Observational diagnostics of self-gravitating MHD turbulence in giant molecular clouds
The Astrophysical Journal, 2015•iopscience.iop.org
We study the observable signatures of self-gravitating magnetohydrodynamics (MHD)
turbulence by applying the probability density functions (PDFs) and the spatial density
power spectrum to synthetic column density maps. We find that there exists three
characterizable stages of the evolution of the collapsing cloud which we term" early,""
intermediate," and" advanced." At early times, ie, $ t\lt 0.15 {t} _ {\mathrm {ff}} $
turbulence by applying the probability density functions (PDFs) and the spatial density
power spectrum to synthetic column density maps. We find that there exists three
characterizable stages of the evolution of the collapsing cloud which we term" early,""
intermediate," and" advanced." At early times, ie, $ t\lt 0.15 {t} _ {\mathrm {ff}} $
Abstract
We study the observable signatures of self-gravitating magnetohydrodynamics (MHD) turbulence by applying the probability density functions (PDFs) and the spatial density power spectrum to synthetic column density maps. We find that there exists three characterizable stages of the evolution of the collapsing cloud which we term" early,"" intermediate," and" advanced." At early times, ie,
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