H2 in interstellar and extragalactic ices - Infrared characteristics, ultraviolet production, and implications

Details H2 in interstellar and extragalactic ices - Infrared characteristics, ultraviolet production, and implications H2 in interstellar and extragalactic ices - Infrared characteristics, ultraviolet production, and implications

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...409l..65s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 409, no. 2, p. L65-L68.

Astronomy and Astrophysics

Astrophysics

57

Hydrogen, Ice, Infrared Spectra, Interstellar Gas, Interstellar Matter, Molecular Clouds, Abundance, Photolysis

Scientific paper

H2 is the most abundant molecule in the universe. We demonstrate that this molecule may be an important component of interstellar and possibly intergalactic ices, both because it can be formed in situ, within the ices, and because gas-phase H2 can freeze out onto dust grains in some astrophysical environments. The condensation-sublimation and infrared spectral properties of ices containing H2 are presented. We show that solid H2 in H2O-rich ices can be detected by an infrared absorption band at 4137/cm (2.417 microns). The surface binding energy of H2 to H2O ice was measured to be Delta-H(s)/k = 555 +/- 35 K. Surface binding energies can be used to calculate the residence times of H2 on grain surfaces as a function of temperature. Some of the implications of these results are considered.

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