A discontinuity in the luminosity-mass relation and fluctuations in the evolutionary tracks of low-mass and low-metallicity stars at the Gaia M-dwarf gap (vol 650, 184, 2021)
2022
Abstrakt
The initial helium abundance used in the models was Y = 0.28 and not the stated metallicity-dependent value of Y = 0.24 + 2Z. The mass ranges for models that undergo the convective kissing instability with this initial helium abundance are: 0.33000 M <= m <= 0.37100 M for Z = 0.01, 0.34300 M <= m <= 0.36900 M for Z = 0.001, and 0.35600 M <= m <= 0.39033 M for Z = 0.0001.
All conclusions remain accurate except that the instability here occurs at a higher mass range for lower metallicity.