New photometry of M10 revises its distance to 5.0 to 5.35 kpc, suggests an age of about 13 Gyr, and models its horizontal branch with a 0.56 to 0.62 solar mass range that hints at variable RGB mass loss.
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Observational analysis of 21 giant stars shows Fe I+Fe II blend emission proportional to Ca II K with matching Teff power-law exponent and a slope break in the flux ratio at log g ≈ 2.5.
MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.
citing papers explorer
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The globular cluster M10: Reassessment of stellar membership, distance and age using its variable and HB stars
New photometry of M10 revises its distance to 5.0 to 5.35 kpc, suggests an age of about 13 Gyr, and models its horizontal branch with a 0.56 to 0.62 solar mass range that hints at variable RGB mass loss.
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On the stellar parameter dependence of the combined Fe I and Fe II chromospheric emission-line in the wings of the Ca II K line
Observational analysis of 21 giant stars shows Fe I+Fe II blend emission proportional to Ca II K with matching Teff power-law exponent and a slope break in the flux ratio at log g ≈ 2.5.
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Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars
MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.