Abstract
AbstractWe model evolution of exoplanets of S-type in close binary systems at the stage when the companion starts to lose mass via a slow stellar wind. At this stage an accretion disc is formed around the planets’ host. Detailed structure of such discs is calculated in quasi-stationary and non-stationary approaches. We model migration of planets embedded in these discs.
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Schedule a callMore From: Proceedings of the International Astronomical Union. International Astronomical Union
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