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Extra info for Cosmic Explosions: On the 10th Anniversary of SN1993J (IAU Colloquium 192)
E. Conway8 1 2 3 4 5 6 7 8 York University, Canada National Radio Astronomy Observatory, USA CARMA, Owens Valley Radio Observatory, USA Max-Planck-Institut f¨ ur Radioastronomie, Germany Jet Propulsion Laboratory, Caltech, USA Instituto di Radioastonomia, CNR, Italy York University & Space Geodynamics Lab/CRESTech, Canada Onsala Space Observatory, Sweden Summary. We present a selection of our VLBI images of SN 1993J, along with our latest results on its expansion and its shell structure. 1 Introduction Supernova 1993J is the most comprehensively monitored radio supernova to date.
A schematic of the shell emission and the central absorption, the generated intensity proﬁle and the deconvolved emission proﬁle. The schematic of the central absorption in Fig. 4 indicates a complete blockage of the emission from the rear side of the shell for the extent of the drawing. The residuals are small everywhere, as before, but in the central region. These large central region residuals indicate the presence of the central absorption, as indeed we know is the case in this simulation. As it can be seen in Fig.
In preparation). It is quite clear that at late times, the emission is almost entirely coming from the shock interaction between the ejecta and circumstellar gas. The model ﬁt to the observed spectrum is quite good, and its total luminosity is ﬁxed by the observed X-ray emission from the shock – it is not a free parameter. Moreover, the detailed line proﬁles show that the emission is coming from a ﬁnite shell rather than a centrally peaked distribution of gas. There are strong, broad emission lines of N II], N III], and N IV], but only weak lines of C III] and C IV — characteristic of CNO processing.