The structure of atomic and molecular gas in the vicinity of the supernova remnant HB3

Details The structure of atomic and molecular gas in the vicinity of the supernova remnant HB3 The structure of atomic and molecular gas in the vicinity of the supernova remnant HB3

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...247..529r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 247, no. 2, July 1991, p. 529-544. Research supported by NSERC.

Astronomy and Astrophysics

Astronomy

32

Interstellar Matter, Molecular Gases, Radio Emission, Stellar Radiation, Supernova Remnants, Carbon Monoxide, H Lines, Radio Astronomy, Stellar Models

Scientific paper

The distribution of molecular gas near HB3 is examined by means of HI-line synthesis observations that are presented and with CO-12 emission maps, and the atomic and molecular gases of the region at the same velocity resolution are compared. The HI-line data suggest the existence of a shell, and about half of the emission is accelerated by about 20 km/s. The CO-12 data indicate interaction with HB3 because a CO-12 'bar' is surrounded by a region of enhanced radio continuum emission from the supernova remnant. Star formation in the region cannot be completely explained without considering the progenitor of HB3. Based on this supposition, a model is developed to describe the spatial features and gases associated with HB3 and W3. The supernova remnant is found to be one of the largest and most evolved, and comparisons with other remnants that have swept-up atomic gas confirms the highly evolved nature of the remnant.

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