Fragmentation of Elongated Cylindrical Clouds

Details Fragmentation of Elongated Cylindrical Clouds Fragmentation of Elongated Cylindrical Clouds

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993rmxaa..27..161m&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 27, 161

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Scientific paper

RESUMEN Usando simulaciones hidrodinamicas tridimensionales estudiamos la fragmentaci6n de nubes moleculares uniformes, isotermicas y alargadas, las cuales estan rotando alrededor de 1111 eje perpendicular a la direcci6n de 511 alargamiento. Argument amos que este proceso puede resultar en la formaci6n de estrellas binarias y multiples. Este nuevo metodo en la producci6n de estrellas binarias puede explicar sistemas binarios de gran separaci6n, con grandes excentricidades y diversas razones de masas. Para niimeros de Jeans, J0, (la raz6n de energias de amarre a energias termicas) relativamente bajos, se forma un sistema binario simple. Para mayores valores de J0, fragmentaci6n multiple ocurre entre los fragmentos binarios, fbrma'ndose asi un sistema miiltiple. Esta fragmentaci6n adicional esponta'nea es inducida por la rotaci6n. El anadir una componente del momento angular paralela al eje de alargamiento, complica este escenario. Para J0 pequeno, aun se forma un sistema binario simple. Para J0 mayor la fragmentaci6n multiple ya no ocurre entre los fragmentos binarios, pero a cambio los mismos fragmentos binarios pueden fragmentarse a trave's de un estado de barra intermedio, 0 a trave's de un estado de disco intermedio. ABSTRACT Using 3D hydrodynamical simulations, we study the fragmentation of uniform, isothermal, elongated molecular clouds, which are slowly rotating around an axis perpendicular to their elongation. We argue that this process could result in the formation of binary and multiple stars. This new method for forming binary stars can explain widely separated binaries with large eccentricities and various mass ratios. At relatively low Jeans numbers Jo (the ratio of the binding energies to thermal energies), a simple binary system is formed. For higher J0, multiple fragmentation occurs between the binary fragments, forming a multiple system. This spontaneous additional fragmentation is induced by rotation. The addition of an angular momentum component parallel to the axis of elongation complicates this scenario. At low J0, a simple binary is still formed. At higher Jo, multiple fragmentation no longer occurs between the binary fragments but instead the binary fragments themselves can fragment through an intermediary bar stage, or through an intermediary fragment-disk stage. Key u;ords: HYDRODYNAMICS ISM: CLOUDS ISM: KINE- MATICS AND DYNAMICS STARS: FORMATION

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