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Pulsations of Proto-Giant-Planets

Published online by Cambridge University Press:  15 February 2018

G. Wuchterl
G. Wuchterl*
Affiliation:
Institut für Theoretische Astrophysik der Univ. Heidelberg, Germany and Institute for Theoretical Physics, UCSB, Santa Barbara, California

Abstract

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Nonlinear oscillations of proto-giant-planets have been found in recent numerical calculations relevant to planetary formation. Pulsations are excited in two phases of the protoplanetary evolution, (a) In an ‘instability strip’ at core masses of typically 0.2M⊙ (M⊕ is the earth mass). Perturbations grow into the nonlinear domain and saturate into perodic variations with relative luminosity-amplitudes of 0.2m (b) At the so called critical mass (typically at Mcore ≈ 15M⊕). There the pulsations drive a strong mass loss. A large portion of the envelope is ejected. Then the mass loss fades and the envelope settles into a new quasi-equilibrium. This remnant — a post nucleated instability protoplanet — has a compact envelope and is in core and envelope mass similar to Uranus and Neptune.

Type
Theoretical Breakthroughs
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 284
Copyright
Copyright © Cambridge University Press 1993

References

Wuchterl, G. 1990, Astron. Astrophys., 238, 83–94.Google Scholar
Wuchterl, G. 1991a, Icarus 91, 39–52.Google Scholar
Wuchterl, G. 1991b, Icarus 91, 53–64.Google Scholar