The Role of Magnetic Fields in Setting the Star Formation Rate and the Initial Mass Function

被引：125
|
作者：
Krumholz, Mark R. [1 ,2 ]
Federrath, Christoph [1 ,2 ]
机构：
[1] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia
[2] Ctr Excellence Astron Three Dimens ASTRO 3D, Canberra, ACT, Australia
来源：
FRONTIERS IN ASTRONOMY AND SPACE SCIENCES | 2019年 / 6卷
基金：
澳大利亚研究理事会;
关键词：
galaxies: star formation; ISM: clouds; ISM: kinematics and dynamics; ISM: magnetic fields; magnetohydrodynamics (MHD); stars: formation; turbulence; MHD TURBULENCE SIMULATIONS; WIND-CLOUD INTERACTIONS; GIANT MOLECULAR CLOUDS; X-RAY-EMISSION; AMBIPOLAR-DIFFUSION; SUPERBUBBLE FEEDBACK; MAGNETOHYDRODYNAMIC TURBULENCE; GRAVITATIONAL-INSTABILITY; PROBABILITY-DISTRIBUTION; SUPERNOVA-REMNANTS;
D O I：
10.3389/fspas.2019.00007
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Star-forming gas clouds are strongly magnetized, and their ionization fractions are high enough to place them close to the regime of ideal magnetohydrodyamics on all but the smallest size scales. In this review we discuss the effects of magnetic fields on the star formation rate (SFR) in these clouds, and on the mass spectrum of the fragments that are the outcome of the star formation process, the stellar initial mass function (IMF). Current numerical results suggest that magnetic fields by themselves are minor players in setting either the SFR or the IMF, changing star formation rates and median stellar masses only by factors of similar to 2 - 3 compared to non-magnetized flows. However, the indirect effects of magnetic fields, via their interaction with star formation feedback in the form of jets, photoionization, radiative heating, and supernovae, could have significantly larger effects. We explore evidence for this possibility in current simulations, and suggest avenues for future exploration, both in simulations and observations.
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页数：28
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