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Stable mass ranges of ν Andromedae planetary system

Published online by Cambridge University Press:  26 May 2016

Takashi Ito  and
Shoken M. Miyama
Takashi Ito
Affiliation:
Astronomical Data Analysis Computer Center, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
Shoken M. Miyama
Affiliation:
Theoretical Astrophysics Division, National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan

Abstract

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Doppler observation of extrasolar planets through the radial velocity displacement of their host stars can only determine lower limits of planetary masses. We numerically integrate ν Andromedae planetary orbits with various initial conditions of masses and angle variables to investigate which initial configuration produces stable orbits during the timescale of host star's age. According to our preliminary results starting from Lick dataset, ν Andromedae planetary system seems to remain stable over the timescale of its host star's age if sin i > 0.7 where i is the unknown line-of-sight inclination of planetary orbits. In this case we may estimate that the upper limit masses of ν Andromedae planets in our model is about 1/0.7 ∽ 1.43 times larger than its minimum.

Type
Part II: Progress in the theory of planet formation
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 193 - 195
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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