Competing mechanisms in molecular hydrogen formation on silicates in conditions relevant to the interstellar medium (up to 70K)

Details Competing mechanisms in molecular hydrogen formation on silicates in conditions relevant to the interstellar medium (up to 70K) Competing mechanisms in molecular hydrogen formation on silicates in conditions relevant to the interstellar medium (up to 70K)

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.230l&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

The most efficient mechanism of molecular hydrogen formation in the universe is by association of H-atoms on the surface of interstellar dust grains. The details of its formation and release processes from the grain are of paramount importance in the physical/chemical evolution of the space environments where it happens. The fate of the 4.5eV released in H2 formation is still puzzling: does it go into internal energy/translational-kinetic-energy/grain heating? The modality of this energy release affects the ISM dynamics and evolution towards stellar formation. We present results of the detection of the ro-vibrational states of the just-formed H2 as it leaves a silicate surface. We find, using REMPI-TOF, that excited molecules are ejected into the gas phase immediately after formation over a much wider range of grain temperature than anticipated. Our results can be explained by the presence of two formation mechanisms operating in partially overlapping ranges of grain temperature, one of them being active up to 70K. Some results concerning the o/p ratio after molecular hydrogen formation will also be presented.

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