Merging Filaments I: A race against collapse

TL;DR

This paper investigates the dynamics of filament mergers in the interstellar medium, developing an analytic model and validating it with simulations to predict outcomes based on initial conditions like distance, mass, and velocity.

Contribution

It introduces a new analytic formula for filament merger timescales and core formation, validated through hydrodynamical simulations, to understand complex filament structures.

Findings

Merger outcomes depend on initial distances, line-masses, and velocities.

The model accurately predicts whether filaments collapse, form cores, or merge into complex structures.

Simulations confirm the analytic predictions across various initial conditions.

Abstract

The interstellar medium is characterised by an intricate filamentary network which exhibits complex structures. These show a variety of different shapes (e.g. junctions, rings, etc.) deviating strongly from the usually assumed cylindrical shape. A possible formation mechanism are filament mergers which we analyse in this study. Indeed, the proximity of filaments in networks suggests mergers to be rather likely. As the merger has to be faster than the end dominated collapse of the filament along its major axis we expect three possible results: (a) The filaments collapse before a merger can happen, (b) the merged filamentary complex shows already signs of cores at the edges or (c) the filaments merge into a structure which is not end-dominated. We develop an analytic formula for the merging and core-formation timescale at the edge and validate our model via hydrodynamical simulations with the adaptive-mesh-refinement-code RAMSES. This allows us to predict the outcome of a filament merger, given different initial conditions which are the initial distance and the respective line-masses of each filament as well as their relative velocities.