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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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.
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
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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Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.