By J.M. Marcaide, Kurt Weiler
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Extra resources for Cosmic Explosions: On the 10th Anniversary of SN1993J (IAU Colloquium 192) (Springer Proceedings in Physics)
2. Intensity proﬁle (continuous line) corresponding to an azimuthal average of the brightness distribution due to a shell of ﬂat radial emission proﬁle (lightshaded) and ﬁnite width (30% of outer radius) and reconstructed emission proﬁle (dark-shaded) using GFD. No noise has been added to the synthetic data which produce the brightness distribution. The residuals of the GFD (dashed line) are almost zero, as expected. The beam sizes used also correspond to 30% of the outer radius. Fig. 3. Same as Fig.
Fig. 1. 7 and 22 GHz. The angular outer radii, θo , are derived from a spherical shell model ﬁt directly to the u-v data. The inset shows outer radii for the latest epochs in more detail. 781 at t ∼ 600 d. A further change in the index is visible in the inset (see  for more detail). and then decreases again. For details and the interpretation of this behavior we refer the reader to . 0 GHz in Fig. 2 (see [1, 4] for more images). The shell structure ﬁrst becomes visible at t = 175 d. Already at this stage the brightness was modulated around the ridge, with a distinct minimum to the west and a maximum to the eastsouth-east.
Lett. W. A. D. van Dyk, N. 03 light yr a) Discovery of shell−like radio structure in a) Discovery of shell−like radio structure in SN 1993J. False− SN 1993J. 6cm VLBI obtained observations after explosion. days after explosion. 373, 1995, (From Marcaide et al. (Marcaide (1995), Nature 44)Nature 373, 44) b) Sequence of images of SN 1993J from VLBI observations observations 330, 427,VLBI and 541 days after b) Sequence ofobtained images 182, of SN239, 1993J from the explosion. 6 cm data. The image on day 541 was obtained from days after the explosion.
Cosmic Explosions: On the 10th Anniversary of SN1993J (IAU Colloquium 192) (Springer Proceedings in Physics) by J.M. Marcaide, Kurt Weiler