H2 in interstellar and extragalactic ices:  infrared characteristics, ultraviolet production, and implications.
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 H20-rich ices can be detected by an infrared absorption band at 4137 cm-1 (2.417 micrometers).  The surface binding energy of H2 to H2O ice was measured to the delta Hs/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.
Sandford
S A
SA
NASA/Ames Research Center, Moffett Field, CA 94035, USA.
Allamandola
L J
LJ
D005118:Extraterrestrial Environment; D006859:Hydrogen / Q000737:chemistry*; D007053:Ice / Q000032:analysis*; D000432:Methanol / Q000737:chemistry; D008956:Models, Chemical; D010782:Photolysis; D013055:Spectrophotometry, Infrared; D014466:Ultraviolet Rays; D014867:Water / Q000737:chemistry
D007053:Ice; D014867:Water; D006859:Hydrogen; D000432:Methanol