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Formation and stellar spin-orbit misalignment of hot Jupiters from Lidov–Kozai oscillations in stellar binaries

Anderson, Kassandra R. and Storch, Natalia I. and Lai, Dong (2016) Formation and stellar spin-orbit misalignment of hot Jupiters from Lidov–Kozai oscillations in stellar binaries. Monthly Notices of the Royal Astronomical Society, 456 (4). pp. 3671-3701. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20160408-104645132

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Abstract

Observed hot Jupiter (HJ) systems exhibit a wide range of stellar spin-orbit misalignment angles. This paper investigates the inward migration of giant planets due to Lidov–Kozai (LK) oscillations induced by a distant stellar companion. We conduct a large population synthesis study, including the octupole gravitational potential from the stellar companion, mutual precession of the host stellar spin axis and planet orbital axis, tidal dissipation in the planet and stellar spin-down in the host star due to magnetic braking. We consider a range of planet masses (0.3–5 MJ) and initial semimajor axes (1–5 au), different properties for the host star, and varying tidal dissipation strengths. The fraction of systems that result in HJs depends on planet mass and stellar type, with fHJ = 1–4 per cent (depending on tidal dissipation strength) for M_p = 1 MJ, and larger (up to 8 per cent) for more massive planets. The production efficiency of ‘hot Saturns’ (M_p = 0.3MJ) is much lower, because most migrating planets are tidally disrupted. We find that the fraction of systems that result in either HJ formation or tidal disruption, f_(mig) ≃ 11–14 per cent is roughly constant, having little variation with planet mass, stellar type and tidal dissipation strength. The distribution of final HJ stellar obliquities exhibits a complex dependence on the planet mass and stellar type. For M_p = (1–3)MJ, the distribution is always bimodal, with peaks around 30° and 130°. The distribution for 5MJ planets depends on host stellar type, with a preference for low obliquities for solar-type stars, and higher obliquities for more massive (1.4 M_⊙) stars.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stv2906DOIArticle
https://mnras.oxfordjournals.org/content/456/4/3671PublisherArticle
http://arxiv.org/abs/1510.08918arXivDiscussion Paper
Additional Information:© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 December 8. Received 2015 October 29. First published online January 14, 2016. We thank Diego Muñoz and Smadar Naoz for useful discussions, and especially Cristobal Petrovich for useful discussion and comments on the manuscript. This work has been supported in part by NSF grant AST-1211061, and NASA grants NNX14AG94G and NNX14AP31G. KRA is supported by the NSF Graduate Research Fellowship Program under Grant No. DGE-1144153.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFAST-1211061
NASANNX14AG94G
NASANNX14AP31G
NSF Graduate Research FellowshipDGE-1144153
Subject Keywords: planets and satellites: dynamical evolution and stability – planet–star interactions binaries: general
Record Number:CaltechAUTHORS:20160408-104645132
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160408-104645132
Official Citation: Kassandra R. Anderson, Natalia I. Storch, and Dong Lai Formation and stellar spin-orbit misalignment of hot Jupiters from Lidov–Kozai oscillations in stellar binaries MNRAS (March 11, 2016) Vol. 456 3671-3701 doi:10.1093/mnras/stv2906 First published online January 14, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:66020
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:08 Apr 2016 18:18
Last Modified:08 Apr 2016 18:18

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