In-depth characterization of the Kepler-10 three-planet system with HARPS-N radial velocities and <i>Kepler</i> transit timing variations

The old G3V star Kepler-10 is known to host two transiting planets, the ultra-short-period super-Earth Kepler-10 b ( P b = 0.837 d; R b = 1.47 R ⊕ ) and the long-period sub-Neptune Kepler-10 c ( P c = 45.294 d; R c = 2.35 R ⊕ ), and a non-transiting planet that causes variations in the Kepler-10 c transit times. Measurements of the mass of Kepler-10 c in the literature have shown disagreement, depending on the radial-velocity dataset and/or the modeling technique used. Here we report on the analysis of almost 300 high-precision radial velocities gathered with the HARPS-N spectrograph at the Telescopio Nazionale Galileo over ∼11 years, and extracted with the YARARA-v2 tool, which corrects for possible systematics and/or low-level activity variations at the spectrum level. To model these radial velocities, we used three different noise models and various numerical techniques, which all converged to the solution: M b = 3.24 ± 0.32 M ⊕ (10 σ ) and ρ b = 5.54 ± 0.64 g cm −3 for planet b; M c = 11.29 ± 1.24 M ⊕ (9 σ ) and ρ c = 4.75 ± 0.53 g cm −3 for planet c; and M d sin i = 12.00 ± 2.15 M ⊕ (6 σ ) and P d = 151.06 ± 0.48 d for the non-transiting planet Kepler-10 d. This solution is further supported by the analysis of the Kepler-10 c transit timing variations and their simultaneous modeling with the HARPS-N radial velocities. While Kepler-10 b is consistent with a rocky composition and a small or no iron core, Kepler-10 c may be a water world that formed beyond the water snowline and subsequently migrated inward.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-03-28
DOI
https://doi.org/10.1051/0004-6361/202453026
Citations
3
Primary Topic
Stellar, planetary, and galactic studies
Type
article
Field-Weighted Citation Impact
3.46

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article

In-depth characterization of the Kepler-10 three-planet system with HARPS-N radial velocities and Kepler transit timing variations

Ken Rice, A. S. Bonomo, L. Malavolta, Annelies Mortier et al.
3 citations
Astronomy and Astrophysics
Stellar, planetary, and galactic studies
3.46
article

In-depth characterization of the Kepler-10 three-planet system with HARPS-N radial velocities and Kepler transit timing variations

Ken Rice, A. S. Bonomo, L. Malavolta, Annelies Mortier, L. Borsato, A.C. Cameron, Vinesh Rajpaul, F. Lienhard, A. Leleu, A. Ghedina, Alessandro Sozzetti, M. Damasso, G. Lacedelli, S. Udry, Luca Naponiello, R. Bongiolatti, E. Poretti, Lars A. Buchhave, N.C. Hara, D.W. Latham, M. Cretignier, F. Pepe, A. Massa, R. D. Haywood, A. Martinez Fiorenzano, N. Unger, X. Dumusque, Li Zeng
article en
3 citations

Abstract

The old G3V star Kepler-10 is known to host two transiting planets, the ultra-short-period super-Earth Kepler-10 b ( P b = 0.837 d; R b = 1.47 R ⊕ ) and the long-period sub-Neptune Kepler-10 c ( P c = 45.294 d; R c = 2.35 R ⊕ ), and a non-transiting planet that causes variations in the Kepler-10 c transit times. Measurements of the mass of Kepler-10 c in the literature have shown disagreement, depending on the radial-velocity dataset and/or the modeling technique used. Here we report on the analysis of almost 300 high-precision radial velocities gathered with the HARPS-N spectrograph at the Telescopio Nazionale Galileo over ∼11 years, and extracted with the YARARA-v2 tool, which corrects for possible systematics and/or low-level activity variations at the spectrum level. To model these radial velocities, we used three different noise models and various numerical techniques, which all converged to the solution: M b = 3.24 ± 0.32 M ⊕ (10 σ ) and ρ b = 5.54 ± 0.64 g cm −3 for planet b; M c = 11.29 ± 1.24 M ⊕ (9 σ ) and ρ c = 4.75 ± 0.53 g cm −3 for planet c; and M d sin i = 12.00 ± 2.15 M ⊕ (6 σ ) and P d = 151.06 ± 0.48 d for the non-transiting planet Kepler-10 d. This solution is further supported by the analysis of the Kepler-10 c transit timing variations and their simultaneous modeling with the HARPS-N radial velocities. While Kepler-10 b is consistent with a rocky composition and a small or no iron core, Kepler-10 c may be a water world that formed beyond the water snowline and subsequently migrated inward.

Astronomy and AstrophysicsVol. 696
University of Geneva (CH), Centre National de la Recherche Scientifique (FR), Planetary Science Institute (US), Harvard University (US), University of Padua (IT), University of St Andrews (GB), Isaac Newton Institute for Mathematical Sciences (GB), University of Milan (IT), Aix-Marseille Université (FR), University of Exeter (GB), University of Cambridge (GB), Brera Astronomical Observatory (IT), ETH Zurich (CH), University of Oxford (GB), Osservatorio Astrofisico di Torino (IT), Center for Astrophysics Harvard & Smithsonian (US), Instituto de Astrofísica de Canarias (ES), Osservatorio Astronomico di Padova (IT), Telescopio Nazionale Galileo (ES), UK Astronomy Technology Centre (GB), University of Turin (IT), University of Birmingham (GB), Technical University of Denmark (DK), University of Edinburgh (GB)
National Science Foundation, Smithsonian Institution, U.S. Department of Energy, National Aeronautics and Space Administration, Harvard University, UK Research and Innovation, Scottish Universities Physics Alliance, University of St Andrews, European Commission, Queen's University Belfast, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, Queen's University, Université de Genève, National Nuclear Security Administration, Smithsonian Astrophysical Observatory, Science Mission Directorate, Science and Technology Facilities Council
Openalex Percentile: Top 8%
Stellar, planetary, and galactic studies
3.46
DOIOpen Access PDFOpenAlex
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