The HI environment of filled-centre supernova remnants. I. G 74.9+1.2.

Details The HI environment of filled-centre supernova remnants. I. G 74.9+1.2. The HI environment of filled-centre supernova remnants. I. G 74.9+1.2.

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...317..212w&link_type=abstract

Astronomy and Astrophysics, v.317, p.212-222

Astronomy and Astrophysics

Astrophysics

10

Supernovae: General, Ism: Bubbles, Ism: Individual Objects: G 74.9+1.2 (Snr 074.9+01.2), Ism: Supernova Remnants, Radio Continuum: Ism, Radio Lines: Ism

Scientific paper

We present the results of an investigation into the HI environment of the filled-centre supernova remnant (SNR) G 74.9+1.2 (CTB87). We confirm earlier results that G 74.9+1.2 lies within the boundaries of an expanding bubble in the HI distribution at the systemic velocity of the SNR. This bubble is defined by a partial HI shell which opens away from the Galactic plane. The north-west portion of G 74.9+1.2 lies adjacent to the inner boundary of the HI shell. The morphology of the HI boundary and the north-west edge of the SNR are similar, suggesting that the HI shell has impeded the expansion of the SNR in this direction. This result, together with the absence of a steep-spectrum synchrotron shell, rules out the presence of an invisible halo of fast moving ejecta, suggesting that the original supernova explosion did not have enough energy to form such a halo. We find that the observed morphology of G 74.9+1.2 can be explained if the kinetic energy of the nebula is comparable to that found in the Crab Nebula. This is roughly a factor of 30 less than the energy found in a shell SNR. This in turn suggests that the progenitors of filled-centre SNRs (and certainly G 74.9+1.2) may be inherently different from those of shell-type SNRs.

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