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The Atomic to Molecular Transition in the Interstellar MediumStudy of H2 in UV and IR continues to surprise us with complexity of excitation state, OPR, and role in astrochemistry. Atomic H in molecular clouds is a very powerful tool suggesting that they are not "young" but that it takes millions of years to convert primarily atomic hydrogen clouds to 99.9% molecular form. Laboratory data suggests that H2 formation is efficient over broader range of temperatures than thought to be the case a few years ago, but range is still limited. Issues of complex grain morphology and surface structure make this a very difficult field in which to obtain definitively meaningful results. Ongoing and future observations of CI and CII will improve our understanding of the structure of clouds, their total mass, and how they have evolved and will continue to do so.
Document ID
20130009319
Acquisition Source
Jet Propulsion Laboratory
Document Type
Presentation
External Source(s)
Authors
Goldsmith, Paul F.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA, United States)
Date Acquired
August 27, 2013
Publication Date
April 3, 2012
Subject Category
Astrophysics
Meeting Information
Meeting: Astrophysics Seminar
Location: Seoul
Country: Korea, Republic of
Start Date: April 3, 2012
Distribution Limits
Public
Copyright
Other
Keywords
interstellar medium
atomic hydrogen
molecular hydrogen

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