Fragmentation of Filamentary Cloud Permeated by Perpendicular Magnetic Field II. Dependence on the Initial Density Profile

Abstract

We examine the linear stability of a filamentary cloud permeated by a perpendicular magnetic field. The initial magnetic field is assumed to be uniform and perpendicular to the cloud axis. The model cloud is assumed to have a Plummer-like density profile and to be supported against the self-gravity by turbulence. The effects of turbulence are taken into account by enhancing the effective pressure of a low density gas. We derive the effective pressure as a function of the density from the condition of the hydrostatic balance. It is shown that the model cloud is more unstable against radial collapse, when the radial density slope is shallower. When the magnetic field is mildly strong, the radial collapse is suppressed. If the displacement vanishes in the region very far from the cloud axis, the model cloud is stabilized completely by a mildly strong magnetic field. If rearrangement of the magnetic flux tubes is permitted, the model cloud is unstable even when the magnetic field is extremely strong. The stability depends on the outer boundary condition as in case of the isothermal cloud. The growth rate of the rearrangement mode is smaller when the radial density slope is shallower.

20 pages, 12 figures, to appear in ApJ

References in corpus (6)

• Polytropic models of filamentary interstellar clouds - I. Structure and stability
• Gravitationally unstable condensations revealed by ALMA in the TUKH122 prestellar core in the Orion A cloud
• Structure and Stability of Filamentary Clouds Supported by Lateral Magnetic Field
• Fragmentation of Filamentary Cloud Permeated by Perpendicular Magnetic Field
• Polytropic models of filamentary interstellar clouds -II. Helical magnetic fields
• Gravitational instability of filamentary molecular clouds, including ambipolar diffusion; Non-isothermal filament

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• Simulation of Head-on Collisions Between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution