TY - JOUR

T1 - The Kepler-10 planetary system revisited by HARPS-N

T2 - a hot rocky world and a solid Neptune-mass planet

AU - Dumusque, Xavier

AU - Bonomo, Aldo S.

AU - Haywood, Raphaelle D.

AU - Malavolta, Luca

AU - Segransan, Damien

AU - Buchhave, Lars A.

AU - Cameron, Andrew Collier

AU - Latham, David W.

AU - Molinari, Emilio

AU - Pepe, Francesco

AU - Udry, Stephane

AU - Charbonneau, David

AU - Cosentino, Rosario

AU - Dressing, Courtney D.

AU - Figueira, Pedro

AU - Fiorenzano, Aldo F. M.

AU - Gettel, Sara

AU - Harutyunyan, Avet

AU - Horne, Keith

AU - Lopez-Morales, Mercedes

AU - Lovis, Christophe

AU - Mayor, Michel

AU - Micela, Giusi

AU - Motalebi, Fatemeh

AU - Nascimbeni, Valerio

AU - Phillips, David F.

AU - Piotto, Giampaolo

AU - Pollacco, Don

AU - Queloz, Didier

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Sozzetti, Alessandro

AU - Szentgyorgyi, Andrew

AU - Watson, Chris

PY - 2014

Y1 - 2014

N2 - Kepler-10b was the first rocky planet detected by the Kepler satellite and confirmed with radial velocity follow-up observations from Keck-HIRES. The mass of the planet was measured with a precision of around 30%, which was insufficient to constrain models of its internal structure and composition in detail. In addition to Kepler-10b, a second planet transiting the same star with a period of 45 days was statistically validated, but the radial velocities were only good enough to set an upper limit of 20 M ⊕ for the mass of Kepler-10c. To improve the precision on the mass for planet b, the HARPS-N Collaboration decided to observe Kepler-10 intensively with the HARPS-N spectrograph on the Telescopio Nazionale Galileo on La Palma. In total, 148 high-quality radial-velocity measurements were obtained over two observing seasons. These new data allow us to improve the precision of the mass determination for Kepler-10b to 15%. With a mass of 3.33 ± 0.49 M ⊕ and an updated radius of  R ⊕, Kepler-10b has a density of 5.8 ± 0.8 g cm–3, very close to the value predicted by models with the same internal structure and composition as the Earth. We were also able to determine a mass for the 45-day period planet Kepler-10c, with an even better precision of 11%. With a mass of 17.2 ± 1.9 M ⊕ and radius of  R ⊕, Kepler-10c has a density of 7.1 ± 1.0 g cm–3. Kepler-10c appears to be the first strong evidence of a class of more massive solid planets with longer orbital periods.

AB - Kepler-10b was the first rocky planet detected by the Kepler satellite and confirmed with radial velocity follow-up observations from Keck-HIRES. The mass of the planet was measured with a precision of around 30%, which was insufficient to constrain models of its internal structure and composition in detail. In addition to Kepler-10b, a second planet transiting the same star with a period of 45 days was statistically validated, but the radial velocities were only good enough to set an upper limit of 20 M ⊕ for the mass of Kepler-10c. To improve the precision on the mass for planet b, the HARPS-N Collaboration decided to observe Kepler-10 intensively with the HARPS-N spectrograph on the Telescopio Nazionale Galileo on La Palma. In total, 148 high-quality radial-velocity measurements were obtained over two observing seasons. These new data allow us to improve the precision of the mass determination for Kepler-10b to 15%. With a mass of 3.33 ± 0.49 M ⊕ and an updated radius of  R ⊕, Kepler-10b has a density of 5.8 ± 0.8 g cm–3, very close to the value predicted by models with the same internal structure and composition as the Earth. We were also able to determine a mass for the 45-day period planet Kepler-10c, with an even better precision of 11%. With a mass of 17.2 ± 1.9 M ⊕ and radius of  R ⊕, Kepler-10c has a density of 7.1 ± 1.0 g cm–3. Kepler-10c appears to be the first strong evidence of a class of more massive solid planets with longer orbital periods.

U2 - 10.1088/0004-637X/789/2/154

DO - 10.1088/0004-637X/789/2/154

M3 - Journal article

VL - 789

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 154

ER -