Physical and dynamical properties of a low-mass star-forming region.

Details Physical and dynamical properties of a low-mass star-forming region. Physical and dynamical properties of a low-mass star-forming region.

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995acaps..15..252z&link_type=abstract

Acta Astrophys. Sin., Vol. 15, No. 3, p. 252 - 260

Astronomy and Astrophysics

Astrophysics

Molecular Clouds: Ammonia, Star-Forming Regions: Dynamics

Scientific paper

Eleven low-mass cores are found in the Orion Molecular Cloud 2 from VLA observations of the line emission of NH3(1,1). They are perhaps clumps prior to gravitational collapse with average radius of 0.03 pc and mass of 3.5 Msun, distributed along the central axes of filaments in the NS direction. The authors find a velocity gradient of ≡5 km s-1pc-1 in the declination direction within a 3' region. The author suggests that most of these dense cores are probably protostellar condensations, not yet containing stellar cores, but are self-gravitating systems in thermodynamical equilibrium.

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