Synthesized spectra of turbulent clouds

Details Synthesized spectra of turbulent clouds Synthesized spectra of turbulent clouds

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..728f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 436, no. 2, p. 728-740

Astronomy and Astrophysics

Astrophysics

90

Compressible Flow, Gas Dynamics, Gas Flow, Interstellar Gas, Magnetohydrodynamic Flow, Molecular Clouds, Supersonic Flow, Velocity Distribution, Computerized Simulation, Flow Velocity, Kinematics, Mathematical Models, Turbulence

Scientific paper

A comparison has been made of the velocity structure of non-star-forming dense molecular clouds and the output of a 5123 hydrodynamic code for compressible gas displaying features of turbulence. A remarkable similarity exists between the interstellar line profiles and the velocity profiles found by integrating, with an optically thin assumption, through subsections of the simulation. This similarity is in terms of both the structure of individual spectra, showing skewness, multiple peaks, and wings, and also the variations of the spectra from point to point. It is possible to see the origin of the various velocity substructures and how they correlate with regions of high density and velocity divergence, or regions of high vorticity, by deprojecting individual spectra of the simulation. It is found that the interstellar medium spectra are best represented by the epoch of the simulation in which the energy spectrum is essentially Kolmogorov-like and initially developed shocks have been largely converted into vorticity structures. Further, it is found that the vorticity peaks ascribed to intermittency contribute to the non-Gaussian features and wings of the line profile, but at an intensity level that is weak compared to the contribution of the bulk of the flow.

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