Abstract
The effects of accretion during core-hydrogen burning and during shell hydrogen burning at constant rates of 3e−3M0yr−1 and 3e−4M0yr−1 on twelve massive stars of 10M0 and 30M0, with and without stellar wind mass loss are examined. For each case relaxation series are computed after 14M0 and after 29M0 have been accreted. The accretion series with the slower rate are well able to adjust their structure almost instantaneously to the increasing mass. The series with the rapid accretion rate show severe overluminosity, having envelopes strongly deviating from thermal equilibrium. After relaxation they return to the normal positions of their corresponding slow accretion models. The process of semi-convection enables the Main-Sequence models to increase their convective core and their core-hydrogen content. The hydrogen shell-burning models increase their intermediate fully convective zone both in size and in hydrogen content.
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