"Energy and timescales of the jittering jet explosion mechanism (JJEM) versus the neutrino-driven mechanism", Wang, Shishkin, Soker 2026

Models, inlists and modified files as described in "Jittering jets in stripped-envelope core-collapse supernovae" by Wang, Shishkin, Soker 2025. Using the one-dimensional stellar evolution code MESA, we find that all our models in the initial mass range of M_ZAMS=12-40Mo, regardless of whether they have hydrogen-rich, hydrogen-stripped, or helium+hydrogen-stripped envelopes, have at least one significant strong convective zone in the inner core, which can facilitate the jittering-jets explosion mechanism (JJEM). We focus on stripped-envelope CCSN progenitors that earlier studies of the JJEM did not study, and examine the angular momentum parameter j(m)=rv_conv, where r is the radius of the layer and v_conv is the convective velocity according to the mixing length theory. In all models, there is at least one prominent convective zone with j(m) > 2x10^15 cm^2/s inside the mass coordinate that is the maximum baryonic mass of a neutron star (NS), m~2.65Mo. According to the JJEM, convection in these zones seeds instabilities above the newly born NS, leading to the formation of intermittent accretion disks that launch pairs of jittering jets, which in turn explode the star. Our finding is encouraging for the JJEM, although it does not show that the intermittent accretion disks indeed form. We strengthen the claim that, according to the JJEM, there are no failed CCSNe and that all massive stars explode. In demonstrating the robust convection in the inner core of stripped-envelope CCSN progenitors, we add to the establishment of the JJEM as the primary explosion mechanism of CCSNe. We use the one-dimensional stellar evolution code MESA (Modules for Experiments in Stellar Astrophysics; version 24.08.1, SDK version x86_64-linux-24.7.1) to simulate twelve different masses of core-collapse supernovae progenitors, having zero-age main sequence masses ranging M_ZAMS=12-40Mo. For each mass we simulated three scenarios of envelope stripping: a regular wind that leaves a hydrogen-rich envelope at the explosion (``full envelope''), evolution that includes an extra mass loss that removes the hydrogen but leaves helium (``H-stripped envelope''), and the removal of both hydrogen and helium (``He-stripped envelope''). Models We make available our set of models at the onset of collapse, where the infall velocity at atleast one mass coordinate exceeds 100 km/s. These are organized according to initial mass, envelope removal, and the (arbitrary) profile number assigned at simulation time as part of the final segment leading to core collapse: ##M_{}profileZZZ.data; ## is the initial stellar mass, {} corresponds to envelope removal ('' for non, '_H' for hydrogen envelope removal and '_He' for helium envelope removal) and ZZZ the profile number along the simulation. Modified files We implement a helium envelope removal scheme that is identical in spirit to the hydrogen removal scheme within MESA. For consistency, we chose to precisely duplicate the hydrogen removal scheme, but set the removal to be to the carbon-oxygen core (from helium core in the default hydrogen removal scheme).As the MESA removal scheme is a star_job routine, we modified source files in the following locations and added a new removal routine and appropriate references: star/public/star_lib star/private/star_job_ctrls_io star/defaults/star_job.defaults star/run_star_support.f90 include/star_job_controls.inc , star_data/private/star_job_controls.inc Exact lines modified can be found by searching for the new routines names: relax_mass_to_remove_He_env, relax_initial_mass_to_remove_He_env Inlists We add an example set of inlists used to run the simulation. These are based on the `20M_pre_ms_to_core_collapse' test_suite example.本数据集包含Wang、Shishkin与Soker于2025年发表的论文《剥离包层核坍缩超新星的抖动喷流》（Jittering jets in stripped-envelope core-collapse supernovae）中提及的模型、输入配置文件（inlists）与修改后的代码文件。 本研究采用一维恒星演化代码MESA（Modules for Experiments in Stellar Astrophysics）开展模拟，结果显示：所有初始零年龄主序星质量（M_ZAMS）处于12~40倍太阳质量（M☉）范围内的模型，无论其包层为富氢型、氢剥离型还是氢+氦剥离型，其内核均存在至少一处显著的强对流区，这一特征可为抖动喷流爆炸机制（Jittering-Jets Explosion Mechanism, JJEM）提供有利条件。 我们聚焦于此前JJEM相关研究未曾涉及的剥离包层核坍缩超新星（Core-Collapse Supernova, CCSN）前身星，对其角动量参数j(m)=rv_conv进行了分析，其中r为对流层半径，v_conv为混合长理论（Mixing Length Theory）框架下的对流速度。所有模型的中子星（Neutron Star, NS）最大重子质量对应的质量坐标内部，均存在至少一处j(m)>2×10^15 cm²/s的强对流区。根据JJEM，此类区域的对流会在新生中子星上方触发不稳定性，进而形成间歇性吸积盘，驱动成对的抖动喷流，最终将恒星炸毁。本研究结果对JJEM而言是有力支撑，尽管尚未直接证明间歇性吸积盘确实能够形成。我们进一步佐证了JJEM的核心论断：根据该机制，不存在‘失败的核坍缩超新星’，所有大质量恒星最终都会发生爆发。本研究通过证实剥离包层CCSN前身星的内核存在强对流，进一步推动了JJEM成为核坍缩超新星主流爆发机制的学界共识。 本研究采用MESA（Modules for Experiments in Stellar Astrophysics）版本24.08.1（SDK版本x86_64-linux-24.7.1），对12组不同初始质量的CCSN前身星进行模拟，其零年龄主序星质量范围为M_ZAMS=12~40M☉。针对每组初始质量，我们模拟了三种包层剥离情景：一是仅通过常规星风保留富氢包层至爆发阶段的‘完整包层’情景；二是通过额外质量损失移除氢元素但保留氦元素的‘氢剥离包层（H-stripped envelope）’情景；三是同时移除氢与氦元素的‘氦剥离包层（He-stripped envelope）’情景。 ### 模型文件 我们公开了所有坍缩起始时刻的模型数据集，此时至少有一个质量坐标处的下落速度超过100 km/s。模型文件按初始恒星质量、包层剥离类型与模拟阶段分配的任意剖面编号（用于标识最终核心坍缩阶段）进行组织，命名格式为：`##M_{}profileZZZ.data`。其中：##为初始恒星质量数值，{}代表包层剥离类型（空字符串代表无剥离，`_H`代表移除氢包层，`_He`代表移除氦包层），ZZZ为模拟过程中的剖面编号。 ### 修改后的代码文件 我们实现了一套与MESA内置氢包层剥离方案精神一致的氦包层剥离方案。为保证代码一致性，我们完全复刻了氢包层剥离的代码逻辑，但将剥离终止位置设置为碳氧核（默认氢剥离方案的终止位置为氦核）。由于MESA的剥离方案属于star_job子程序，我们修改了以下路径的源代码文件，并新增了一套剥离子程序与相关引用： - star/public/star_lib - star/private/star_job_ctrls_io - star/defaults/star_job.defaults - star/run_star_support.f90 - include/star_job_controls.inc、star_data/private/star_job_controls.inc 可通过检索新增子程序名称`relax_mass_to_remove_He_env`与`relax_initial_mass_to_remove_He_env`，定位所有被修改的代码行。 ### 输入配置文件（inlists） 我们提供了一套用于运行模拟的示例输入配置文件，其基于`20M_pre_ms_to_core_collapse`测试套件的示例文件修改而来。