Volume 398, Number 2, February I 2003
|Page(s)||621 - 630|
|Section||Interstellar and circumstellar matter|
|Published online||21 January 2003|
Gas-phase recombination, grain neutralization and cosmic-ray ionization in diffuse gas
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
Corresponding author: email@example.com
Accepted: 12 November 2002
Atomic ions are mostly neutralized by small grains (or PAH molecules) in current theories of heating and cooling in cool diffuse clouds; in the main they do not recombine with free electrons. This alters the ionization balance by depressing n(H+) and n(He+) while carbon generally remains nearly fully once-ionized: charge exchange with atomic oxygen and formation of H2 and OH also depress n(H+) in partly molecular gas. Seemingly restrictive empirical limits on are relaxed and higher values for are favored in a wide range of circumstances, when grain neutralization is recognized. Maintenance of the proton density at levels needed to reproduce observations of HD requires s-1, but such models naturally explain the presence of both HD and H3p in relatively tenuous H I clouds. In dense gas, a higher ionization rate can account for high observed fractions of atomic hydrogen, and recognition of the effects of grain neutralization can resolve a major paradox in the formation of sulfur-bearing compounds.
Key words: ISM: general / ISM: cosmic rays / ISM: atoms / ISM: molecules
© ESO, 2003
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