Supernova models with slow energy pumping and galactic supernova remnants

Abstract

The study of supernova (SN) models with slow energy pumping is continued. At maximum luminosity the main characteristics of a SN are shown to be independent of the initial structure of the model (Table I, Figure 1). However, they depend on the massM e of the envelope, and on the intensity of energy pumpingL ɛ, with an increase ofM e leading qualitatively to the same changes in the SN parameters as a decrease inL ɛ (Table I, Figures 2 and 3). A simple relationship connecting the important SN parameters is obtained (Equation (6)). From the inflection of the color indexB-V curve, the possibility of deriving the characteristic time of energy pumping with intensityL ɛ ∼ 1044 erg s−1 is pointed out. The comparison of the extragalactic type I SN observations with the results of calculations leads to the estimate ofM e ≈ 0.3–0.7M⊙. An investigation of the galactic type I SN remnants is carried out (Table III). The estimate ofM e ≈ 0.2–0.3M ⊙ is obtained for the remnants of supernovae SN 1006, SN 1572, and SN 1604. It completely fits the results for the extragalactic type I SNs. The total initial mass of SN 1604 presupernova was shown to be at least about 7M ⊙. It was established that the Crab nebula resulted from the outburst of a peculiar SN. The unique properties of such SNs, including SN 1054, are due to the low intensity of energy pumping (L ⊙ ∼ 1042 erg s−1). The mass of the envelope of the Crab nebula is evaluated to beM e ≈ 0.7M ⊙. SN 1054 was shown to have m max v =−4 m . 0 at maximum luminosity.