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Habitable zones for Earth-mass planets in multiple planetary systems

Published online by Cambridge University Press:  01 October 2007

Jianghui JI ,
Lin LIU ,
Hiroshi KINOSHITA  and
Guangyu LI
Jianghui JI
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: jijh@pmo.ac.cn
Lin LIU
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: xhliao@nju.edu.cn
Hiroshi KINOSHITA
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
Guangyu LI
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: jijh@pmo.ac.cn
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Abstract

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We perform numerical simulations to study the Habitable zones (HZs) and dynamical structure for Earth-mass planets in multiple planetary systems. For example, in the HD 69830 system, we extensively explore the planetary configuration of three Neptune-mass companions with one massive terrestrial planet residing in 0.07 AU ≤ a ≤ 1.20 AU, to examine the asteroid structure in this system. We underline that there are stable zones of at least 105 yr for low-mass terrestrial planets locating between 0.3 and 0.5 AU, and 0.8 and 1.2 AU with final eccentricities of e < 0.20. Moreover, we also find that the accumulation or depletion of the asteroid belt are also shaped by orbital resonances of the outer planets, for example, the asteroidal gaps at 2:1 and 3:2 mean motion resonances (MMRs) with Planet C, and 5:2 and 1:2 MMRs with Planet D. In a dynamical sense, the proper candidate regions for the existence of the potential terrestrial planets or HZs are 0.35 AU < a < 0.50 AU, and 0.80 AU < a < 1.00 AU for relatively low eccentricities, which makes sense to have the possible asteroidal structure in this system.

Keywords

methods:n-body simulations-planetary systems-stars:individual (HD69830, 47 UMa)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 499 - 502
Copyright
Copyright © International Astronomical Union 2008

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