The interaction of the supernova remnant HB 21 with the interstellar medium - CO, H I, and radio continuum observations

Details The interaction of the supernova remnant HB 21 with the interstellar medium - CO, H I, and radio continuum observations The interaction of the supernova remnant HB 21 with the interstellar medium - CO, H I, and radio continuum observations

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...237..189t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 237, no. 1, Oct. 1990, p. 189-200. Research supported by the Japan Society for

Astronomy and Astrophysics

Astronomy

44

Interstellar Gas, Interstellar Magnetic Fields, Interstellar Matter, Supernova Remnants, Carbon Monoxide, Cygnus Constellation, Emission Spectra, Molecular Gases, Radio Astronomy

Scientific paper

The region of the shell SNR HB 21 has been observed in CO, H I, and the radio continuum. Features are found in the ISM with which the SNR is interacting. An interstellar gas wall consisting of atomic and molecular gas is considered to have caused the straight eastern boundary of the SNR by impeding the expansion of the blast wave. The interstellar gas wall is part of the warped gas disk, of the outer Galaxy. The molecular gas shows highly clumpy structure, whereas the atomic gas is distributed rather smoothly. Of the three observed CO clumps which are apparently located along the eastern boundary of HB 21, two are likely to be actually associated with this SNR. The radio continuum there is not particularly intense, although strong compression of magnetic fields is considered to have occurred. Since the interstellar gas associated with HB 21 probably belongs to the Cyg OB7 association, the distance to HB 21 is determined to be 800 + or - 70 pc.

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