The remnant of Nova Cassiopeiae 1993 (V705 Cassiopeiae)

We have detected radio emission from the remnant of V705 Cas, beginning 221 d after visual maximum. We follow the remnant from first detection while still optically thick through the turn-over to optically thin emission, and finally confirming the absence of emission due to expansion and fading by t...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2000-11, Vol.318 (4), p.1086-1092
Main Authors: Eyres, S. P. S., Bode, M. F., O'Brien, T. J., Watson, S. K., Davis, R. J.
Format: Article
Language:English
Subjects:
cataclysmic variables
circumstellar matter
novae
novae, cataclysmic variables
radio continuum: stars
stars: individual: Nova Cassiopeiae 1993
stars: individual: V705 Cas
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Summary:We have detected radio emission from the remnant of V705 Cas, beginning 221 d after visual maximum. We follow the remnant from first detection while still optically thick through the turn-over to optically thin emission, and finally confirming the absence of emission due to expansion and fading by the end of 1998. While the emission is consistent with thermal bremsstrahlung, as seen in most previous novae, the small-scale structure shows two ridge-like features, which develop significantly from day 585 until our last detection on day 1544. While the development is fairly rapid, it is also much smoother than that seen in V1974 Cyg, in that we can follow individual features as they change over almost 1000 d. Our optical spectra unequivocally indicate some form of axial symmetry, as derived from the velocity structure. This is difficult to reconcile with the observed development in the radio images. We suggest a number of possible explanations.
ISSN:0035-8711
1365-2966
DOI:10.1046/j.1365-8711.2000.03767.x