Hot subdwarfs' models with rotation, internal magnetic fields and accretion

Hot subdwarfs' models with rotation, internal magnetic fields and accretion: Companion data and code repository for: Asteroseismic rotation rates of hot subdwarf B stars hint at transient accretion from leftover common envelope matter (Moyano et al. 2026, MNRAS) Authors: Facundo D. Moyano, Hongwei Ge, Zhanwen Han, Beatriz Bordadágua, Murat Uzundag, Philipp Podsiadlowski, Veronika chaffenroth, Xuefei Chen, Zhengwei Liu Corresponding author: Facundo D. Moyano (moyanofacu at hotmail . com) Overview This repository contains stellar evolutionary tracks of rotating hot subdwarfs including internal magnetic fields and accretion. All the models were computed with MESA (version 24.08.1, SDK version x86_64-linux-24.7.1, all computations were made in CentOS Linux release 7.4.1708). The needed initial parameters' files and software modifications necessary to reproduce our results are provided as well. In addition, we provide the stellar evolutionary tracks of models evolved from the zero age main sequence until the tip of the red giant branch used to construct our rotating hot subdwarf models. These models include rotation and internal magnetic fields, and are tailored to reproduce asteroseismic rotation rates of red giant branch stars. Repository structure Hot subdwarfs models: The sdB models are provided in different folders depending on whether they include accretion and whether the accretion was included until the core (or envelope) spins up to a given rotation rate given in nanoHertz. These are specified by the keyword "core" or "env" and the number next to it. For example, the file "sdb_accretion_env200.tar.gz" contains sdB models where the envelope is spun up to 200 nHz by accretion whereas the file "sdb.tar.gz" contains sdB models without accretion. The individual folders containing the sdB models are named depending on the properties of their progenitors and the hydrogen-rich envelope mass of the sdB. For the properties of the progenitor, the folders are named according to the initial mass at the ZAMS, and their initial rotation period (in days) or rate (in microHertz) also at the ZAMS. The hydrogen-rich envelope mass is given in Msun for each model. For example: M12_5d_menv5e-4/ : initial ZAMS mass of 1.2 Msun and initial rotation period of 5 days. The sdB model has a hydrogen-rich envelope mass of 5 x 10^-4 Msun. M16_10muhz_menv1e-3/ : initial ZAMS mass of 1.6 Msun and initial rotation rate of 10 microHertz. The sdB model has a hydrogen-rich envelope mass of 1 x 10^-3 Msun. In addition to the standard columns provided by MESA, the following columns are given: nu_max: Frequency of maximum oscillation power [muhz]om_g: Mean core angular velocity as sensed by g-modes [rad/s]om_p: Mean envelope angular velocity as sensed by p-modes [rad/s]delta_nu: Large frequency separation [muhz]delta_pi1: Period spacing of g-modes [s]mixmod_freq: Mixed mode densityomegadotmag: Rate of angular velocity decrease by magnetised winds [rad/s^2]total_mass_h: Total mass of hydrogen [Msun]macc: Mass accreted [Msun] (only in sdB models with accretion) Among these, the only relevant ones for sdB models are om_g, om_p, delta_pi1, total_mass_h, and macc (only for sdB models with accretion) ZAMS to RGB tip models: are provided in the file "zamstorgb.tar.gz", which