DOI: 10.5281/zenodo.13936543
title: MESA (r11701) models with convective turnover times

description: $\texttt{MESA r11701}$ (Paxton et al. 2019) stellar models in the range 0.08 - 1.3 $\rm M_{\odot}$ with a metallicity of $\rm Z_{\odot}$ (as according to Asplund et al. 2009) and no rotation. These models are part of a study on convective turnover times submitted to ApJ and available to read on arXiv here: Gossage et al. 2024.

 



$\texttt{MESA r11701}$ may be downloaded here: https://zenodo.org/records/2665077

The associated $\texttt{MESA SDK}$ may be found here: old release archive (compiled under $\texttt{GCC version 8.3.0}$)


 

Models and inlists

The compressed archive files $\texttt{MESA_run_directories_to_XGyr.tar.gz}$ contain run directories for our models evolved up to $\texttt{X}$ Gyrs (1, 5, or 14). Each directory within has a name corresponding to the model's initial mass (e.g., with $\texttt{00101M_dir}$ corresponding to a 1.01 $\rm M_{\odot}$ model) and contains the inlist (called $\texttt{inlist_project}$) used for that run. Each directory contains a subdirectory called $\texttt{LOGS}$ that contains the run's output (stellar profiles and histories in this case). The stellar profiles are available at approximately 1 Myr, 1 Gyr, 5 Gyr and 14 Gyr, when possible. Every $\texttt{LOGS}$ directory should contain a $\texttt{final_profile.data}$ file which is the stellar profile at the final simulation step of that run. These models were produced to study the variation of the convective turnover time, according to mixing length theory (as according to Henyey et al. 1965) in 1D stellar evolution.

In the history files, the convective turnover times provided are (in units of seconds):



$\texttt{conv_env_turnover_time_l_hp}$, calculated one half of a (local) pressure scale height from the bottom of the convection zone (BCZ), or core in fully convective stars. This calculation corresponds to the values cited in Gossage et al. 2024.

$\texttt{conv_env_turnover_time_l_hp_mid}$ at one pressure scale height from the BCZ

$\texttt{conv_env_turnover_time_l_hp_hi}$ at two pressure scale heights from the BCZ

$\texttt{conv_env_turnover_time_l_hp_hi2}$ at four pressure scale heights from the BCZ

$\texttt{conv_env_turnover_time_l_hp_hi3}$ at eight pressure scale heights from the BCZ

$\texttt{conv_env_turnover_time_l_b}$ at half pressure scale height from the BCZ, as calculated and adopted in Giliand et al. 1985

$\texttt{conv_env_turnover_time_l_t}$ at one pressure scale height from the BCZ (calculated in same manner as Giliand et al. 1985)

$\texttt{conv_env_turnover_time_g}$ a "global" convective turnover time, calculated as a running sum of local distances divided by convective velocities (computed cell-wise)  through the outer convection zone of the model


The quantities 1-5 above are scaled by the $\texttt{inlist}$ parameter $\texttt{x_ctrl(15)}$, which is set to 0.5 by default.

$\texttt{MESA src (run_star_extras.f90)}$ and other files 

Our $\texttt{run_star_extras.f90}$ file is provided as well. Several additional files may be needed, such as reaction networks (these are as in $\texttt{MIST v1.0}$, Choi et al. 2016) that may be downloaded here: https://waps.cfa.harvard.edu/MIST/resources.html. Our $\texttt{run_star_extras.f90}$ file is also based on that used in the $\texttt{MIST v1.0}$ models, but with some additions. 

Observational Data

The compiled observational data used in our study is recorded in literature_sample.csv. This data is comprised of observations from several sources:



Stassun & Kounkel 2024

Wright et al. 2011

Nunez et al. 2022

Shan et al. 2024

Pizzocaro et al. 2019

Magaudda et al. 2022

Gondoin 2012

Wright et al. 2018

Gondoin 2013

Wright & Drake 2016


The csv contains the cross-match with Gaia DR3 (Gaia Collaboration et al. 2016; Gaia Collaboration et al. 2023), and we removed duplicated sources which had the same X-ray measurement.