Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...250..475i&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 2, Oct. 1991, p. 475-483.
Astronomy and Astrophysics
Astrophysics
17
H Ii Regions, Magellanic Clouds, Molecular Excitation, Shock Wave Interaction, Wave Excitation, Infrared Spectroscopy, Line Shape, Molecular Clouds, Near Infrared Radiation, Stellar Mass Ejection
Scientific paper
Various H2 transitions were observed in five objects in the SMC in order to identify the H2 excitation mechanism. Observed line ratios indicate that N83B and N81 are radiatively excited. The remaining objects either contain a shock-excited H2 component or have densities sufficiently high that collisional de-excitation influences observed line ratios. In both cases, radiative excitation is the energetically dominant mechanism in all objects. For the observed H2 clouds, volume densities of 200-10,000/cu cm are derived, with a mean of 5000/cu cm. If significant subparsec clumping occurs, densities may be higher. Limits on shock contributions to the observed H2 emission suggest shock velocities less than 10 km/s (J-type shocks) or less than 15-23 km/s (C-type shocks). It is inferred from this that early-type stars in the observed objects have stellar winds weaker than Galactic O-type stars. The strength of the observed near-IR He I transitions is briefly discussed.
Israel Frank P.
Koornneef Jan
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