Solid H2 in the interstellar medium

TL;DR

This study uses molecular dynamics simulations to quantify the formation of solid hydrogen in the interstellar medium, revealing rapid condensation and potential implications for star formation and baryon hiding.

Contribution

It provides the first detailed quantification of solid H2 formation in the ISM, including extrapolation laws for various densities and temperatures, aiding complex astrophysical simulations.

Findings

Solid H2 fraction exceeds 0.1 in phase transition conditions

Condensation occurs within less than one second, considered instantaneous

Solid fraction and energy increase depend linearly on density outside phase transition

Abstract

Condensation of H 2 in the interstellar medium (ISM) has long been seen as a possibility, either by deposition on dust grains or thanks to a phase transition combined with self-gravity. H 2 condensation might explain the observed low efficiency of star formation and might help to hide baryons in spiral galaxies. Our aim is to quantify the solid fraction of H 2 in the ISM due to a phase transition including self-gravity for different densities and temperatures in order to use the results in more complex simulations of the ISM as subgrid physics. We used molecular dynamics simulations of fluids at different temperatures and densities to study the formation of solids. Once the simulations reached a steady state, we calculated the solid mass fraction, energy increase, and timescales. By determining the power laws measured over several orders of magnitude, we extrapolated to lower densities the higher density fluids that can be simulated with current computers. The solid fraction and energy increase of fluids in a phase transition are above 0.1 and do not follow a power law. Fluids out of a phase transition are still forming a small amount of solids due to chance encounters of molecules. The solid mass fraction and energy increase of these fluids are linearly dependent on density and can easily be extrapolated. The timescale is below one second, the condensation can be considered instantaneous. The presence of solid H 2 grains has important dynamic implications on the ISM as they may be the building blocks for larger solid bodies when gravity is included. We provide the solid mass fraction, energy increase, and timescales for high density fluids and extrapolation laws for lower densities.