Abstract
It is generally thought that Type I supernovae are the outcome of the explosion of a massive white dwarf in a close binary system. The properties of the light curves as well as the Pskovskii-Branch effect suggest that such explosions should leave a bound remnant in some cases. This condition is naturally fulfilled by taking into account that the white dwarf may have a solid core and that the thermal runaway starts at the edge of this core. In this paper, observed light curves are compared with the theoretical ones obtained from the explosion of partially solid white dwarfs for a wide range of the relevant parameters. Our results show that the "slow" and "fast" character of the light curve depends basically on the expelled material (Mej) and on the fraction of this material that has not been processed to the nuclear statistical equilibrium (M6). The observations constrain these parameters to take values in the range 0.8 M⊙ < Mej < 1.4 M⊙ and 0.2 M⊙ <Mδ < 0.4 M⊙. A value of the Hubble constant H0 = 100 km 1 seems to be excluded for any reasonable choice of the relevant parameters of our models.
