The formation of interstellar molecular lines in a turbulent velocity field with finite correlation length III. Spherical clouds in hydrostatic equilibrium.

Details The formation of interstellar molecular lines in a turbulent velocity field with finite correlation length III. Spherical clouds in hydrostatic equilibrium. The formation of interstellar molecular lines in a turbulent velocity field with finite correlation length III. Spherical clouds in hydrostatic equilibrium.

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..841p&link_type=abstract

Astronomy and Astrophysics, v.297, p.841

Astronomy and Astrophysics

Astrophysics

11

Line: Formation, Radiative Transfer, Turbulence, Ism: Clouds, Ism: Molecules, Radio Lines: Interstellar

Scientific paper

We investigated the formation of interstellar molecular lines in a turbulent velocity field with finite correlation length, extending previous work (Albrecht & Kegel 1987; Kegel et al. 1992) to isothermal spheres in hydrostatic equilibrium as cloud models with σ>>v_ therm _. For this we use the transformed generalized radiative transfer equation (Kegel et al. 1992). We concentrate our calculations on the CO-molecule with up to 12 energy levels. We give numerical results for models with T_kin_=50K, σ=3.9km/sec (σ/v_ therm _=22), and different values of the central H_2_ density and different values of the correlation length. As our results show, accounting for a velocity field with a finite correlation length affects the line profiles, the center-to-limb variation, and the intensity ratios. We find that the higher transitions are more strongly affected than the J=1-0 transition.

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