标题： 由暗物质湮灭驱动的原初 III.1 原恒星的演化。 I. 基准模型和初步结果 显示英文标题

标题： The Evolution of Pop III.1 Protostars Powered by Dark Matter Annihilation. I. Fiducial model and first results

摘要： 在红移$z \gtrsim 7$处存在十亿倍太阳质量的类星体，这对黑洞形成理论提出了严峻的挑战，需要快速生长大质量种子的途径。 第三星族1型恒星，在原始、致密的暗物质（DM）小晕中形成，是有力的前身星。 本研究展示了使用\textsc{基因}代码计算的吸积第三星族1型原恒星的一套恒星演化模型。 我们系统地探索了广泛的参数空间，涵盖环境WIMP密度为$\rho_\chi \sim 10^{12}\mbox{-}10^{16}\,\mathrm{GeV\,cm^{-3}}$和气体吸积率为$10^{-3}\mbox{-}10^{-1}\,M_\odot\,\mathrm{yr^{-1}}$，以量化暗物质湮灭的影响。 一个核心发现是，为了使原恒星增长到超大质量尺度（$\gtrsim 10^5 \, M_{\odot}$），恒星附近的环境暗物质密度必须超过一个临界阈值$\rho_{\chi} \gtrsim 5 \times 10^{14} \, \text{GeV cm}^{-3}$。 WIMP湮灭注入的能量膨胀了原恒星，降低了其表面温度，抑制了会阻止吸积的电离反馈，并显著延迟了氢融合的开始。 这种加热也决定了恒星的最终命运：在致密的晕（$\rho_\chi \gtrsim 10^{15}\,\mathrm{GeV\,cm^{-3}}$）中，恒星在$10^6 \, M_{\odot}$以上仍能抵抗广义相对论不稳定性，而在较低密度（$\rho_\chi \lesssim 10^{13}\,\mathrm{GeV\,cm^{-3}}$）下，它们会在$\sim 5 \times 10^5 \, M_{\odot}$的质量下坍缩。 一旦暗物质燃料耗尽并开始核心燃烧，原恒星会收缩，其电离光子输出可以达到非常高的水平$\sim 10^{53} s^{-1}$。 这些不同的演化阶段为JWST提供了清晰的观测特征，为早期宇宙中形成大质量黑洞种子提供了一条坚实且物理基础牢固的路径。 显示英文摘要

摘要： The existence of billion-solar-mass quasars at redshifts $z \gtrsim 7$ poses a formidable challenge to theories of black hole formation, requiring pathways for the rapid growth of massive seeds. Population III.1 stars, forming in pristine, dense dark matter (DM) minihalos, are compelling progenitors. This study presents a suite of stellar evolution models for accreting Pop III.1 protostars, calculated with the \textsc{GENEC} code. We systematically explore a wide parameter space, spanning ambient WIMP densities of $\rho_\chi \sim 10^{12}\mbox{-}10^{16}\,\mathrm{GeV\,cm^{-3}}$ and gas accretion rates of $10^{-3}\mbox{-}10^{-1}\,M_\odot\,\mathrm{yr^{-1}}$, to quantify the effects of DM annihilation. A central finding is that for a protostar to grow to supermassive scales ($\gtrsim 10^5 \, M_{\odot}$), the ambient DM density in the immediate vicinity of the star must exceed a critical threshold of $\rho_{\chi} \gtrsim 5 \times 10^{14} \, \text{GeV cm}^{-3}$. The energy injected by WIMP annihilation inflates the protostar, lowering its surface temperature, which suppresses the ionizing feedback that would otherwise halt accretion and significantly delays the onset of hydrogen fusion. This heating also governs the star's final fate: in dense halos ($\rho_\chi \gtrsim 10^{15}\,\mathrm{GeV\,cm^{-3}}$), stars remain stable against general relativistic instability beyond $10^6 \, M_{\odot}$, whereas at lower densities ($\rho_\chi \lesssim 10^{13}\,\mathrm{GeV\,cm^{-3}}$), they collapse at masses of $\sim 5 \times 10^5 \, M_{\odot}$. Once the DM fuel is exhausted and core burning commences, the protostar contracts and its ionising photon output can reach very high levels $\sim 10^{53} s^{-1}$. These distinct evolutionary phases offer clear observational signatures for the JWST, providing a robust, physically-grounded pathway for forming heavy black hole seeds in the early universe.