DOI: 10.5281/zenodo.18307074
title: Relationship Between Major Stellar Physical Parameters and Normal Mode Frequencies in Accreting White Dwarf Stars

description: Kumar, Townsley & Anz (2026)Relationship Between Major Stellar Physical Parameters and Normal Mode Frequencies in Accreting White Dwarf StarsThis repository contains the relevant files and inlists that were used in the paper titled Relationship Between Major Stellar Physical Parameters and Normal Mode Frequencies in Accreting White Dwarf Stars“ Kumar, Townsley & Anz (2026).

The requirements are



MESA Release Version: 15140 (Paxton et al. 2011, 2013, 2015, 2018, 2019)

MESASDK Version: 21.4.1

Proper Environments, see MESA Documentation

GYRE Version: 7.0 (GYRE Documentation) (Townsend & Teitler (2013), Townsend et al. (2018))


The details of each step on MESA models and GYRE input/output are provide in readme.md.



There are six top-level directories in this repo: Cases, DwarfNovae, GyreData, ModelsBeforeAccretion, ModelsCooledWDs, and ModelsIgnitionWDs.

1) ModelsBeforeAccretion contains the initial cooled white dwarf (WD) models of five different WD masses: 0.6 Msun, 0.7 Msun, 0.78 Msun, 0.86 Msun, and 0.93 Msun. 0.78 Msun and 0.93 Msun models are taken from Kumar & Townsley (2023),and they are in the subfolders “0.78M” and “0.93M.” The 86 Msun WD model is evolved from the pms to a cooled WD with element diffusion enabled, and the files are located in “0.86M.”  0.6 Msun and 0.70 Msun WD models are rescaled from the final 0.78 Msun model and the files are located in “Mass_rescale_0.6M_0.7M.”

A) 0.78M: inlist_wd_cool: cools the initial WD model “wd_relax_100.mod” to Teff=15000 K; the final model is “wd_cool_0.78_ppcno.mod.”  wd_relax_100.mod is taken from Kumar & Townsley (2023).

B) 0.86M:inlist_pms_hot_wd: evolves to a hot WD with the leaving out of the hydrogen layer~1.62e-4 Msun and the corresponding model is “zams_hot_wd_0.000162.mod.”inlist_wd_relax: strips out the remaining outer envelope.inlist_wd_cool: cools this hot WD with element diffusion to Teff~15kK

C) 0.93:“wd_relax_mesa49.mod” is taken from Kumar & Townsley (2023), and this was evolved in Mesa r10398.inlist_wd_cool: cools the relaxed WD to Teff~15kK.

D) Mass_rescale_0.6M_0.7M:inlist_wd_relax: Rescales 0.78M (wd_cool_0.78_mesa49_1e6.mod) to 0.6Msun and 0.7Msun respectively, using relax_mass_scale.The relax models are “0.6M_wd_relax_mesa49.mod” and “0.7M_wd_relax_mesa49.mod” for 0.6Msun and 0.7Msun, respectively.

2) ModelsCooledWDs contains the cooled WD models. The inlist_wd_cool cools the initial WD models using pp_cno_extras_o18_ne22.net with element diffusion.A) 0.60M_cooled: The initial model “0.6M_wd_relax_mesa49.mod” is cooled to a core temperature (Tc) of 6e6K. The final model is “wd_cool_0.60_ppcno_6e6K.mod.”B) 0.70M_cooled: The initial model “0.7M_wd_relax_mesa49.mod” is cooled to Tc=6e6K. The final model is “wd_cool_0.70_ppcno_6e6K.mod.”C) 0.78M_cooled: The initial model “wd_cool_0.78_ppcno.mod” is then cooled to various Tc. The final models are wd_cool_0.78_ppcno_{1e7K, 9e6K, 8e6K, 7e6K, 6.5e6K, 6e6K, 5.5e6K, 5e6K}.mod for Tc = 1e7K, 9e6K, 8e6K, 7e6K, 6.5e6K, 6e6K, 5.5e6K, and 5e6K, respectively.D) 0.86M_cooled: The initial model “wd_cool_0.8618_ppcnp.mod” is cooled to Tc=6e6K. The final model is “wd_cool_0.8618_ppcno_6e6K.mod.”E) 0.93M_cooled: The initial model “wd_cool_0.93_ppcnp.mod” is cooled to Tc=6e6K. The final model is “wd_cool_0.93_ppcno_6e6K.mod.”

