Dense cores in dark clouds. VII - Line width-size relations

Details Dense cores in dark clouds. VII - Line width-size relations Dense cores in dark clouds. VII - Line width-size relations

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...384..523f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 384, Jan. 10, 1992, p. 523-527.

Astronomy and Astrophysics

Astronomy

164

Interstellar Matter, Line Spectra, Molecular Clouds, Radio Spectra, Radio Astronomy, Spectral Line Width, Stellar Cores

Scientific paper

Observations of 14 dense cores in lines of CS, C(O-18) and NH3 are combined to examine the relations between the Doppler width of a line and the spatial extent of the map of line intensity. The line width increases with map size R as R exp p. The deduced width of the velocity distribution of the molecule of mean mass has p = 0.20 +/- 0.04, and the deduced width of the nonthermal velocity distribution has p = 0.7 +/- 0.1. The values of p for eight cores with embedded stars and for six cores without embedded stars are statistically indistinguishable, but p is better determined for cores without stars. Thus the physical basis of the line width-size relations is part of the initial conditions for star formation, rather than a consequence of the star-core interaction. The cores appear close to virial equilibrium, consequently the variation of number density with distance from the core density maximum is deduced.

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