Calibrating Convective properties of Solar-like Stars in the Kepler Field of View

TL;DR

This study uses Kepler data to calibrate the mixing-length parameter for convection in solar-like stars, revealing it varies with metallicity and differs from the solar value, impacting stellar modeling accuracy.

Contribution

It provides the first empirical calibration of the mixing-length parameter for a large sample of stars using Kepler data, showing its dependence on stellar properties.

Findings

The solar-calibrated  is often inappropriate for other stars.

The mixing-length parameter  is generally lower than the solar value.

 increases with stellar metallicity.

Abstract

Stellar models generally use simple parametrizations to treat convection. The most widely used parametrization is the so-called "Mixing Length Theory" where the convective eddy sizes are described using a single number, \alpha, the mixing-length parameter. This is a free parameter, and the general practice is to calibrate \alpha using the known properties of the Sun and apply that to all stars. Using data from NASA's Kepler mission we show that using the solar-calibrated \alpha is not always appropriate, and that in many cases it would lead to estimates of initial helium abundances that are lower than the primordial helium abundance. Kepler data allow us to calibrate \alpha for many other stars and we show that for the sample of stars we have studied, the mixing-length parameter is generally lower than the solar value. We studied the correlation between \alpha and stellar properties, and we find that \alpha increases with metallicity. We therefore conclude that results obtained by fitting stellar models or by using population-synthesis models constructed with solar values of \alpha are likely to have large systematic errors. Our results also confirm theoretical expectations that the mixing-length parameter should vary with stellar properties.