Other
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........15c&link_type=abstract
Thesis (PH.D.)--THE UNIVERSITY OF TEXAS AT AUSTIN, 1995.Source: Dissertation Abstracts International, Volume: 56-10, Section: B,
Other
4
Helium Lines
Scientific paper
Five studies concerning mainly the hybrid type SN 1993J, the Type Ib SN 1983N, and the Type Ic SNe 1983V, 1994I and 1987M are presented, together with less profound analyses of the Type Ic SNe 1962L, 1983I, 1988L, 1990B, 1990U. We study the very early spectrophotometric evolution of SN 1993J, measure its intrinsic flux, color temperature and foreground extinction in a self consistent manner, and obtain constraints on the size of the progenitor star, and early temperature and velocity evolution. We present spectra of SN 1994I and analyze the evidence for He in the optical wavelength region finding that, contrary to earlier interpretation, Type Ic SNe contain small amounts of He expanding at high velocity. We present the late time light curve of the Type Ib SN 1983N and show that, both from the photometric and photospheric velocity evolution, this SN was very similar to SN 1993J. We present a detailed study of the Type Ic SN 1983V, thoroughly discuss its photometric and spectroscopic characteristics and find that it followed a light curve very similar to that of SN 1993J, as well. We finally present a comparative analysis of seven Type Ic SNe and find that, in spite of their very similar spectra and spectroscopic evolution, the light curves of some of them are probably faster than that of a Type Ia SNe while those of some others are similar to the light curve of SN 1993J. The objects of Type Ib/c whose light curves are similar to those of SN 1993J, together with the spectroscopic links connecting them, lead us to the concept of Transition Type SNe, a group of SNe which do not share the spectroscopic class but have very similar inner structure as revealed by the similar photometric behavior. This group poses a controversy: They have similar light curves but different mass to energy ratio. We conclude that, in this group of SNe at least, the late time light curves are not determined by the total mass of the ejecta but by the deposition function in substructures (or inclusions) which do not follow a homologous spherical expansion.
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