Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2009-11-23
Astronomy Reports 2009, vol. 53, pp. 1127-1135
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
12 pages, 3 figures, 4 tables
Scientific paper
10.1134/S1063772909120051
Radial density profiles for the sample of dense cores associated with high-mass star-forming regions from southern hemisphere have been derived using the data of observations in continuum at 250 GHz. Radial density profiles for the inner regions of 16 cores (at distances $\la 0.2-0.8$ pc from the center) are close on average to the $\rho\propto r^{-\alpha}$ dependence, where $\alpha=1.6\pm 0.3$. In the outer regions density drops steeper. An analysis with various hydrostatic models showed that the modified Bonnor-Ebert model, which describes turbulent sphere confined by external pressure, is preferable compared with the logotrope and polytrope models practically in all cases. With a help of the Bonnor-Ebert model, estimates of central density in a core, non-thermal velocity dispersion and core size are obtained. The comparison of central densities with the densities derived earlier from the CS modeling reveals differences in several cases. The reasons of such differences are probably connected with the presence of density inhomogenities on the scales smaller than the telescope beam. In most cases non-thermal velocity dispersions are in agreement with the values obtained from molecular line observations.
No associations
LandOfFree
Density Profiles in Molecular Cloud Cores Associated with High-Mass Star-Forming Regions does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Density Profiles in Molecular Cloud Cores Associated with High-Mass Star-Forming Regions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Density Profiles in Molecular Cloud Cores Associated with High-Mass Star-Forming Regions will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-173339