Evolutionary models for solar metallicity low-mass stars: mass-magnitude relationships and color-magnitude diagrams

TL;DR

This paper develops and validates evolutionary models for low-mass stars with solar metallicity, providing accurate mass-magnitude and color-magnitude relationships, and compares them with observational data from star clusters and field stars.

Contribution

It introduces updated low-mass star models incorporating recent physics and atmosphere models, improving reliability in near-infrared predictions and offering new calibration tools.

Findings

Mass-M$_V$ and mass-M$_K$ relations agree with observations.

Theoretical color-magnitude diagrams match well with cluster data.

Models are reliable in near-infrared but have optical discrepancies below 3700K.

Abstract

We present evolutionary models for low mass stars from 0.075 to 1 $\msol$ for solar-type metallicities [M/H]= 0 and -0.5. The calculations include the most recent interior physics and the latest generation of non-grey atmosphere models. We provide mass-age-color-magnitude relationships for both metallicities. The mass-M$_V$ and mass-M$_K$ relations are in excellent agreement with the empirical relations derived observationally. The theoretical color-magnitude diagrams are compared with the sequences of globular clusters (47 Tucanae) and open clusters (NGC2420 and NGC2477) observed with the Hubble Space Telescope. Comparison is also made with field star sequences in $M_V$-$(V-I)$, $M_K$-$(I-K)$ and $M_K$-$(J-K)$ diagrams. These comparisons show that the most recent improvements performed in low-mass star atmosphere models yield now reliable stellar models in the near-infrared. These models can be used for metallicity, mass, temperature and luminosity calibrations. Uncertainties still remain, however, in the optical spectral region below $T_{eff} \sim 3700K$, where predicted (V-I) colors are too blue by 0.5 mag for a given magnitude. The possible origins for such a discrepancy, most likely a missing source of opacity in the optical and the onset of grain formation are examined in detail.