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
SN - 0004-637X
VL - 789
JO - The Astrophysical Journal
JF - The Astrophysical Journal
IS - 2
M1 - 154
ER -