Physics

Supernova

Magnetic field

Star formation

Stars

Photoionization

Initial mass function

Ionization

Astrophysics

Quantum mechanics

Radiative transfer

Frontiers in Astronomy and Space Sciences

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 by 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 fairly minor players in setting either the SFR or the IMF, changing outcomes only at the factor of ~2-3 level compared to non-magnetized flows. However, the possibility remains that 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 hints at that direction in current simulations, and suggest avenues for future exploration, both in simulations and observations.

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