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Orbital Eccentricity Growth through Disc–Companion Tidal Interactions

Published online by Cambridge University Press:  26 May 2016

Richard P. Nelson ,
John C.B. Papaloizou  and
Frédéric Masset
Richard P. Nelson
Affiliation:
Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
John C.B. Papaloizou
Affiliation:
Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Frédéric Masset
Affiliation:
Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London E1 4NS, UK

Abstract

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We present the results of 2–D non linear hydrodynamic simulations performed to examine the driving of orbital eccentricity through disc-companion tidal interaction. We examine the eccentricity evolution for companion masses, mp, in the range 1 > mp >; 30 MJupiter. The disc model we employ is similar to a minimum mass solar nebula model.

We find that there is a transition in behaviour, characterised by a rapid growth in eccentricity, for companion masses mp ≳ 20 MJupiter. Companions with masses below this limit show essentially no growth in eccentricity, for the disc model parameters that we examine. Our results suggest that if giant planets form from protostellar discs with properties similar to those studied in this paper, then the observed orbital eccentricities of the extrasolar planets are not a consequence of tidal interaction with their protostellar discs during formation.

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. 226 - 228
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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