Abstract
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 (ρc) 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 (r c) decreases in proportion to (t 0-t)1/2.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Alves, J., Lada, C.J., Lada, E.A., Kenyon, S.J. and Phelps, R.: 1998, Astrophys. J. 506, 292.
Bonnell, I. and Bastien, P.: 1991, Astrophys. J. 374, 610.
Bouquet, S., Feix, M.R., Fijalkow, E. and Munier, A.: 1985, Astrophys. J. 293, 494.
Curry, C.L.: 2000, Astrophys. J. 541, 831.
Fiege, J.D. and Pudritz, R.E.: 2000, Mon. Not. R. Astron. Soc. 311, 105.
Foster, P.N. and Chevalier, R.A.: 1993, Astrophys. J. 416, 303.
Gehman, C.S., Adams, F.C. and Watkins, R.: 1996, 472, 673.
Harjunpaa, P., Kaas, A.A., Carlqvist, P. and Gahm, G.F.: 1999, Astron. Astrophys. 349, 912.
Houlahan, P. and Scalo, J.M.: 1992, Astrophys. J. 393, 172.
Inutsuka, S. and Miyama, S.M.: 1992, Astrophys. J. 388, 392.
Kawachi, T. and Hanawa, T.: 1998, Publ. Astron. Soc. Jpn. 50, 577.
Larson, R.B.: 1969, Mon. Not. R. Astron. Soc. 145, 271.
Larson, R.B.: 1972, Mon. Not. R. Astron. Soc. 157, 121.
Mac Low, M.M.: 1999, Astrophys. J. 524, 169.
Meerson, B., Megged, E. and Tajima, T.: 1996, Astrophys. J. 457, 321.
Myers, P.C.: 1991, in: E. Falgarone and G. Duvert (eds.), Fragmentation of Molecular Clouds and Star Formation, IAU Symp. 147, Kluwer, Dordrecht, 221.
Nagasawa, M.: 1987, Prog. Theor. Phys. 77, 635.
Nagai, T., Inutsuka, S.I. and Miyama, S.M.: 1998, 506, 306.
Nakamura, F. and Hanawa, T.: 1997, Astrophys. J. 480, 701.
Nakamura, F., Hanawa, T. and Nakano, T.: 1993, Publ. Astron. Soc. Jpn. 45, 551.
Nakamura, F., Hanawa, T. and Nakano, T.: 1995, Astrophys. J. 444, 770.
Nakamura, F., Matsumoto, T., Hanawa, T. and Tomisaka, K.: 1999, Astrophys. J. 510, 274.
Ostriker, J.: 1964, Astrophys. J. 140, 1056.
Penston, M.V.: 1969, Mon. Not. R. Astron. Soc. 144, 425.
Saigo, K. and Hanawa, T.: 1998, Astrophys. J. 493, 342.
Schneider, S. and Elmegreen, B.: 1979, Astrophys. J. Suppl. 41, 87.
Semelin, B., Sanchez, N. and de Vega, H.J.: 1999, astro-ph/9908073.
Shu, F.H.: 1977, Astrophys. J. 214, 488.
Spitzer, L., Jr.: 1978, Physical Processes in the Interstellar Medium, Wiley, New York.
Terebey, S., Shu, F.H. and Cassen, P.: 1984, Astrophys. J. 286, 529.
Wiseman, J.J. and Adams, F.C.: 1994, Astrophys. J. 435, 708.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Shadmehri, M., Ghanbari, J. Radiative cooling flows of self-gravitating filamentary clouds. Astrophysics and Space Science 278, 347–355 (2001). https://doi.org/10.1023/A:1013177820161
Issue Date:
DOI: https://doi.org/10.1023/A:1013177820161