Turbulent Fragmentation and Star Formation

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dc.creatorBallesteros-Paredes, Javier
dc.date2003-11-13
dc.date.accessioned2026-07-07T11:29:16Z
dc.date.available2026-07-07T11:29:16Z
dc.descriptionWe review the main results from recent numerical simulations of turbulent fragmentation and star formation. Specifically, we discuss the observed scaling relationships, the ``quiescent'' (subsonic) nature of many star-forming cores, their energy balance, their synthesized polarized dust emission, the ages of stars associated with the molecular gas from which they have formed, the mass spectra of clumps, and the density and column density probability distribution function of the gas. We then give a critical discussion on recent attempts to explain and/or predict the star formation efficiency and the stellar initial mass function from the statistical nature of turbulent fields. Finally, it appears that turbulent fragmentation alone cannot account for the final stages of fragmentation: although the turbulent velocity field is able to produce filaments, the spatial distribution of cores in such filaments is better explained in terms of gravitational fragmentation.
dc.description14 pages, 1 ps figure. Refered invited review, to appear in "Magnetic Fields and Star Formation: Theory versus Observations", eds. A.I. Gomez de Castro et al. (Kluwer), in press
dc.identifierhttps://arxiv.org/abs/astro-ph/0311319
dc.identifierhttp://arxiv.org/abs/astro-ph/0311319
dc.identifierAstrophys.SpaceSci.292:193-205,2004
dc.identifierdoi:10.1023/B:ASTR.0000045018.50154.b0
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196660
dc.subjectAstrophysics
dc.titleTurbulent Fragmentation and Star Formation
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