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This paper provides collapses of massive, fully convective, and non-rotatingwhite dwarfs (WDs) formed by accretion-induced collapse or merger-inducedcollapse and the subsequent explosions with the general relativisticneutrino-radiation hydrodynamics simulations. We produce initial WDs inhydrostatic equilibrium, which have super-Chandrasekhar mass and are about tocollapse. The WDs have masses of 1.6$M_\odot$ with different initial centraldensities specifically at $10^{10}$, $10^{9.6}$, $10^{9.3}$ and $10^{9.0}\,{\rmg\,cm^{-3}}$. First, we check whether initial WDs are stable without weakinteractions. Second, we calculate the collapse of WDs with weak interactions.We employ hydrodynamics simulations with Newtonian gravity in the first andsecond steps. Third, we calculate the formation of neutron stars andaccompanying explosions with general relativistic simulations. As a result, WDswith the highest density of $10^{10}\,{\rm g\,cm^{-3}}$ collapse not by weakinteractions but by the photodissociation of the iron, and three WDs with lowcentral densities collapse by the electron capture as expected at the secondstep and succeed in the explosion with a small explosion energy of $\sim10^{48}$ erg at the third step. By changing the surrounding environment of WDs,we find that there is a minimum value of ejecta masses being $\sim10^{-5}M_{\odot}$. With the most elaborate simulations of this kind so far, thevalue is one to two orders of magnitude smaller than previously reported valuesand is compatible with the estimated ejecta mass from FRB~121102.

Gravitational Collapse of White Dwarfs to Neutron Stars. I. From Initial Conditions to Explosions with Neutrino-radiation Hydrodynamics Simulations