A new deepening of mass-radius empirical relation for main sequence stars

TL;DR

This paper compares existing mass-radius relations for main sequence stars with DEBCat data, finds the best agreement with Zamorano's model, and proposes a new empirical relation based on a two-piece power-law fit.

Contribution

It introduces a new empirical mass-radius relation for main sequence stars using DEBCat data and evaluates existing models' accuracy.

Findings

Zamorano's model shows the best agreement with DEBCat data.

A new two-piece power-law relation is proposed for main sequence stars.

The study highlights differences in energy transport behaviors across stellar masses.

Abstract

In the following paper I have compared some typical mass-radius relations for main sequence stars by studying their level of agreement with DEBCat [https://doi.org/10.48550/arXiv.1411.1219], which is a recent catalogue by J. Southworth. Models chosen for testing were originally developed using older, smaller datasets than DEBCat. Each model follows a two-piece function structure, where each branch is a monomial power-law. This approach is motivated by theoretical considerations suggesting that low-mass and high-mass main sequence stars exhibit distinct behaviors in energy production and energy transport. Best level of agreement is found for Zamorano's model [https://doi.org/10.1007/bf00653969]. Also a new empirical relation is proposed by fitting a two-piece monomial power-law to DEBCat main sequence stars.