Supplementary data for the article Fichtner et al., 2024, A&A, 690, A72

Supplementary data for the paper:Fichtner Y. A., Mackey J., Grassitelli L., Romano-Díaz E., Porciani C., 2024, A&A, 690, A72, Connecting stellar and galactic scales: Energetic feedback from stellar wind bubbles to supernova remnants, DOI: https://doi.org/10.1051/0004-6361/202449638 

Paper abstract:Context. Energy and momentum feedback from stars is a key element of models for galaxy formation and interstellar medium dynamics, but resolving the relevant length scales to directly include this feedback remain out of reach of current-generation simulations.Aims. We aim to constrain the energy feedback by winds, photoionisation and supernovae (SNe) from massive stars.Methods. We measure the thermal and kinetic energy imparted to the interstellar medium on various length scales, calculated from high-resolution 1D radiation-hydrodynamics simulations. Our grid of simulations covers a broad range of densities, metallicities, and state-of-the-art evolutionary models of single and binary stars.Results. A single star or binary system can carve a cavity of tens-of-pc size into the surrounding medium. During the pre-SN phase, post-main-sequence stellar winds and photoionisation dominate. While SN explosions dominate the total energy budget, the pre-SN feedback is of great importance by reducing the circumstellar gas density and delaying the onset of radiative losses in the SN remnant. Contrary to expectations, the metallicity dependence of the stellar wind has little effect on the cumulative energy imparted by feedback to the ISM; the only requirement is the existence of a sufficient level of pre-SN radiative and mechanical feedback. The ambient medium density determines how much and when feedback energy reaches to distance >= 10 − 20 pc and affects the division between kinetic and thermal feedback.Conclusions. Our results can be used as a sub-grid model for feedback in large-scale simulations of galaxies. The results reinforce that the uncertain mapping of stellar evolution sequences to SN explosion energy is very important to determining the overall feedback energy from a stellar population.

General description of the data release:The data release contains tables with the cumulative flows of kinetic energy, thermal energy, mass and metal mass as a function of time for every simulation presented in the corresponding paper. The cumulative flows are calculated at three different distances from the stellar source (5, 10 and 20 pc). Exemplary parameter files of the simulations and readme files are also included.The tables could be used in a sub-grid model of stellar feedback to determine the amount of feedback ejecta (mass, metals, thermal and kinetic energy) that can be injected, taking into account the circumstellar medium. It is possible to do so as a function of time, ambient metallicity and ambient density. The data release includes simulations of different stellar models of single and binary stars, making it possible to choose between different stellar populations.It is also possible to use the data for a comparison to other work.

本数据集为以下论文的补充数据：《Connecting stellar and galactic scales: Energetic feedback from stellar wind bubbles to supernova remnants》（关联恒星与银河尺度：星风泡与超新星遗迹的能量反馈），作者为Fichtner Y. A.、Mackey J.、Grassitelli L.、Romano-Díaz E.、Porciani C.，发表于2024年《天文学与天体物理学》（Astronomy & Astrophysics, A&A）第690卷A72号，DOI：https://doi.org/10.1051/0004-6361/202449638。

论文摘要：
研究背景：恒星的能量与动量反馈是星系形成与星际介质（Interstellar Medium, ISM）动力学模型的核心要素，但当前一代模拟仍无法解析相关长度尺度以直接纳入此类反馈。
研究目标：我们旨在约束大质量恒星的星风、光致电离与超新星（Supernovae, SNe）所产生的能量反馈。
研究方法：我们基于高分辨率一维辐射流体动力学模拟结果，计算了不同长度尺度下注入星际介质（ISM）的热能与动能。我们的模拟网格覆盖了宽范围的密度、金属丰度，以及当前最先进的单星与双星演化模型。
研究结果：单颗恒星或双星系统可在周围介质中刻蚀出数十秒差距（pc）尺度的空腔。在超新星前（pre-SN）阶段，主序后星风与光致电离占据主导地位。尽管超新星爆发主导总能量预算，但超新星前反馈通过降低星周气体密度、延迟超新星遗迹的辐射损失起始，具有重要意义。与预期相悖的是，星风的金属丰度依赖性对反馈注入星际介质（ISM）的累积能量影响极小；唯一的必要条件是存在足够水平的超新星前辐射与力学反馈。周围介质密度决定了反馈能量到达≥10-20秒差距距离的程度与时间，并影响动能与热能反馈的分配比例。
研究结论：我们的结果可作为星系大尺度模拟中反馈的亚网格模型。研究结果进一步证实，恒星演化序列到超新星爆发能量的不确定映射关系，对于确定恒星族群的总反馈能量至关重要。

数据发布总体说明：本数据发布包含表格，收录了对应论文中所有模拟的动能、热能、质量与金属质量随时间的累积流量，这些流量是在距恒星源5、10和20秒差距三个不同距离处计算得到的。此外还附带了模拟示例参数文件与自述文件。
该表格可应用于恒星反馈的亚网格模型，用于确定可注入的反馈抛射物（质量、金属、热能与动能）总量，同时可纳入星周介质的影响。上述分析可作为时间、周围金属丰度与周围密度的函数进行。本数据发布包含单星与双星的不同恒星模型模拟，支持针对不同恒星族群进行选择。
此外，本数据也可用于与其他研究工作进行对比。