We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). © 2014. The American Astronomical Society. All rights reserved..
Masses, radii, and orbits of small Kepler planets: The transition from gaseous to rocky planets / Marcy G.W.; Isaacson H.; Howard A.W.; Rowe J.F.; Jenkins J.M.; Bryson S.T.; Latham D.W.; Howell S.B.; Gautier T.N.; Batalha N.M.; Rogers L.; Ciardi D.; Fischer D.A.; Gilliland R.L.; Kjeldsen H.; Christensen-Dalsgaard J.; Huber D.; Chaplin W.J.; Basu S.; Buchhave L.A.; Quinn S.N.; Borucki W.J.; Koch D.G.; Hunter R.; Caldwell D.A.; Van Cleve J.; Kolbl R.; Weiss L.M.; Petigura E.; Seager S.; Morton T.; Johnson J.A.; Ballard S.; Burke C.; Cochran W.D.; Endl M.; Macqueen P.; Everett M.E.; Lissauer J.J.; Ford E.B.; Torres G.; Fressin F.; Brown T.M.; Steffen J.H.; Charbonneau D.; Basri G.S.; Sasselov D.D.; Winn J.; Sanchis-Ojeda R.; Christiansen J.; Adams E.; Henze C.; Dupree A.; Fabrycky D.C.; Fortney J.J.; Tarter J.; Holman M.J.; Tenenbaum P.; Shporer A.; Lucas P.W.; Welsh W.F.; Orosz J.A.; Bedding T.R.; Campante T.L.; Davies G.R.; Elsworth Y.; Handberg R.; Hekker S.; Karoff C.; Kawaler S.D.; Lund M.N.; Lundkvist M.; Metcalfe T.S.; Miglio A.; Aguirre V.S.; Stello D.; White T.R.; Boss A.; Devore E.; Gould A.; Prsa A.; Agol E.; Barclay T.; Coughlin J.; Brugamyer E.; Mullally F.; Quintana E.V.; Still M.; Thompson S.E.; Morrison D.; Twicken J.D.; Desert J.-M.; Carter J.; Crepp J.R.; Hebrard G.; Santerne A.; Moutou C.; Sobeck C.; Hudgins D.; Haas M.R.; Robertson P.; Lillo-Box J.; Barrado D.. - In: ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES. - ISSN 0067-0049. - ELETTRONICO. - 210:2(2014), pp. 20.1-20.94. [10.1088/0067-0049/210/2/20]
Masses, radii, and orbits of small Kepler planets: The transition from gaseous to rocky planets
Miglio A.;
2014
Abstract
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). © 2014. The American Astronomical Society. All rights reserved..I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
