2000/07/31 by Mohsen Shadmehri, Jamshid Ghanbari
Physics and Astronomy · #Advanced Thermodynamics and Statistical Mechanics #Astrophysics and Star Formation Studies #Constant (computer programming) #Cosmology and Gravitation Theories #Distribution function #Line (geometry) #Parameterized complexity #Polytropic process #Protein filament #RADIUS #Radiative cooling #Radiative transfer #astro-ph
paper · pdf · doi:10.1023/a:1013177820161
published as Astrophys.Space Sci. 278 (2001) 347-355 · 6 pages, Revised Version, Accepted by the Astrophysics and Space Science
arxiv created 2001/01/30 · openalex publication_date 2001/11/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 γ, 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 (t0-t)-1, where t denotes the time. The term, t0, denotes an epoch at which the central density increases infinitely. We also found that the radius of the filament decreases in proportion to (t0-t)0.5.