Uncertainties in H2 and HD chemistry and cooling and their role in early structure formation

• Published in: Monthly notices of the Royal Astronomical Society Vol. 388; no. 4; pp. 1627 - 1651
• Main Authors: Glover, S. C. O., Abel, T.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Publishing Ltd 01-08-2008; Blackwell Science; Oxford University Press
• Subjects: Astronomy; Astrophysics; Cooling; Cosmology; cosmology: theory; Earth, ocean, space; Exact sciences and technology; Hydrogen; molecular data; molecular processes; Star & galaxy formation; stars: formation; molecular processes; stars: formation; molecular data; cosmology: theory; Molecular process; Protons; Turbulent heating; Uncertainty; Cooling rate; Cosmic background radiation; Molecular gas; Fragmentation; Population III; Hydrogen deuteride; Atom collisions; Star formation; Thermal evolution; Gravitational collapse; Cosmology; Excitation; Hydrogen molecules; Timing; Low temperature
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2008.13224.x

At low temperatures, the main coolant in primordial gas is molecular hydrogen, H2. Recent work has shown that primordial gas that is not collapsing gravitationally but is cooling from an initially ionized state forms hydrogen deuteride, HD, in sufficient amounts to cool the gas to the temperature of the cosmic microwave background. This extra cooling can reduce the characteristic mass for gravitational fragmentation and may cause a shift in the characteristic masses of Population III stars. Motivated by the importance of the atomic and molecular data for the cosmological question, we assess several chemical and radiative processes that have hitherto been neglected: the sensitivity of the low-temperature H2 cooling rate to the ratio of ortho-H2 to para-H2, the uncertainty in the low-temperature cooling rate of H2 excited by collisions with atomic hydrogen, the effects of cooling from H2 excited by collisions with protons and electrons, and the large uncertainties in the rates of several of the reactions responsible for determining the H2 fraction in the gas.
It is shown that the most important of neglected processes is the excitation of H2 by collisions with protons and electrons. Their effect is to cool the gas more rapidly at early times, and consequently to form less H2 and HD at late times. This fact, as well as several of the chemical uncertainties presented here, significantly affects the thermal evolution of the gas. We anticipate that this may lead to clear differences in future detailed three-dimensional studies of first structure formation. In such calculations it has previously been shown that the details of the timing between cooling and merger events decide between immediate runaway gravitational collapse and a slower collapse delayed by turbulent heating.
Finally, we show that although the thermal evolution of the gas is in principle sensitive to the ortho-para ratio, in practice the standard assumption of a 3:1 ratio produces results that are almost indistinguishable from those produced by a more detailed treatment.