Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...399..563b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 2, p. 563-572.
Astronomy and Astrophysics
Astronomy
103
Emission Spectra, H Lines, Interstellar Gas, Photodissociation, Rotational Spectra, Hydrogen, Infrared Astronomy, Shock Waves
Scientific paper
The line emission from the v = 0-0 S(0), S(2), and S(3), and the v = 1-0 and v = 2-1 S(1) transitions of molecular hydrogen in clouds exposed to high FUV fluxes and in shocks is modeled. Particular attention is given to the lowest pure rotational H2 transitions at 20 and 17 microns, respectively. It is found that, in photodissociation regions (PDRs), the emission comes from warm (greater than about 100 k) molecular gas, situated at optical depths greater than about 1, beyond the hot atomic surface layer of the clouds. For FUV fields, G0 = 1000 to 100,000 times the average interstellar field densities n = 10 exp 3 - 10 exp 7/cu cm, the typical line intensities are in the range 10 exp -6 to 10 exp -4 ergs/s sq cm sr. The predictions for the line intensities from both C-type and J-type shock models are compared. The results are applied to recent observations of the 0-0 S(1) transition in both the PDR and the shocked gas in Orion.
Burton Michael G.
Hollenbach David J.
Tielens Alexander G.
No associations
LandOfFree
Mid-infrared rotational line emission from interstellar molecular hydrogen does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Mid-infrared rotational line emission from interstellar molecular hydrogen, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Mid-infrared rotational line emission from interstellar molecular hydrogen will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1551744