The Molecular Hydrogen Deficit in Gamma-Ray Burst Afterglows

TL;DR

This study investigates why molecular hydrogen is absent in gamma-ray burst afterglows despite conditions that should favor its presence, using advanced radiation hydrodynamical models to explore environmental effects.

Contribution

The paper introduces comprehensive radiation hydrodynamical models that include radiative transfer, chemistry, and dust effects to explain H$_2$ suppression in GRB environments.

Findings

GRB progenitors ionize hydrogen out to 50-100 pc

Galactic Lyman-Werner background dissociates H$_2$ in the ISM

H$_2$ destruction depends on ambient density and metallicity

Abstract

Recent analysis of five gamma-ray burst (GRB) afterglow spectra reveal the absence of molecular hydrogen absorption lines, a surprising result in light of their large neutral hydrogen column densities and the detection of H$_2$ in similar, more local star-forming regions like 30 Doradus in the Large Magellanic Cloud (LMC). Observational evidence further indicates that the bulk of the neutral hydrogen column in these sight lines lies 100 pc beyond the progenitor and that H$_2$ was absent prior to the burst, suggesting that direct flux from the star, FUV background fields, or both suppressed its formation. We present one-dimensional radiation hydrodynamical models of GRB host galaxy environments, including self-consistent radiative transfer of both ionizing and Lyman-Werner photons, nine-species primordial chemistry with dust formation of H$_2$, and dust extinction of UV photons. We find that a single GRB progenitor is sufficient to ionize neutral hydrogen to distances of 50 - 100 pc but that a galactic Lyman-Werner background is required to dissociate the molecular hydrogen in the ambient ISM. Intensities of 0.1 - 100 times the Galactic mean are necessary to destroy H$_2$ in the cloud, depending on its density and metallicity. The minimum radii at which neutral hydrogen will be found in afterglow spectra is insensitive to the mass of the progenitor or the initial mass function (IMF) of its cluster, if present.