Evolutionary models of red supergiants: Evidence for a metallicity-dependent mixing length and implications for Type IIP supernova progenitors

TL;DR

This study calibrates the mixing length parameter in red supergiant models across different metallicities, revealing a metallicity-dependent increase that impacts supernova progenitor characteristics and their observable properties.

Contribution

It provides the first evidence that the mixing length parameter in RSG models depends on metallicity, with implications for supernova progenitor modeling.

Findings

Mixing length increases with metallicity in RSGs.

Type IIP supernova progenitors have radii of 400-800 R_sun regardless of metallicity.

Hydrogen-rich envelope mass predictions vary with convection criteria and metallicity.

Abstract

Recent studies on the temperatures of red supergiants (RSGs) in the local universe provide us with an excellent observational constraint on RSG models. We calibrate the mixing length parameter by comparing model predictions with the empirical RSG temperatures in Small and Large Magellanic Clouds, Milky Way, and M31, which are inferred from the TiO band and the spectral energy distribution (SED). Although our RSG models are computed with the MESA code, our result may be applied to other stellar evolution codes, including the BEC and TWIN codes. We find evidence that the mixing length increases with increasing metallicity for both cases where the TiO and SED temperatures of RSGs are used for the calibration. Together with the recent finding of a similar correlation in low-mass red giants by Tayar et al, this implies that the metallicity dependence of the mixing length is a universal feature in post-main sequence stars of both low and high masses. Our result implies that typical Type IIP supernova (SN IIP) progenitors with initial masses of $\sim 10 - 16~M_\odot$ have a radius range of $400 R_\odot \lesssim R \lesssim 800 R_\odot$ regardless of metallicity. As an auxiliary result of this study, we find that the hydrogen-rich envelope mass of SN IIP progenitors for a given initial mass is predicted to be largely independent of metallicity if the Ledoux criterion with slow semiconvection is adopted, while the Schwarzschild models predict systematically more massive hydrogen-rich envelopes for lower metallicity.