The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet

Xavier Dumusque; Aldo S. Bonomo; Raphaëlle D. Haywood; Luca Malavolta; Damien Ségransan; Lars A. Buchhave; Andrew Collier Cameron; David W. Latham; Emilio Molinari; Francesco Pepe; Stéphane Udry; David Charbonneau; Rosario Cosentino; Courtney D. Dressing; Pedro Figueira; Aldo F. M. Fiorenzano; Sara Gettel; Avet Harutyunyan; Keith Horne; Mercedes Lopez-Morales; Christophe Lovis; Michel Mayor; Giusi Micela; Fatemeh Motalebi; Valerio Nascimbeni; David F. Phillips; Giampaolo Piotto; Don Pollacco; Didier Queloz; Ken Rice; Dimitar Sasselov; Alessandro Sozzetti; Andrew Szentgyorgyi; Christopher Watson

doi:10.1088/0004-637X/789/2/154

The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet

Xavier Dumusque, Aldo S. Bonomo, Raphaëlle D. Haywood, Luca Malavolta, Damien Ségransan, Lars A. Buchhave, Andrew Collier Cameron, David W. Latham, Emilio Molinari, Francesco Pepe, Stéphane Udry, David Charbonneau, Rosario Cosentino, Courtney D. Dressing, Pedro Figueira, Aldo F. M. Fiorenzano, Sara Gettel, Avet Harutyunyan, Keith Horne, Mercedes Lopez-MoralesChristophe Lovis, Michel Mayor, Giusi Micela, Fatemeh Motalebi, Valerio Nascimbeni, David F. Phillips, Giampaolo Piotto, Don Pollacco, Didier Queloz, Ken Rice, Dimitar Sasselov, Alessandro Sozzetti, Andrew Szentgyorgyi, Christopher Watson

Research output: Contribution to journal › Article › peer-review

139 Citations (Scopus)

Abstract

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 1.47+0.03 −0.02 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 2.35+0.09 −0.04 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

Original language	English
Pages (from-to)	154
Number of pages	14
Journal	The Astrophysical Journal
Volume	789
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/789/2/154
Publication status	Published - 10 Jul 2014

Keywords

planetary systems
stars: individual: Kepler-10 KOI-072 KIC 11904151
stars: statistics
techniques: photometric
techniques: spectroscopic

Access to Document

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

http://adsabs.harvard.edu/abs/2014ApJ...789..154D

Christopher Watson
- c.a.watsonqub.acuk
- School of Mathematics and Physics - Professor
- Astrophysics Research Centre (ARC)
Person: Academic

Cite this

Dumusque, X., Bonomo, A. S., Haywood, R. D., Malavolta, L., Ségransan, D., Buchhave, L. A., Collier Cameron, A., Latham, D. W., Molinari, E., Pepe, F., Udry, S., Charbonneau, D., Cosentino, R., Dressing, C. D., Figueira, P., Fiorenzano, A. F. M., Gettel, S., Harutyunyan, A., Horne, K., ... Watson, C. (2014). The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet. The Astrophysical Journal, 789(2), 154. https://doi.org/10.1088/0004-637X/789/2/154

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title = "The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet",

abstract = "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 wasinsufficient 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 onlygood 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 spectrographon 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 1.47+0.03 −0.02 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 2.35+0.09 −0.04 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",

keywords = "planetary systems, stars: individual: Kepler-10 KOI-072 KIC 11904151, stars: statistics, techniques: photometric, techniques: spectroscopic",

author = "Xavier Dumusque and Bonomo, {Aldo S.} and Haywood, {Rapha{\"e}lle D.} and Luca Malavolta and Damien S{\'e}gransan and Buchhave, {Lars A.} and {Collier Cameron}, Andrew and Latham, {David W.} and Emilio Molinari and Francesco Pepe and St{\'e}phane Udry and David Charbonneau and Rosario Cosentino and Dressing, {Courtney D.} and Pedro Figueira and Fiorenzano, {Aldo F. M.} and Sara Gettel and Avet Harutyunyan and Keith Horne and Mercedes Lopez-Morales and Christophe Lovis and Michel Mayor and Giusi Micela and Fatemeh Motalebi and Valerio Nascimbeni and Phillips, {David F.} and Giampaolo Piotto and Don Pollacco and Didier Queloz and Ken Rice and Dimitar Sasselov and Alessandro Sozzetti and Andrew Szentgyorgyi and Christopher Watson",

year = "2014",

month = jul,

day = "10",

doi = "10.1088/0004-637X/789/2/154",

language = "English",

volume = "789",

pages = "154",

journal = "The Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd",

number = "2",

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Dumusque, X, Bonomo, AS, Haywood, RD, Malavolta, L, Ségransan, D, Buchhave, LA, Collier Cameron, A, Latham, DW, Molinari, E, Pepe, F, Udry, S, Charbonneau, D, Cosentino, R, Dressing, CD, Figueira, P, Fiorenzano, AFM, Gettel, S, Harutyunyan, A, Horne, K, Lopez-Morales, M, Lovis, C, Mayor, M, Micela, G, Motalebi, F, Nascimbeni, V, Phillips, DF, Piotto, G, Pollacco, D, Queloz, D, Rice, K, Sasselov, D, Sozzetti, A, Szentgyorgyi, A & Watson, C 2014, 'The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet', The Astrophysical Journal, vol. 789, no. 2, pp. 154. https://doi.org/10.1088/0004-637X/789/2/154

TY - JOUR

T1 - The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet

AU - Dumusque, Xavier

AU - Bonomo, Aldo S.

AU - Haywood, Raphaëlle D.

AU - Malavolta, Luca

AU - Ségransan, Damien

AU - Buchhave, Lars A.

AU - Collier Cameron, Andrew

AU - Latham, David W.

AU - Molinari, Emilio

AU - Pepe, Francesco

AU - Udry, Stéphane

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, Christopher

PY - 2014/7/10

Y1 - 2014/7/10

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 wasinsufficient 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 onlygood 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 spectrographon 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 1.47+0.03 −0.02 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 2.35+0.09 −0.04 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 wasinsufficient 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 onlygood 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 spectrographon 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 1.47+0.03 −0.02 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 2.35+0.09 −0.04 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

KW - planetary systems

KW - stars: individual: Kepler-10 KOI-072 KIC 11904151

KW - stars: statistics

KW - techniques: photometric

KW - techniques: spectroscopic

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

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

M3 - Article

SN - 0004-637X

VL - 789

SP - 154

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 2

ER -

The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and a Solid Neptune-Mass Planet

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