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
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
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astro-ph.SR 4years
2026 4representative citing papers
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.
citing papers explorer
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Blue Straggler Stars in Old Open Clusters and the Kraft Break
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.
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The Distribution of Blue Straggler Stars in the Color-Magnitude Diagrams of Old Open Clusters
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.
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The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors
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.