than $\rho_0$ in pre-supernova matter.

Suppose that the phase transition condition is met, the energy budget problem for supernova explosions can be then naturally resolved[@bh89]. Because each nucleon contributes about 30 MeV energy during phase conversion[@cdwl98], the total released phase transition energy $E_{\rm pt}$ is then approximately $$E_{\rm pt} = M c^2 \times {30 \over 931}
\sim 5.8 \times 10^{52} {M\over M_{\odot}}~~{\rm ergs,}$$ where $M$ is the mass of the inner core. The timescale to burn a protoneutron star to a protostrange star, $\sim 10^{-4}$ s, is usually much smaller than that of neutrino diffusion and thermal evolution, $\sim 0.5$ s[@bet90], since the actual combustion could be in the detonation mode[@detonation] and the propagation velocity could be very probably close to the speed of light. Thus, the neutrino luminosity $L$ caused by this conversion could be estimated as about $E_{\rm pt}/0.5 \sim 10^{53}$ erg/s. In Wilson’s computations[@wil85bw85], the typical value of neutrino luminosity is $5\times 10^{52}$ erg/s, thus the total neutrino luminosity with the inclusion of SQM phase transition should be $1.5 \times 10^{53}$ erg/s ([*three*]{} times that of Wilson value). The simulated explosion energy should also be raised by a factor of three, which is 0.9-1.2 foe, adequate to 