# Stellar models and isochrones from low-mass to massive stars including pre-main sequence phase with accretion

## TL;DR

This paper presents a comprehensive grid of stellar models from low-mass to massive stars, including the pre-main sequence phase with accretion, to better understand young stellar clusters across all evolutionary stages.

## Contribution

The authors develop the first extensive grid of stellar models covering from pre-MS with accretion to post-MS for a wide mass range, integrated with existing models for complete evolutionary coverage.

## Key findings

- Provides evolutionary tracks and isochrones for 0.8 to 120 solar masses.
- Connects pre-MS accretion models with existing MS and post-MS grids.
- Offers publicly available numerical tables of models and isochrones.

## Abstract

Grids of stellar models are useful tools to derive the properties of stellar clusters, in particular young clusters hosting massive stars, and to provide information on the star formation process in various mass ranges. Because of their short evolutionary timescale, massive stars end their life while their low-mass siblings are still on the pre-main sequence (pre-MS) phase. Thus the study of young clusters requires consistent consideration of all the phases of stellar evolution. But despite the large number of grids that are available in the literature, a grid accounting for the evolution from the pre-MS accretion phase to the post-MS phase in the whole stellar mass range is still lacking. We build a grid of stellar models at solar metallicity with masses from 0.8 $M_\odot$ to 120 $M_\odot$, including pre-MS phase with accretion. We use the {\sc genec} code to run stellar models on this mass range. The accretion law is chosen to match the observations of pre-MS objects on the Hertzsprung-Russell diagram. We describe the evolutionary tracks and isochrones of our models. The grid is connected to previous MS and post-MS grids computed with the same numerical method and physical assumptions, which provides the widest grid in mass and age to date. Numerical tables of our models and corresponding isochrones are available online.