2002/08/07 by M. F. Bietenholz, N. Bartel, M. P. Rupen · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Cosmic Phenomena #Brightness #Flux (metallurgy) #Gamma-ray bursts and supernovae #Nebula #Pulsar #RADIUS #Spiral galaxy #Supernova #Supernova remnant #Surface brightness #astro-ph
paper · pdf · doi:10.1086/344251
published as Astrophys.J. 581 (2002) 1132-1147 · 24 pages, 9 Figures, LaTeX Accepted for Publication in the Astrophysical Journal
arxiv created 2002/08/07 · openalex publication_date 2002/12/16 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We report on VLBI observations of supernova 1986J in the spiral galaxy NGC 891 at two new epochs, 1990 July and 1999 February, t = 7.4 and 15.9 yr after the explosion, respectively, and on a comprehensive analysis of these and earlier observations from t ~ 4 yr after the explosion date, which we estimate to be 1983.2 ± 1.1. The source is a shell or composite and continues to show a complex morphology with large brightness modulations along the ridge and with protrusions. The supernova is moderately to strongly decelerated. The average outer radius expands as t 0.71±0.11 , and the expansion velocity has slowed to 6000 km s -1 at t = 15.9 yr from an extrapolated 20,000 km s -1 at t = 0.25 yr. The structure changes significantly with time, showing that the evolution is not self-similar. The shell structure is best visible at the latest epoch, when the protrusions have diminished somewhat in prominence and a new, compact component has appeared. The radio spectrum shows a clear inversion above 10 GHz. This might be related to a pulsar nebula becoming visible through the debris of the explosion. The radio flux density between 1.5 and 23 GHz decreases strongly with time, with the flux density ∝ t -2.94±0.24 between t ~ 15 and 19 yr. This decrease is much more rapid than that found in earlier measurements up to t ~ 6 yr.