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Kepler-102 : masses and compositions for a super-Earth and sub-Neptune orbiting an active star

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Date
01/02/2023
Author
Brinkman, Casey L.
Cadman, James
Weiss, Lauren
Gaidos, Eric
Rice, Ken
Huber, Daniel
Claytor, Zachary R.
Bonomo, Aldo S.
Buchhave, Lars A.
Cameron, Andrew Collier
Cosentino, Rosario
Dumusque, Xavier
Martinez Fiorenzano, Aldo F.
Ghedina, Adriano
Harutyunyan, Avet
Howard, Andrew
Isaacson, Howard
Latham, David W.
López-Morales, Mercedes
Malavolta, Luca
Micela, Giuseppina
Molinari, Emilio
Pepe, Francesco
Philips, David F.
Poretti, Ennio
Sozzetti, Alessandro
Udry, Stéphane
Keywords
QB Astronomy
QC Physics
3rd-DAS
MCC
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Abstract
Radial velocity (RV) measurements of transiting multiplanet systems allow us to understand the densities and compositions of planets unlike those in the solar system. Kepler-102, which consists of five tightly packed transiting planets, is a particularly interesting system since it includes a super-Earth (Kepler-102d) and a sub-Neptune-sized planet (Kepler-102e) for which masses can be measured using RVs. Previous work found a high density for Kepler-102d, suggesting a composition similar to that of Mercury, while Kepler-102e was found to have a density typical of sub-Neptune size planets; however, Kepler-102 is an active star, which can interfere with RV mass measurements. To better measure the mass of these two planets, we obtained 111 new RVs using Keck/HIRES and Telescopio Nazionale Galileo/HARPS-N and modeled Kepler-102's activity using quasiperiodic Gaussian process regression. For Kepler-102d, we report a mass upper limit Md < 5.3 M⊕ (95% confidence), a best-fit mass Md = 2.5 ± 1.4 M⊕, and a density ρd = 5.6 ± 3.2 g cm−3, which is consistent with a rocky composition similar in density to the Earth. For Kepler-102e we report a mass Me = 4.7 ± 1.7 M⊕ and a density ρe = 1.8 ± 0.7 g cm−3. These measurements suggest that Kepler-102e has a rocky core with a thick gaseous envelope comprising 2%–4% of the planet mass and 16%–50% of its radius. Our study is yet another demonstration that accounting for stellar activity in stars with clear rotation signals can yield more accurate planet masses, enabling a more realistic interpretation of planet interiors.
Citation
Brinkman , C L , Cadman , J , Weiss , L , Gaidos , E , Rice , K , Huber , D , Claytor , Z R , Bonomo , A S , Buchhave , L A , Cameron , A C , Cosentino , R , Dumusque , X , Martinez Fiorenzano , A F , Ghedina , A , Harutyunyan , A , Howard , A , Isaacson , H , Latham , D W , López-Morales , M , Malavolta , L , Micela , G , Molinari , E , Pepe , F , Philips , D F , Poretti , E , Sozzetti , A & Udry , S 2023 , ' Kepler-102 : masses and compositions for a super-Earth and sub-Neptune orbiting an active star ' , Astronomical Journal , vol. 165 , no. 2 , 74 . https://doi.org/10.3847/1538-3881/aca64d
Publication
Astronomical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-3881/aca64d
ISSN
0004-6256
Type
Journal article
Rights
Copyright © 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
Description
Funding: This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 1842402. C.L.B., L.W., and D.H. acknowledge support from National Aeronautics and Space Administration (grant No. 80NSSC19K0597) issued through the Astrophysics Data Analysis Program. D.H. also acknowledges support from the Alfred P. Sloan Foundation. K.R. acknowledges support from the UK STFC via grant No. ST/V000594/1. E.G. acknowledges support from NASA grant No. 80NSSC20K0957 (Exoplanets Research Program).
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/26857

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