3) ModelsIgnitionWDs contains the long-term accretion process with element diffusion and evolves until the WD reaches its surface ignition. The choice is safely set at when log(LH/Lsun)~5. The general layout for each mass model is broken into three phases:i) inlist_pre_accretion: this uses the cooled WD model 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 element diffusion and thermohaline mixing. We evolve the WD until the surface is ignited, set at log(LH/Lsun)~5. This choice is explained in detail in the text of the paper. In short, we choose this due to MESA having difficulty in evolving the hydrogen flashes with diffusion and producing unrealistic profiles. The final model is noted with “accretion_to_ignpoint.mod” for 0.6, 0.7, 0.86, and 0.93 Msun models for Tc=6e6K. The 0.78 Msun model has seven different ignition model at various Tc (5e6K,..,9e6K). The “accretion_to_logLH2.mod” is when log(LH/Lsun)~2. The sub directories’ names have usual meaning.

4) Cases contain the WD evolution during the long-term accretion process for three different case models: core temperature, accreted thickness layer, and WD mass.i) a_CoreTemp contains files for the evolution of accretion processes for Tc=5, 5.5, 6, 6.5, and 7e6K of the 0.78 Msun WD model. The accretion process is explained above (3). All models have the same final surface temperature (Teff) of 14000K and the same accreted layer of 1.5e-4Msun. The crystallization condition is taken at gamma = 175.ii) b_AccretedLayer contains files for various accretion rates, resulting in different accreted thickness layer with a final Teff = 14000K of a Tc=5e6 K, 0.78 Msun model. The accretion rates (also used for sub-dir names) are 8, 8.2, 8.4, 8.6, 8.8, 9, 10, 10.5, 11, 11.5, 12, 13, and 14e-11 Msun/year.  ./rn is the execution script. iii) c_WdMass contains the files for WD masses of 0.6, 0.7, 0.78, 0.86, and 0.93 Msun with final Teff=14000K. The core temperature of all models is 6e6K. We find the right accretion rate to achieve Teff=14000K. With the suitable accretion rate and the same Teff, the accreted thickness layers are different for different WD masses. The higher mass model (0.93 Msun) has the lowest accreted thickness layer.

5) DwarfNovae contains the inlist files used for the strong-short accretion event, namely the dwarf nova phase. Overall, there are two 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 phases are 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 long accretion. “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.

The step files are copied to “inlist_current_step,” see “runall_new” for the full execution orders.0.60M, 0.70M, 0.86M, and 0.93M have files that only do three and six months post the outburst (after step_accrete2) for Tc=6e6K. The final profiles for GYRE input are “final_profile_6e6K_3ma.data.GYRE” and “final_profile_6e6K_6ma.data.GYRE” for three and six months post dwarf novae, located in directories “./6e6K/3months_after_burst” and  “./6e6K/6months_after_burst” for each mass model for point 4-iii, as mentioned above.0.78M have inlist files for various Tc (point 4-i) at 5e6K, 6e6K, 6,5e6K, and 7e6K: i) 5e6K/7e6K: “3months_after_burst” contains the inlist files for the dwarf nova phase. The final GYRE input files are noted with “final_profile_5e6K/7e6K_3ma.data.GYRE.”  For different burst model at various times are “final_profile_5e6K/7e6K_{-9,-6,-1, -0, 0, 1, 3, 6, 9, 12, 18, 24, 48, 120}ma.data.GYRE”. The negative numbers indicate months before the outburst, and -0 and 0 are just before and just after the outburst, respectively.ii) 6e6K/6.5e6K: The final model for the GYRE input is “final_profile_6e6K/6.5e6K_3ma/6ma.data.GYRE” for three and six months post the dwarf novae.

