Magnetic Field - Gas Density Relation and Observational Implications Revisited

TL;DR

This paper reevaluates the magnetic field and gas density relation in molecular clouds, showing that previous claims of a $B ho^{2/3}$ relation are based on oversimplified models, and that the data actually support a $B ho^{1/2}$ relation.

Contribution

The study identifies flaws in earlier statistical models and observational assumptions, demonstrating that the $B ho^{1/2}$ relation is more consistent with molecular cloud data.

Findings

The $B ho^{2/3}$ relation is inconsistent with observational data.

Relaxing assumptions favors the $B ho^{1/2}$ relation.

Previous models underestimated observational uncertainties.

Abstract

We revisit the relation between magnetic-field strength ($B$) and gas density ($\rho$) for contracting interstellar clouds and fragments (or, cores), which is central in observationally determining the dynamical importance of magnetic fields in cloud evolution and star formation. Recently, it has been claimed that a relation $B \propto \rho^{2/3} $ is statistically preferred over $B \propto \rho^{1/2}$ in molecular clouds, when magnetic field detections and nondetections from Zeeman observations are combined. This finding has unique observational implications on cloud and core geometry: The relation $B \propto \rho^{2/3} $ can only be realized under spherical contraction. However, no indication of spherical geometry can be found for the objects used in the original statistical analysis of the $B-\rho$ relation. We trace the origin of the inconsistency to simplifying assumptions in the statistical model used to arrive at the $B\propto \rho^{2/3}$ conclusion and to an underestimate of observational uncertainties in the determination of cloud and core densities. We show that, when these restrictive assumptions are relaxed, $B \propto \rho^{1/2}$ is the preferred relation for the (self-gravitating) molecular-cloud data, as theoretically predicted four decades ago.