contains stellar evolutionary tracks of models evolved with rotation and internal magnetic fields from the ZAMS until the RGB tip. Each folder is named according to their mass and initial rotation as explained above. Inputs and software needed to recompute models: The file source.tar.gz contains the necessary input files to recompute the models presented in the work, from the ZAMS until the sdB phase including both rotation and internal magnetic fields (and optionally accretion). Each folder within this file contains the specific files with the input parameters and the necessary software modifications to account for internal magnetic fields and accretion. All files are already configured to compute a model with Mzams= 1 Msun, initial rotation period Prot,zams=1 day, and an sdB model with a hydrogen-rich envelope mass Menv=10^-3 Msun. Each specific folder contains: run_sdb_accretion: input files needed to run sdB models with accretion run_sdb_deg: input files needed to run sdB models from the RGB tip for sdB's whose progenitors ignite helium in degenerate conditions run_sdb_nondeg: input files needed to run sdB models from the RGB tip for sdB's whose progenitors ignite helium in non-degenerate conditions run_zamstorgb: input files needed to run models from the ZAMS to the RGB tip. The resulting RGB tip models are then used then to construct the sdB models In addition to the standard input parameters to change the initial mass and the initial angular velocity of the model provided by MESA by default, the parameter x_ctrl(9) in the file run_sdb_deg/inlist_postcee_presdb or run_sdb_nondeg/inlist_cee should be changed to compute sdB models with different envelope masses, by default it is set to 10^-3 Msun and reads as shown below: x_ctrl(9) = 1d-3 ! target hydrogen-rich envelope mass [Msun] To compute sdB models whose rotation is affected by accretion the target rotation rate can be modified in the source files, namely in the function extras_check_model through the variables omp_target or omg_target. To compute the whole evolution from ZAMS to the sdB phase the models should be computed in the following order: From the ZAMS until the RGB tip. Use the files provided in the folder run_zamstorgb. If needed change the initial parameters in inlist_msrgb. From the RGB tip until the sdB phase: use the files in the folders run_sdb_deg or run_sdb_nondeg depending on whether the RGB models ignite helium in degenerate or non-degenerate conditions. In the degenerate case, use the inlists in the order: inlist_cee: this will remove the outer hydrogen-rich envelope until it has only 10^-2 Msun and save a model for the next step inlist_postcee_presdb: this will load the model produced by inlist_cee and continue the evolution with smaller mass-loss rates until the core-helium ignition. To compute models with different hydrogen-rich envelope masses, the parameter x_ctrl(9) can be modified at this step so the first step (inlist_cee) does not have to be repeated for each model with similar initial conditions. inlist_sdb: this will load the model produced by inlist_postcee_presdb and compute the core-helium burning phase of the sdB model. It will stop once the central helium mass fraction drops below 10^-6 in mass fraction. For models with non-degenerate helium ignition, the second step is skipped and the hydrogen-rich envelope mass can be modified in inlist_cee. To compute sdB models with accretion, use the files given in the folder run_sdb_accretion, for which you will need the zero-age sdB model, which can be computed following the previously mentioned steps. If you have any questions or additional requests please only contact the corresponding author (Facundo D. Moyano).