Guillermo Arreaga–García and Julio Saucedo Morales
Centro de Investigación en Física, Universidad de Sonora, Apdo. Postal 14740, CP. 83000, Hermosillo, Sonora, Mexico. (garreaga@cajeme.cifus.uson.mx).
Received 2011 August 18.
Accepted 2011 November 17.
]]> RESUMEN
En este trabajo estudiamos el colapso gravitacional de una nube de gas de hidrógeno molecular compuesta de un núcleo más una envolvente de gas rodeando al núcleo. Simulamos numéricamente el colapso de cuatro modelos de nube para entrever la evolución temporal de algunas variables dinámicas, entre otras, el momento angular y la razón aem; las razones entre las energías térmica y rotacional con respecto a la energía potencial gravitacional, denotadas como α y β, respectivamente. Retomamos los modelos introducidos por Arreaga et al. (2010) para hacer una caracterización cuantitativa de los diferentes resultados del colapso de la nube por medio de las variables dinámicas ya mencionadas. Mostramos que podemos comparar cuantitativamente los electos de la extensión de la envolvente de gas sobre el colapso del núcleo.
ABSTRACT
In this paper we study the gravitational collapse of a molecular hydrogen gas cloud composed of a core plus a gas envelope surrounding the core. We numerically simulate the collapse of four cloud models to obtain a glimpse into the time evolution of several dynamic variables, such as the angular momentum and the aem ratio, as well as the ratios between the thermal and rotational energies with respect to the potential gravitational energy, denoted as α and β, respectively, among others. We reconsider the models introduced by Arreaga et al. (2010) in the present paper in order to produce different outcomes of the collapsing cloud characterized in terms of the aforementioned dynamical variables. Such characterization was missing in the paper by Arreaga et al. (2010), and here we show that the gas envelope extension effects on the collapsing core can be quantitatively compared.
Key Words: binaries: close — hydrodynamics — methods: numerical — stars: formation.
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REFERENCES
]]>Arreaga, G., Klapp, J., & Gómez, F. 2010, A & A, 509, A96 [ Links ]
Arreaga, G., Klapp, J., Sigalotti, L., & Gabbasov, R. 2007, ApJ, 666, 290 [ Links ]
Arreaga, G., Saucedo, J., Duarte, R., & Carmona, J. 2008, RevMexAA, 44, 2, 259 [ Links ]
Bate, M. R., Bonnell, I. A., & Price, N. M. 1995, MNRAS, 277, 362 [ Links ]
Boss, A. P. 1987, ApJ, 319, 149 [ Links ]
––––––––––. 1991, Nature, 351, 298 [ Links ]
Boss, A. P., & Bodenheimer, P. 1979, ApJ, 234, 289 [ Links ]
Boss, A. P., Fisher, R. T., Klein, R., & McKee, C. F. 2000, ApJ, 528, 325 [ Links ]
Bodenheimer, P. 1995, ARA & A, 33, 199 [ Links ]
Bodenheimer, P., Burkert, A., Klein, R. I., & Boss, A. P. 2000, in Protostars and Planets IV, ed. V. G. Mannings, A. P. Boss, & S. S. Russell (Tucson: Univ. Arizona Press), 675 [ Links ]
Burkert, A., & Bodenheimer, P. 1993, MNRAS, 264, 798 [ Links ]
––––––––––. 1996, MNRAS, 280, 1190 [ Links ]
Burkert, A., & Hartmann, L. 2004, ApJ, 616, 288 [ Links ]
Felice, F., & Sigalotti, L. D. 1992, ApJ, 389, 386 [ Links ]
Goodman, A. A., Benson, P. J., Fuller, G. A., & Myers, P. C. 1993, ApJ, 406, 528 [ Links ]
Lin, M. K., Krumholz, M., & Kratter, K. M. 2011, MNRAS, 416, 580 [ Links ]
Natarajan, P., & Lyndell–Bell, D. 1997, MNRAS, 286, 268 [ Links ]
Plummer, H. C. 1911, MNRAS, 71, 460 [ Links ]
Sigalotti, L. D., & Klapp, J. 1994, MNRAS, 268, 625 [ Links ]
––––––––––. 1996, MNRAS, 281, 449 [ Links ]
––––––––––. 1997, A & A, 319, 547 [ Links ]
–––––––––– . 2001, Int. J. Mod. Phys. D, 10, 115 [ Links ]
Springel, V., Yoshida, N., & White, D. M. 2001, New Astron., 6, 79 [ Links ]
Tsukamoto, Y., & Machida, M. N. 2011, MNRAS, 416, 591 [ Links ]
Tsuribe, T. 2002, Prog. Theor. Phys. Suppl, 147, 155 [ Links ]
Tsuribe, T., & Inutsuka, S. 1999, ApJ, 523, L155 [ Links ]
Whitworth, A. P., & Ward–Thompson, D. 2001, ApJ, 54, 317 [ Links ]
Zinnecker, H. 2004, RevMexAA, 22, 77 [ Links ] ]]>