Abstract
A simple model which can explain the large angular momentum loss that a star suffers in its post-main-sequence evolution is presented. The basic assumptions are that main-sequence stars and white dwarfs rotate as rigid bodies and that the mass loss between the two stages is due to stellar winds. The angular momentum loss, even without considering braking effects of magnetic fields, turns out to be very large, with a lower limit which varies from 99 per cent for a star which evolves into a 0.5 M ⊙ white dwarf to more than 99.99 per cent for a final mass higher than 1.1 M ⊙
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