1998/09/16 by Isabel Salamanca, I. Salamanca, R. Cid Fernandes +8 · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Emission spectrum #Gamma-ray bursts and supernovae #Physics #Spectral line #Spectroscopy #Star (game theory) #Supernova #Supernova remnant #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.1998.02093.x
10 pages, 2 figures, acepted for publication in MNRAS. Uses referee.sty, psfig.sty and mn.sty. A postscript file can also be retrieved at http://www.strw.LeidenUniv.nl/~salamanc/latest.html
arxiv created 1998/09/16 · openalex publication_date 1998/10/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report the detection of the slow-moving wind into which the compact supernova remnant SN 1997ab is expanding. Echelle spectroscopy provides clear evidence for a well-resolved narrow (full width at zero intensity, FWZI ∼180 km s−1) P Cygni profile, both in Hα and Hβ, superimposed on the broad emission lines of this compact supernova remnant. From theoretical arguments we know that the broad and strong emission lines imply a circumstellar density (n ≥ 107 cm−3). This, together with our detection, implies a massive and slow stellar wind experienced by the progenitor star shortly prior to the explosion.