For point 4-iii: the dwarf nova files are in “6e6K_twothird” of the 0.78M model with accreted thickness layer 1.89e-4Msun.

For point 4-ii: the dwarf nova final GYRE input files are located in “3months_after_burst” and 6months_after_burst” for the dwarf nova phase executed for different accreted layer models presented in point 4-ii. 

6) GyreData contains GYRE input files and output files for three cases defined in point 4 above. Within this there are four subdirectories: “modes_core_temperatures,” “modes_dwarfnovae,” “modes_masses,” and “modes_with_acclayer_5e6K_0.78M.” 

i) modes_core_temperatures: 0.78 Model: 5e6_Tc, 5.5e6_Tc, 6e6_Tc, 6.5e6_Tc, and 7e6_Tc contain the gyre input “gyre_time.in” and their corresponding eigenfunctions and eigenfrequencies in “datafile.” The  g-modes are evaluated after the long-term accretion phase for each Tc model.ii) modes_dwarfnovae: g-modes are evaluated for each model post dwarf novae.0.6M: 6e6K_2.55e-4Msun: gyre_time is copied to final gyre input file “gyre_time.in” for three and six months post outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.60M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.70M: 6e6K_2.08e-4Msun: gyre_time is copied to the final gyre input file “gyre_time.in” for three- and six- month post-outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.70M_3/6.txt” for three and six months, respectively. The “final_profile_6e6K_3ma/6ma.data.GYRE” is the GYRE input for 3/6 months post dwarf nova phase.

0.86M: 6e6K_1.38e-4Msun: gyre_time is copied to the final gyre input file “gyre_time.in” for three and six-months- post outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.86M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.93M: 6e6K_1.01e-4Msun: gyre_time is copied to the final gyre input file “gyre_time.in” for three and six- month post outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.93M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.78M: 6e6K_1.89e-4Msun:  gyre_time is copied to the final gyre input file “gyre_time.in” for three- and six- month post-outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.78M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.78M: 5e6K_1.5e-4Msun: The .GYRE files are the initial GYRE input files taken post dwarf nova phase  for Tc = 5e6K. The negative and positive number at the end of filename indicate before and after the dwarf nova. gyre_time and gyre_time.in are working gyre working file. The ./rn does the execution process. The corresponding summary file is located in “/datafile.”

0.78M: 6e6K_1.5e-4Msun:  gyre_time is copied to the final gyre input file “gyre_time.in” for three- and six- month post-outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6e6K_0.78M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.78M: 6.5e6K_1.5e-4Msun:  gyre_time is copied to final gyre input file “gyre_time.in” for three and six-month post outbursts mode calculations. The calculated modes are located in “datafile/summary_ad_rot_gmode_6.5e6K_0.78M_3/6.txt” for three and six months, respectively. The .GYRE is the GYRE input file.

0.78M: 7e6K_1.5e-4Msun: The .GYRE files are the initial GYRE input files taken post dwarf nova phase  for Tc = 7e6K. The negative and positive numbers at the end of filenames indicate before and after the dwarf nova. gyre_time and gyre_time.in are working gyre working file. The ./rn does the execution process. The corresponding summary file is located in “/datafile.”

iii) modes_masses: g-modes evaluated after the long-term accretion event for the 0.6, 0.7, 0.78, 0.86, and 0.93 Msun model at Tc=6e6K. The queuescript_gmode.sh does the main execution. gyre_gmode_crystalcore and gyre_gmode_nocrystalcore are the temporary files for the solid and non-solid core WD mass models, which are processed to gyre_diff_mass_6e6K.in. The summary files are located in “/datafile.” Modes without Cowling approximation are in the sub-folder “/without_Cowling.”

iv) modes_with_acclayer_5e6K_0.78M: g-modes evaluated following the long-term accretion process for various accreted thickness layers. The queuescript_gmode.sh does the main execution. gyre_acclayer.in is the gyre input file. The summary files are indicated with “summary_ad_rot_gmode_5e6K_0.78M_{…}.txt” for different accretion rates.