Physical properties of interstellar filaments

TL;DR

This paper models interstellar filaments as isothermal self-gravitating cylinders, analyzing their physical properties, stability, and relation to star formation, with results aligning well with recent observations.

Contribution

It provides analytical expressions for filament properties based on the mass line ratio and compares these with observations, enhancing understanding of filament stability and star formation.

Findings

Good agreement between model predictions and observed filament widths and densities.

Filaments become more gravitationally unstable as the mass line ratio approaches unity.

Core formation is promoted in intermediate stability filaments with specific separations.

Abstract

We analyze the physical parameters of interstellar filaments that we describe by an idealized model of isothermal self-gravitating infinite cylinder in pressure equilibrium with the ambient medium. Their gravitational state is characterized by the ratio f_cyl of their mass line density to the maximum possible value for a cylinder in a vacuum. Equilibrium solutions exist only for f_cyl < 1. This ratio is used in providing analytical expressions for the central density, the radius, the profile of the column density, the column density through the cloud centre, and the fwhm. The dependence of the physical properties on external pressure and temperature is discussed and directly compared to the case of pressure-confined isothermal self-gravitating spheres. Comparison with recent observations of the fwhm and the central column density N_H(0) show good agreement and suggest a filament temperature of ~10 K and an external pressure p_ext/k in the range 1.5x10^4 K/cm^3 to 5x10^4 K/cm^3. Stability considerations indicate that interstellar filaments become increasingly gravitationally unstable with mass line ratio f_cyl approaching unity. For intermediate f_cyl>0.5 the instabilities should promote core formation through compression, with a separation of about five times the fwhm. We discuss the nature of filaments with high mass line densities and their relevance to gravitational fragmentation and star formation.