Effects of the environment and feedback physics on the initial mass function of stars in the STARFORGE simulations
Effects of the environment and feedback physics on the initial mass function of stars in the STARFORGE simulations
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STARFORGE 模拟中环境和反馈物理对恒星初始质量函数的影响
DOI：
10.1093/mnras/stac2060
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发表时间：
2022
影响因子：
4.8
通讯作者：
Rosen, Anna L.
中科院分区：
文献类型：
--
作者：
Guszejnov, Dávid;Grudić, Michael Y.;Offner, Stella S. R.;Faucher-Giguère, Claude-André;Hopkins, Philip F.;Rosen, Anna L.
星星形成的一个关键谜团是恒星初始质量函数（IMF）的起源。IMF在银河系及其卫星中几乎是普遍存在的，只有在极端环境中才能推断出显著的变化，例如大质量椭圆星系的核心和中央分子带。在这项工作中，我们提出了模拟的STARFORGE项目是第一个云尺度的辐射磁流体动力学模拟，遵循个别恒星，包括所有相关的物理过程。模拟包括详细的气体热力学，以及恒星反馈的形式，原恒星喷流，恒星辐射，风和超新星。在这项工作中，我们专注于恒星辐射，风和超新星如何影响恒星形成云。辐射反馈在猝灭星星的形成和破坏云中起着重要作用;然而，IMF峰值主要由原恒星喷流物理学设定。我们发现，恒星风的影响是轻微的，和超新星“发生太晚"影响IMF或淬火星星的形成。我们还研究了初始条件对IMF的影响。我们发现，IMF是不敏感的初始湍流，云的质量，云的表面密度，即使这些参数显着形状的星星形成历史的云，包括最终的星星形成效率。同时，特征恒星质量与金属丰度和星际辐射场的关系很弱，而星际辐射场基本上决定了气体的平均温度。最后，虽然湍流驱动和磁化水平强烈影响星星的形成历史，但它们只影响IMF的高质量斜率。
One of the key mysteries of star formation is the origin of the stellar initial mass function (IMF). The IMF is observed to be nearly universal in the Milky Way and its satellites, and significant variations are only inferred in extreme environments, such as the cores of massive elliptical galaxies and the Central Molecular Zone. In this work, we present simulations from the STARFORGE project that are the first cloud-scale radiation-magnetohydrodynamic simulations that follow individual stars and include all relevant physical processes. The simulations include detailed gas thermodynamics, as well as stellar feedback in the form of protostellar jets, stellar radiation, winds, and supernovae. In this work, we focus on how stellar radiation, winds, and supernovae impact star-forming clouds. Radiative feedback plays a major role in quenching star formation and disrupting the cloud; however, the IMF peak is predominantly set by protostellar jet physics. We find that the effect of stellar winds is minor, and supernovae ‘occur too late’ to affect the IMF or quench star formation. We also investigate the effects of initial conditions on the IMF. We find that the IMF is insensitive to the initial turbulence, cloud mass, and cloud surface density, even though these parameters significantly shape the star formation history of the cloud, including the final star formation efficiency. Meanwhile, the characteristic stellar mass depends weakly on metallicity and the interstellar radiation field, which essentially set the average gas temperature. Finally, while turbulent driving and the level of magnetization strongly influence the star formation history, they only influence the high-mass slope of the IMF.
M33 巨型分子云中嵌入大量年轻恒星物体
DOI：
--
发表时间：
2019
期刊：
影响因子：
--
作者：
Tokuda;Kazuki; Muraoka;Kazuyuki; Kondo;Hiroshi; Nishimura;Atsushi; Tosaki;Tomoka; Zahorecz;Sarolta; Onodera;Sachiko; Miura;Rie E.; Torii;Kazufumi; Kuno;Nario; Fujita;Shinji; Sano;Hidetoshi; Onishi;Toshikazu; Saigo;Kazuya; Fukui;Yasuo; Kawam;Rie E. Miura
通讯作者：
Rie E. Miura