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Instability of mass transfer in a planet-star system
Jia S(贾石)1,2,3,4; Spruit, H. C.2
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2017-02-11
Volume465Issue:1Pages:149-160
DOI10.1093/mnras/stw1693
Contribution Rank第1完成单位
Indexed BySCI
KeywordPlanets And Satellites: General Planet-star Interactions Stars: General Planetary Systems
Abstract

We show that the angular momentum exchange mechanism governing the evolution of mass-transferring binary stars does not apply to Roche lobe filling planets, because most of the angular momentum of the mass-transferring stream is absorbed by the host star. Apart from a correction for the difference in specific angular momentum of the stream and the centre of mass of the planet, the orbit does not expand much on Roche lobe overflow. We explore the conditions for dynamically unstable Roche lobe overflow as a function of planetary mass and mass and radius (age) of host star and equation of state of planet. For a Sun-like host, gas giant planets in a range of mass and entropy can undergo dynamical mass transfer. Examples of the evolution of the mass transfer process are given. Dynamic mass transfer of rocky planets depends somewhat sensitively on equation of state used. Silicate planets in the range 1 < M-p < 10M(circle plus) typically go through a phase of dynamical mass transfer before settling to slow overflow when their mass drops to less than 1 M-circle plus.

Funding ProjectMPG-CAS Joint Doctoral Promotion Program (DPP) ; Max Planck Institute for Astrophysics (MPA)
Funding OrganizationMPG-CAS Joint Doctoral Promotion Program (DPP) ; Max Planck Institute for Astrophysics (MPA)
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
Archive Date2017-01-05
WOS IDWOS:000393782000012
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordROCHE-LOBE OVERFLOW ; CATACLYSMIC VARIABLE EVOLUTION ; CLASSICAL T-TAURI ; CLOSE-IN PLANETS ; GIANT PLANETS ; CIRCUMBINARY DISKS ; ACCRETION DISKS ; MAGNETIC-FIELD ; BINARY-SYSTEMS ; HOT JUPITERS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9924
Collection大样本恒星演化研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorJia S(贾石)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
2.Max-Planck-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany
3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
4.University of Chinese Academy of Sciences, Beijing 100049, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Jia S,Spruit, H. C.. Instability of mass transfer in a planet-star system[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2017,465(1):149-160.
APA Jia S,&Spruit, H. C..(2017).Instability of mass transfer in a planet-star system.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,465(1),149-160.
MLA Jia S,et al."Instability of mass transfer in a planet-star system".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 465.1(2017):149-160.
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