Star Formation in Molecular Clouds

@article{Krumholz2011StarFI,
  title={Star Formation in Molecular Clouds},
  author={Mark R. Krumholz},
  journal={arXiv: Astrophysics of Galaxies},
  year={2011},
  volume={1386},
  pages={9-57}
}
  • M. Krumholz
  • Published 26 January 2011
  • Physics
  • arXiv: Astrophysics of Galaxies
Star formation is one of the least understood processes in cosmic evolution. It is difficult to formulate a general theory for star formation in part because of the wide range of physical processes involved. The interstellar gas out of which stars form is a supersonically turbulent plasma governed by magnetohydrodynamics. This is hard enough by itself, since we do not understand even subsonic hydrodynamic turbulence very well, let alone supersonic non‐ideal MHD turbulence. However, the behavior… 
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References

SHOWING 1-10 OF 13 REFERENCES
Collapse-Driven Outflow in Star-Forming Molecular Cores
Dynamical collapses of magnetized molecular cloud cores are studied with magnetohydrodynamic simulations from the runaway collapse phase to the accretion phase. In the runaway collapse phase, a disk
Two Regimes of Turbulent Fragmentation and the Stellar Initial Mass Function from Primordial to Present-Day Star Formation
The Padoan and Nordlund model of the stellar initial mass function (IMF) is derived from low-order statistics of supersonic turbulence, neglecting gravity (e.g., gravitational fragmentation,
Giant Molecular Clouds in Local Group Galaxies
We present the first comparative study of extragalactic GMCs using complete data sets for entire galaxies and a uniform set of reduction and analysis techniques. We present results based on CO
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample
Physical dust models are presented for 65 galaxies in SINGS that are strongly detected in the four IRAC bands and three MIPS bands. For each galaxy we estimate (1) the total dust mass, (2) the
The Initial Mass Function: From Salpeter 1955 to 2005
Fifty years after Ed Salpeter's seminal paper, tremendous progress both on the observational and theoretical sides allow a fairly accurate determination of the Galactic IMF not only down to the
The Formation of Stars
Preface. I Star Formation in Our Galaxy. 1 Overview. 1.1 Stellar Nurseries: Orion. 1.2 Stellar Nurseries: Taurus-Auriga. 1.3 Stars and Their Evolution. 1.4 The Galactic Context. 2 The Interstellar
The Physics and Chemistry of the Interstellar Medium
1. The galactic ecosystem 2. Cooling processes 3. Heating processes 4. Chemical processes 5. Interstellar dust 6. Interstellar polycyclic aromatic hydrocarbon molecules 7. HII regions 8. The phases
The Mass Spectra of Giant Molecular Clouds in the Local Group
We reanalyze the catalogs of molecular clouds in the Local Group to determine the parameters of their mass distributions in a uniform manner. The analysis uses the error‐in‐variables method of
THE STAR FORMATION RATE OF SUPERSONIC MAGNETOHYDRODYNAMIC TURBULENCE
This work presents a new physical model of the star formation rate (SFR), which is verified with an unprecedented set of large numerical simulations of driven, supersonic, self-gravitating,
The Initial Mass Function and Its Variation (Review)
  • 2002
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