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Effect of mass gain on stellar evolution

Published online by Cambridge University Press:  12 April 2016

R. Ebert  and
H. Zinnecker
R. Ebert
Affiliation:
Institut für Theoretische Physik der Universität Würzburg, F.R.G.
H. Zinnecker
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, Institut für Extraterrestrische Physik Garching, F.R.G.

Abstract

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In this paper we present a fully hydrodynamical treatment of the stationary isothermal accretion problem onto a moving gravitating point mass. The derivation is purely analytical. We find that the accretion rate is more than a factor of 50 higher than the accretion rate derived from the partially non-hydrodynamical treatment by Hoyle and Lyttleton (1939) or Bondi and Hoyle (1944). This result may have some bearing on the evolutionary tracks of young pre-Main Sequence stars still embedded in their parent protocluster cloud. We discuss the work by Federova (1979) who investigated the pre-Main Sequence evolution of degenerate low mass ‘stars’ with strong accretion of protocluster cloud material. We suggest that the stars which lie below the Main Sequence in young clusters could strongly accrete matter at the pre-Main Sequence stage.

Type
Session VI - Mass Loss and Stellar Evolution: Low Mass Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 361 - 371
Copyright
Copyright © Reidel 1981

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