Interstellar Chemistry: Radiation, Dust and Metals

Abstract

An overview is given of the chemical processes that occur in primordial systems under the influence of radiation, metal abundances and dust surface reactions. It is found that radiative feedback effects differ for UV and X-ray photons at any metallicity, with molecules surviving quite well under irradiation by X-rays. Starburst and AGN will therefore enjoy quite different cooling abilities for their dense molecular gas. The presence of a cool molecular phase is strongly dependent on metallicity. Strong irradiation by cosmic rays (>100x the Milky Way value) forces a large fraction of the CO gas into neutral carbon. Dust is important for H2 and HD formation, already at metallicities of 10^-4-10^-3 solar, for electron abundances below 10^-3.

arXiv commentInvited contribution to IAU Symposium 255 -- Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies

References in corpus (5)

• The Formation of the First Star in the Universe
• The Polytropic Equation of State of Interstellar Gas Clouds
• A semianalytical model for the observational properties of the dominant carbon species at different metallicities
• Molecular hydrogen formation on dust grains in the high redshift universe
• On the Detection of High Redshift Black Holes with ALMA through CO and H2 Emission