Structure and radial equilibrium of filamentary molecular clouds

TL;DR

This study investigates the structure and stability of filamentary molecular clouds, emphasizing the potential role of magnetic fields in their equilibrium, through observational analysis of five galactic filaments.

Contribution

It provides observational evidence supporting the influence of magnetic fields, particularly toroidal magnetic fields, in the radial equilibrium of filamentary molecular clouds.

Findings

Filaments have lower lineal masses than their virial masses.

Virial parameters suggest magnetic confinement.

Dust emission shapes indicate toroidal magnetic fields.

Abstract

Recent dust continuum surveys have shown that filamentary structures are ubiquitous along the Galactic plane. While the study of their global properties has gained momentum recently, we are still far from fully understanding their origin and stability. Theories invoking magnetic field have been formulated to help explain the stability of filaments; however, observations are needed to test their predictions. In this paper, we investigate the structure and radial equilibrium of five filamentary molecular clouds with the aim of determining the role that magnetic field may play. To do this, we use continuum and molecular line observations to obtain their physical properties (e.g. mass, temperature and pressure). We find that the filaments have lower lineal masses compared to their lineal virial masses. Their virial parameters and shape of their dust continuum emission suggests that these filaments may be confined by a toroidal dominated magnetic field.