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

## TL;DR

This study investigates how the initial density profile influences the linear stability of filamentary clouds with perpendicular magnetic fields, revealing conditions under which magnetic fields stabilize or fail to stabilize against collapse.

## Contribution

It provides a detailed analysis of the stability dependence on density slope and magnetic field strength, incorporating turbulence effects and boundary conditions.

## Key findings

- Shallower density slopes increase instability against collapse.
- Mildly strong magnetic fields suppress radial collapse.
- Magnetic flux rearrangement can destabilize the cloud even with strong magnetic fields.

## 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.