Dynamical evolution and stability maps of the Proxima Centauri system

doi:10.1093/mnras/sty2682

	Dynamical evolution and stability maps of the Proxima Centauri system
	Meng, Tong 1,2; Ji, Jianghui1 ; Dong, Yao1
刊名	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
	2019
卷号	482 期号:1 页码:372-383
关键词	methods: numerical celestial mechanics planets and satellites: dynamical evolution and stability stars: individual: Proxima Centauri
ISSN号	0035-8711
DOI	10.1093/mnras/sty2682
通讯作者	Ji, Jianghui(jijh@pmo.ac.cn)
英文摘要	Proxima Centauri was recently discovered to host an Earth-mass planet of Proxima b, and a 215-d signal which is probably a potential planet c. In this work, we investigate the dynamical evolution of the Proxima Centauri system with the full equations of motion and semi-analytical models including relativistic and tidal effects. We adopt the modified Lagrange-Laplace secular equations to study the evolution of eccentricity of Proxima b, and find that the outcomes are consistent with those from the numerical simulations. The simulations show that relativistic effects have an influence on the evolution of eccentricities of planetary orbits, whereas tidal effects primarily affects the eccentricity of Proxima b over long time-scale. Moreover, using the MEGNO (the Mean Exponential Growth factor of Nearby Orbits) technique, we place dynamical constraints on orbital parameters that result in stable or quasi-periodic motions for coplanar and non-coplanar configurations. In the coplanar case, we find that the orbit of Proxima b is stable for the semi-major axis ranging from 0.02 au to 0.1 au and the eccentricity being less than 0.4. This is where the best-fitting parameters for Proxima b exactly fall. Additional simulations show that the robust stability of this system would favour an eccentricity of Proxima b less than 0.45 and that of Proxima c below 0.65. In the non-coplanar case, we find that mutual inclinations of two planets must be lower than 50A degrees in order to provide stability. Finally, we estimate the mass of Proxima c to be 3.13 M-aS center dot a parts per thousand 70.7 M-aS center dot, when 1.27 M-aS center dot a parts per thousand 1.6 M-aS center dot, if i(mutual) a parts per thousand> 50A degrees and Delta Omega = 0A degrees.
WOS关键词	TIDAL EVOLUTION ; PLANETARY SYSTEM ; GLOBAL DYNAMICS ; HABITABLE ZONES ; MOTION ; CIRCULARIZATION ; MIGRATION ; ORBIT ; MASS
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	OXFORD UNIV PRESS
WOS记录号	WOS:000454575300029
内容类型	期刊论文
源URL	[http://libir.pmo.ac.cn/handle/332002/20502]
专题	中国科学院紫金山天文台
通讯作者	Ji, Jianghui
作者单位	1.Chinese Acad Sci, CAS Key Lab Planetary Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China 2.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
推荐引用方式 GB/T 7714	Meng, Tong,Ji, Jianghui,Dong, Yao. Dynamical evolution and stability maps of the Proxima Centauri system[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2019,482(1):372-383.
APA	Meng, Tong,Ji, Jianghui,&Dong, Yao.(2019).Dynamical evolution and stability maps of the Proxima Centauri system.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,482(1),372-383.
MLA	Meng, Tong,et al."Dynamical evolution and stability maps of the Proxima Centauri system".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 482.1(2019):372-383.