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- W1660632007 abstract "We present the results of population number synthe- sis calculations on young starbursts in regions of solar metal- licity (Z=0.02), using a Monte Carlo simulation of bursts con- taining 1000 stellar objects. They clearly show that one has to account for interacting binaries to get a correct image of these regions. Independently of all sorts of distributions such as initial mass function (IMF) or mass ratio distribution, interact- ing binary evolution makes starbursts look younger than they really are. What happens is that after some time, the area of the main sequence (MS) above the actual turnoff point of the Hertzsprung-Russell Diagram (HRD) gets crowded with accre- tion stars, which are part of the end product of mass transfer in close binaries. Shortly after their appearance, these accretion stars (blue Stragglers) begin to dominate the O star population in a starburst, proceeding to the moment where they are the only ones left (since at that particular stage, all the O type single stars and binary O type primaries have disappeared). As a con- sequence, if it is assumed that the entire population are single stars, or that the features of the starburst are solely due to sin- gle star evolution, the resulting age estimation of the starburst is wrong, i.e. the starburst may be considerably older than it appears." @default.
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- W1660632007 date "1998-06-01" @default.
- W1660632007 modified "2023-09-26" @default.
- W1660632007 title "The rejuvenation of starburst regions due to massive close binary evolution" @default.
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