Morphology of prestellar cores in pressure confined filaments

TL;DR

This paper explains the different observed morphologies of prestellar cores in star-forming filaments using a gravitational instability model, linking core shape to filament line-mass and stability conditions.

Contribution

It introduces a model connecting core morphology to filament line-mass and stability, providing a diagnostic for core formation based on initial conditions.

Findings

Broad cores form in less than half critical line-mass filaments.

Pinched cores form in more than half critical line-mass filaments.

Core morphology is independent of perturbation scale and inclination.

Abstract

Observations of prestellar cores in star-forming filaments show two distinct morphologies. While molecular line measurements often show broad cores, submillimeter continuum observations predominantly display pinched cores compared to the bulk of the filament gas. In order to explain how different morphologies arise, we use the gravitational instability model where prestellar cores form by growing density perturbations. The radial extent at each position is set by the local line-mass. We show that the ratio of core radius to filament radius is determined by the initial line-mass of the filament. Additionally, the core morphology is independent of perturbation length scale and inclination, which makes it an ideal diagnostic for observations. Filaments with a line-mass of less than half its critical value should form broad cores, whereas filaments with more than half its critical line-mass value should form pinched cores. For filaments embedded in a constant background pressure, the dominant perturbation growth times significantly differ for low and high line-mass filaments. Therefore, we predict that only one population of cores is present if all filaments within a region begin with similar initial perturbations.