FORMATION AND EVOLUTION OF FILAMENTARY MOLECULAR CLOUDS WITH OBLIQUE MAGNETIC-FIELD

Using two-dimensional numerical simulations, we have constructed a mod el for formation of a filamentary molecular cloud permeated with an al most perpendicular magnetic held. The model filamentary cloud is forme d by fragmentation of a magnetized sheetlike cloud. It stays in a quas i-static equilibrium for a period that is much longer than its free-fa ll time. In the quasi-static equilibrium, the magnetic held runs paral lel to the cloud axis in the central part of the cloud and almost perp endicular to the axis in the less dense part of the cloud. The inner p arallel magnetic held supports the cloud in part against the cloud gra vity. The parallel magnetic field escapes from the cloud through the A lfven wave and the quasistatic equilibrium state ends. During the quas i-static equilibrium, the cloud is expected to fragment in the directi on of the axis by gravitational instability. We discuss the applicatio n of our model to the filamentary clouds in Taurus.