Computer Science
Scientific paper
Jan 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005esasp.577..369h&link_type=abstract
In: Proceedings of the dusty and molecular universe: a prelude to Herschel and ALMA, 27-29 October 2004, Paris, France. Ed. by A
Computer Science
Molecular Hydrogen, Interstellar Dust, Grains, Grain Chemistry, Molecular Clouds
Scientific paper
The formation of molecular hydrogen in interstellar dust and molecular clouds is a key step towards formation of new stars and the development of molecular complexity. Since there is no known effective gas phase route for H2 formation in these regions it is the generally accepted view that H2 is formed on the surface of interstellar dust grains. During recent years laboratory experiments have lent further credence to this view by confirming that H2 can indeed be formed efficiently on various dust grain analog surfaces under interstellar conditions (Katz et al. 1999; Manico et al. 2001; Roser et al. 2002; Hornekaer et al. 2003). These experiments have aimed at identifying the formation mechanism and determining its efficiency, as well as determining how the 4.5 eV which is liberated in the formation process is distributed between grain surface heating and translational and ro-vibrational degrees of freedom of the formed molecule. In the present paper we will briefly review a series of experiments performed by the authors and reported on in Hornekaer et al. (2003) aimed at determining the influence of grain surface morphology on molecular hydrogen formation in the interstellar medium. Furthermore, we will examine the implications of surface morphology on the residence time of molecular hydrogen on grain surfaces.
Baurichter A.
Hornekaer Liv
Luntz A. C.
Petrunin V. V.
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