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Star formation in cloud cores — simulations and observations of dense molecular cores and the formation of solar mass stars

Published online by Cambridge University Press:  13 January 2020

C. Federrath Open the ORCID record for C. Federrath [Opens in a new window]
C. Federrath*
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia email: christoph.federrath@anu.edu.au
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Abstract

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Star formation is inefficient. Recent advances in numerical simulations and theoretical models of molecular clouds show that the combined effects of interstellar turbulence, magnetic fields and stellar feedback can explain the low efficiency of star formation. The star formation rate is highly sensitive to the driving mode of the turbulence. Solenoidal driving may be more important in the Central Molecular Zone, compared to more compressive driving agents in spiral-am clouds. Both theoretical and observational efforts are underway to determine the dominant driving mode of turbulence in different Galactic environments. New observations with ALMA, combined with other instruments such as CARMA, JCMT and the SMA begin to reveal the magnetic field structure of dense cores and protostellar disks, showing highly complex field geometries with ordered and turbulent field components. Such complex magnetic fields can give rise to a range of stellar masses and jet/outflow efficiencies in dense cores and protostellar accretion disks.

Keywords

ISM: cloudsISM: jets and outflowsmagnetic fieldsstars: formationturbulence

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