
]}

Fabrycky, Daniel C. ^{[3
]}

Fischer, Debra ^{[16
]}

Ford, Eric B. ^{[17
]}

Fortney, Jonathan ^{[18
]}

Girouard, Forrest R. ^{[19
]}

Holman, Matthew J. ^{[3
]}

Johnson, John

Isaacson, Howard ^{[11
]}

Klaus, Todd C. ^{[19
]}

Machalek, Pavel ^{[2
]}

Moorehead, Althea V. ^{[17
]}

Morehead, Robert C. ^{[17
]}

Ragozzine, Darin ^{[3
]}

Tenenbaum, Peter ^{[2
]}

Twicken, Joseph ^{[2
]}

Quinn, Samuel ^{[3
]}

VanCleve, Jeffrey ^{[2
]}

Walkowicz, Lucianne M. ^{[11
]}

Welsh, William F. ^{[20
]}

机构：

[1] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA

[2] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[4] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[5] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA

[6] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA

[7] Lowell Observ, Flagstaff, AZ 86001 USA

[8] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[9] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[10] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[11] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[12] MIT, Cambridge, MA 02139 USA

[13] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA

[14] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA

[15] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[16] Yale Univ, Dept Astron, New Haven, CT 06510 USA

[17] Univ Florida, Dept Astron, Gainesville, FL 32611 USA

[18] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[19] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA

[20] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA

[21] Lawrence Hall Sci, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 729卷 / 01期

基金：

美国国家科学基金会;

关键词：

planetary systems; stars:; individual; (Kepler-10; KIC; 11904151; 2MASS; 19024305+5014286); techniques: photometric; techniques: spectroscopic; MASS-RADIUS RELATIONSHIPS; TESTING BLEND SCENARIOS; INITIAL CHARACTERISTICS; LIGHT CURVES; SUPER-EARTHS; EXOPLANET; STARS; EVOLUTION; OSCILLATIONS; CANDIDATES;

D O I：

10.1088/0004-637X/729/1/27

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：21

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