带自转、内部磁场与吸积过程的热亚矮星模型： 配套数据与代码仓库对应论文： 《热亚矮星B的星震学自转速率暗示来自残留共包层物质的暂态吸积》（Moyano等，2026，《皇家天文学会月报》（MNRAS）） 作者：Facundo D. Moyano、葛宏伟（Hongwei Ge）、韩占文（Zhanwen Han）、Beatriz Bordadágua、Murat Uzundag、Philipp Podsiadlowski、Veronika Chaffenroth、陈雪飞（Xuefei Chen）、刘正伟（Zhengwei Liu） 通讯作者：Facundo D. Moyano（邮箱：[e-mail]） 概述 本仓库包含带自转、内部磁场与吸积过程的热亚矮星的恒星演化轨道。所有模型均采用MESA（恒星天体物理实验模块，Modules for Experiments in Stellar Astrophysics，版本24.08.1，SDK版本x86_64-linux-24.7.1）计算完成，计算环境为CentOS Linux release 7.4.1708。本仓库同时提供复现本文结果所需的初始参数文件与软件修改脚本。 此外，本仓库还提供了从零年龄主序（Zero Age Main Sequence, ZAMS）演化至红巨星支端（Red Giant Branch Tip, RGB tip）的恒星演化轨道，用于构建本文的自转热亚矮星模型。此类模型包含自转与内部磁场，专门用于复现红巨星支星的星震学自转速率。 仓库结构 热亚矮星模型： 本仓库按是否包含吸积过程、以及吸积是否持续至恒星核心（或包层）自转至给定纳赫兹（nanoHertz, nHz）自转速率，将热亚矮星B（sdB）模型置于不同文件夹中。文件夹命名由关键词"core"或"env"加后续数字构成。例如，文件"sdb_accretion_env200.tar.gz"包含通过吸积将包层自转加速至200 nHz的sdB模型，而文件"sdb.tar.gz"则包含无吸积过程的sdB模型。 存储sdB模型的单个文件夹名称由其前身星性质与sdB的富氢包层质量决定。前身星性质方面，文件夹名称依据其在ZAMS处的初始质量、以及ZAMS处的初始自转周期（单位：天）或自转速率（单位：微赫兹（microHertz, μHz））命名。每个模型的富氢包层质量以太阳质量（Msun）为单位给出。 示例如下： M12_5d_menv5e-4/：ZAMS处初始质量为1.2 Msun，初始自转周期为5天，对应的sdB模型富氢包层质量为5×10^-4 Msun。 M16_10muhz_menv1e-3/：ZAMS处初始质量为1.6 Msun，初始自转速率为10 μHz，对应的sdB模型富氢包层质量为1×10^-3 Msun。 除MESA标准输出列外，本仓库还提供以下额外列： nu_max：振荡功率峰值频率，单位：μHz om_g：通过g模式探测得到的核心平均角速度，单位：rad/s om_p：通过p模式探测得到的包层平均角速度，单位：rad/s delta_nu：大频率间隔，单位：μHz delta_pi1：g模式的周期间距，单位：秒（s） mixmod_freq：混合模式密度 omegadotmag：磁场风导致的角速度衰减速率，单位：rad/s² total_mass_h：氢总质量，单位：Msun macc：吸积质量，单位：Msun（仅在含吸积过程的sdB模型中提供） 其中，与sdB模型相关的有效参数仅包括om_g、om_p、delta_pi1、total_mass_h以及macc（仅含吸积过程的sdB模型提供）。 ZAMS至RGB tip模型：存储于文件"zamstorgb.tar.gz"中，该文件包含从ZAMS演化至RGB tip、且包含自转与内部磁场的恒星演化轨道。单个文件夹名称按前文所述的质量与初始自转规则命名。 复现模型所需的输入文件与软件： 文件source.tar.gz包含复现本文模型所需的全部输入文件，覆盖从ZAMS至sdB阶段的演化过程，包含自转与内部磁场（可选吸积过程）。该文件内的每个子文件夹均包含对应参数的输入文件与适配内部磁场与吸积过程的软件修改脚本。所有文件默认配置为：ZAMS处初始质量Mzams=1 Msun，初始自转周期Prot,zams=1天，最终生成的sdB模型富氢包层质量Menv=10^-3 Msun。每个子文件夹包含以下内容： run_sdb_accretion：运行含吸积过程的sdB模型所需的输入文件 run_sdb_deg：针对前身星在简并条件下点燃氦的sdB模型，运行从RGB tip至sdB阶段所需的输入文件 run_sdb_nondeg：针对前身星在非简并条件下点燃氦的sdB模型，运行从RGB tip至sdB阶段所需的输入文件 run_zamstorgb：运行从ZAMS至RGB tip阶段模型所需的输入文件，生成的RGB tip模型将用于构建sdB模型 除MESA默认提供的可修改模型初始质量与初始角速度的标准输入参数外，若需生成不同富氢包层质量的sdB模型，需修改run_sdb_deg/inlist_postcee_presdb或run_sdb_nondeg/inlist_cee文件中的x_ctrl(9)参数。该参数默认值为10^-3 Msun，格式如下： x_ctrl(9) = 1d-3 ! 目标富氢包层质量，单位：Msun 若需计算自转受吸积过程影响的sdB模型，可在源代码文件的extras_check_model函数中，通过omp_target或omg_target变量修改目标自转速率。 若需完成从ZAMS至sdB阶段的完整演化计算，需按以下顺序运行模型： 1. 从ZAMS演化至RGB tip：使用run_zamstorgb文件夹中的输入文件，如需可修改inlist_msrgb中的初始参数。 2. 从RGB tip演化至sdB阶段：根据RGB模型的氦点燃条件（简并/非简并），分别使用run_sdb_deg或run_sdb_nondeg文件夹中的输入文件。对于简并氦点燃的情况，需按以下顺序使用输入列表文件： inlist_cee：移除外层富氢包层直至剩余质量为10^-2 Msun，并保存用于下一步的模型文件 inlist_postcee_presdb：加载inlist_cee生成的模型文件，以更低的质量损失速率继续演化直至核心氦点燃。若需生成不同富氢包层质量的模型，可在此步骤修改x_ctrl(9)参数，无需为每组相似初始条件的模型重复第一步（inlist_cee）。 inlist_sdb：加载inlist_postcee_presdb生成的模型文件，计算sdB模型的核心氦燃烧阶段，当中心氦质量分数降至10^-6以下时停止计算。 对于非简并氦点燃的模型，可跳过第二步，并直接在inlist_cee中修改富氢包层质量。 若需计算含吸积过程的sdB模型，需使用run_sdb_accretion文件夹中的输入文件，此时需预先通过前文所述步骤生成零年龄sdB模型。 如有任何疑问或额外需求，请仅联系通讯作者Facundo D. Moyano。