authors: Mathieu Renzo, Ylva Goetberg
Code for reproducing the numerical results of arXiv:2107.10933, accepted by the Astrophysical Journal.
We used MESA version r15140 with the MESA SDK x86_64-linux-20.12.1.
The data produced are available at https://doi.org/10.5281/zenodo.4701565.
The setup for our binary evolution runs, until the
post-mass-transfer detachment is in
MESA_setup/binary_to_postRLOF
. This is a MESA work directory for a
binary system. To use it you need to change MASS1
, MASS2
, and
PERIOD
to the appropriate values in
MESA_setup/binary_to_postRLOF/inlist_binary
, and METALLICITY
in
MESA_setup/binary_to_postRLOF/inlist_both
.
We restart the evolution of the accretor from a model saved in the
binary run. The MESA work directory MESA_setup/accretor_to_TAMS
is
used for this purpose. You need to modify
MESA_setup/accretor_to_TAMS/inlist_extra
to point it to the
location of the MESA model (*.mod
file) saved at the end of the
binary run by modifying saved_model_name
, and modify ZBASE
to be the initial metallicity of the model.
The single star models are produced with the
MESA_setup/single_rotating_stars
work directory. You need to set
explicitly the initial ω/ωcrit and mass wanted in inlist_extra
.
Inside notebooks/
you can find the scripts to reproduce the
numerical analysis of our models and the figures. Many auxiliary
functions are defined in plot_aux.py
, and the notebooks also rely
on https://github.com/mathren90/plotFunc. The other dependencies
are listed in pyproject.toml
. You will need to download the
simulation output from https://doi.org/10.5281/zenodo.4701565 and
modify some strings (typically starting with /mnt/home/mrenzo/
) to
match the location of these files to run the scripts.
The code to reproduce Fig. 1 and 2 is in
notebooks/Best_model.ipynb
.
The code to reproduce Fig. 3-7 and 9-11 is in notebooks/mixing_and_AM.ipynb
.
The code to reproduce Fig. 8 and the resolution tests is in notebook/resolution_test.ipynb
.
The code to create Table 1 is in notebooks/table.ipynb
.
Contains the Gaia DR3 data for ζ Ophiuchi. These are unfortunately not usable (large RUWE).
The bulk of the simulation data is publicly available at https://doi.org/10.5281/zenodo.4701565
Contains the movies of the mixing processes and chemical
composition of our accretor models. The frames for these movies are
created using the ipython notebook notebooks/mixing_and_AM.ipynb
.
This folder is probably not interesting to you. It contains the tex
file and other auxiliary files for the paper associated to this
repository. Unlike the rest of the repository, licensed with GPLv3,
that subfolder is licensed with CC BY-NC-ND 3.0.