2010MNRAS.402.1072P -
Mon. Not. R. Astron. Soc., 402, 1072-1080 (2010/February-3)
Magnetic field evolution of white dwarfs in strongly interacting binary star systems.
POTTER A.T. and TOUT C.A.
Abstract (from CDS):
The surface magnetic field strength of white dwarfs is observed to vary from very little to around 109G. Here, we examine the proposal that the strongest fields are generated by dynamo action during the common envelope phase of strongly interacting stars that leads to binary systems containing at least one white dwarf. The resulting magnetic field depends strongly on the electrical conductivity of the white dwarf, the lifetime of the convective envelope and the variability of the magnetic dynamo. We assess the various energy sources available and estimate necessary lifetimes of the common envelope. In the case of a dynamo that leads a randomly oriented magnetic field, we find that the induced field is confined to a thin boundary layer at the surface of the white dwarf. This then decays away rapidly upon dispersal of the common envelope. The residual field is typically less than 10–8 times the strength of the external field. Only in the case where there is some preferential direction to the dynamo-generated field can an induced field, which avoids rapid decay, be produced. We show that a surface field of a magnitude a fewper cent of the external field may be produced after a few Myr. In this case, the residual field strength is roughly proportional to the lifetime of the dynamo activity.
Abstract Copyright:
© 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s):
binaries: close - stars: evolution - stars: magnetic fields - white dwarfs
Simbad objects:
3
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