Astronomy and Astrophysics – Astrophysics
Scientific paper
2000-07-02
Astrophys.Space Sci. 278 (2001) 347-355
Astronomy and Astrophysics
Astrophysics
6 pages, Revised Version, Accepted by the Astrophysics and Space Science
Scientific paper
10.1023/A:1013177820161
We study the dynamics of a self-gravitating cooling filamentary cloud using a simplified model. We concentrate on the radial distribution and restrict ourselves to quasi-hydrostatic, cylindrically symmetric cooling flows. For a power-law dependence of cooling function on the temperature, self-similar solutions which describe quasi-hydrostatic cooling flows are derived. We consider obtically thin filaments with a constant mass per unit length and the solutions are parameterized by their line masses. There is no polytropic relation between the density and the pressure. The filament experiences radiative condensation, irrespective of the \gamma, the gas specific heat ratio. So, the filament becomes denser due to the quasi-hydrostatic flows and the density at the center increases in proportion to (t_{0}-t)^{-1}, where t denotes the time. The term, t_{0}, denotes an epoch at which the central density increases infinitely. We also found that the radius of the filament decreases in proportion to (t_{0}-t)^{0.5}.
Ghanbari Jamshid
Shadmehri Mohsen
No associations
LandOfFree
Radiative Cooling Flows of Self-Gravitating Filamentary Clouds 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 Radiative Cooling Flows of Self-Gravitating Filamentary Clouds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radiative Cooling Flows of Self-Gravitating Filamentary Clouds will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-516042