Astronomy and Astrophysics – Astrophysics
Scientific paper
2001-11-14
Mon.Not.Roy.Astron.Soc. 330 (2002) 473
Astronomy and Astrophysics
Astrophysics
9 pages, 6 figures. MNRAS, accepted. Typos added, acknowledgments corrected
Scientific paper
10.1046/j.1365-8711.2002.05086.x
Modelling of high resolution Balmer line profiles in the early-time spectra of SN 1998S shows that the inferred fast (roughly 400 km/s) circumstellar (CS) gas on days 23 and 42 post-explosion is confined to a narrow, negative velocity gradient shell just above the photosphere. This gas may be identified with a slow (v < 40 km/s) progenitor wind accelerated at the ejecta-wind interface. In this scenario, the photosphere coincides with a cool dense shell formed in the reverse shock. Acceleration by radiation from the supernova or by a shock-accelerated relativistic particle precursor are both possible explanations for the observed fast CS gas. An alternative, equally plausible scenario is that the fast CS gas is accelerated within shocked clouds engulfed by the outer shock, as it propagates through the intercloud wind.
Blinnikov Sergei I.
Chugai Nikolai
Fassia Alexandra
Lundqvist Peter
Meikle W. P. S.
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