Blue straggler stars in old open clusters exhibit a Kraft break in rotation, with rapid rotators above the break and slow rotators below, indicating their envelopes behave like those of single stars.
A case study of a binary mass-gainer in the SPB instability strip
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Blue straggler stars in old open clusters predominantly appear near the terminal-age main sequence because mass transfer from asymptotic giant branch donors enriches their cores with helium.
1D models show convective boundary mixing dominates the asteroseismic imprint of accretion in massive stars, robust to semiconvection changes but drastically altered without it, with thermal relaxation as key.
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