The Environment Around Young Stars in Molecular Cores

Details The Environment Around Young Stars in Molecular Cores The Environment Around Young Stars in Molecular Cores

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dln.........17g&link_type=abstract

Daresbury Laboratory: Newsletter on Analysis of Astronomical Spectra, p. 17

Astronomy and Astrophysics

Astronomy

Stars, Star Formation, Clumps, Radio Emission, Molecular Clouds, Molecular Gases, Infrared Radiation, Ammonia, Gas Density, Hydrogen, Radii

Scientific paper

It has been established in recent years that molecular clouds exhibit a hierarchichal structure (Goldsmith). This structure can be loosely categorized in the following way: molecular clouds are composed of 'cores', which in turn are composed of 'clumps', within which stars form. The cores have mean molecular hydrogen densities of a few 104/cu cm and radii 0.1-0.5 pc. These structures are often traced by ammonia emission (Benson & Myers). Higher resolution observations in the emission of HCO(+), CS etc. reveal substructure within these cores. The clumps are more compact (r approximately 0.05 pc or less) and somewhat denser (nH2 approximately 106/cu cm). The ultimate signature of the (proto)stars themselves, such as infrared and radio emission, arises from within the clumps.

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