Unified gravity mode and Rossby mode Analysis of Accreting White Dwarf Stars

This repository contains the files and related work directories used in the preparation of the paper "Unified g-mode and r-mode Analysis of Accreting White Dwarf Stars." This has mesa models including the inlists and the gyre input files. The cooled WD model is taken from "Gravity Modes on Rapidly Rotating Accreting White Dwarfs and Their Variation after Dwarf Novae." The requirements are MESA version: 15140 MESASDK version: 21.4.1 Proper environments, see MESA Documentation GYRE version: 7.0 (GYRE Documentation) The details of the steps on MESA models and GYRE input/output are provided in README.txt. Some of the files are modified from v1. This repository contains the inlists and model outputs for a 0.78 Msun WD model used in ``Kumar \& Townsley (2025).``It includes files for the white dwarf (WD) cooling phase,accretion history, short-term accretion events (dwarf novae), and gyreinput/output files used for the seismological calculations. There are fourdirectories: ``0Cool_WD_5e6K,`` ``1WD_Accretion_0.78Msun,`` ``2Dwarf_Novae,`` and ``3Gyre_Data.``0Cool_WD_5e6K: This does the initial cooling phase of the WD. The initial WD model is taken from the ``Kumar \& Townsley (2023)`` with the core temperature of ~ 1.26e7 K (``wd_cool_basic_network_0.785.mod``). The ``initial_setup`` cools the WD to 5e6 K using the ``basic network``. At this core temperature the WD is approximately 8.4 % solid in radius at ``$\Gamma=213$``. This crystallization condition is chosen based on ``Blouin et al. 2021.``The final WD model is ``cooled_wd_5e6K_0.78M_revised.mod``.1WD_Accretion_0.78Msun:A) inlist_pre_accretion: this uses the cooled WD model ``cooled_wd_5e6K_0.78M_revised.mod``and runs for another 1e5 years without any accretion and diffusion but with ``pp_cno_extras_o18_ne22.net``. Thisproduces the output model ``pre_acc_pre_diff_1e5.mod.`` B) inlist_pre_diff: this is the second step of the accretion evolution, where the WD evolves for another 1e5 years with accretion but without diffusion. We also turn off the mixing(mix_factor = 0) to avoid any residual burning to start the accretion process.This produces the ``acc_pre_diff_2e5.mod.``C) inlist_accretion: this is the REAL accretion process with elementdiffusion and thermohaline mixing. We evolvethe WD about two-thirds of the first outburst time (hydrogen flash). This choiceis explained in detail in the text of the paper. In short, we choose this due toMESA having difficulty in evolving the hydrogen flashes with diffusion andproducing unrealistic profiles. To unravel the WD seismological knowledge, weuse this condition, which has relatively physical interiors in the WD,especially the buoyancy profile. The final output of this phase is``outburst_two_third_revised.mod`` and will be the starting model for the dwarf nova cycle.2Dwarf_novae: This directory contains the inlist files used for thestrong-short accretion event, namely the dwarf nova phase. Overall, there aretwo phases in this cycle: a short accretion event for two months (step_accrete*)and the recurrent cooling phase for 30 years (step_rest*). The separate phasesare worked with a common ``inlist_cvteff_postoutburst.`` ``step_rest0`` is the first cooling phase of the WD for 30 years post the two-thirds of the longaccretion. ``step_accrete0`` is the first strong accretion event lasting for two months. ``step_rest1`` is the second cooling phase of the WD lasting for 30 years. ``step_accrete1`` is the second strong accretion event lasting for two months. ``step_rest2`` is the third cooling phase of the WD lasting for 30 years.``step_accrete2`` is the third strong accretion event lasting for two months.``step_rest3`` is the fourth cooling phase of the WD lasting for 30 years. Theseismology is conducted on the past three months past during this phase. Thefinal GYRE output is 'final_profile_3ma.data.GYRE.' The step files are copied to ``inlist_current_step,`` see ``runall_new`` for the full execution orders.3Gyre_Data: This folder contains the gyre input files for both gravity ($g$) and Rossby ($r$) modes calculations. There are three subfolders init: ``gmode-prograde``, ``gmode-retrograde``, and ``rmode.`` A) ``gmode-prograde``contains the gyre inputfile ``gyre_time.in`` and temporary file ``gyre_time_g_modes.`` The ``queuescript.sh``carries out the gyre execution. The ``final_profile_3m.data.GYRE`` is the gyreinput file, extracted from MESA. The gyre summary output file is ``gmode_pro_summary_ad_rot_3_revise.txt.``B) ``gmode-retrograde`` contains the gyre input file ``gyre_time.in`` and the temporary file ``gyre_time_g_modes.``C) ``rmode`` contains the gyre input file ``gyre_time.in`` and temporary file ``gyre_time.`` The queuescript.sh carries out the gyre execution. The 'final_profile_3m.data.GYRE'is the gyre input file. The gyre summary output file is ``rmode_summary_ad_rot_revise_3.txt`` and the detail files are located in ``burst_after_rmode_corot_3.``