  We present magnetohydrodynamical simulations of a strong accretion onto
magnetized proto-neutron stars for the Kesteven 79 (Kes 79) scenario. The
supernova remnant Kes 79, observed with the Chandra ACIS-I instrument during
approximately 8.3 h, is located in the constellation Aquila at a distance of
7.1 kpc in the galactic plane. It is a galactic and a very young object with an
estimate age of 6 kyr. The Chandra image has revealed, for the first time, a
point-like source at the center of the remnant. The Kes 79 compact remnant
belongs to a special class of objects, the so-called Central Compact Objects,
which exhibits no evidence for a surrounding pulsar wind nebula. In this work
we show that the submergence of the magnetic field during the hypercritical
phase can explain such behavior for Kes 79 and others CCOs. The simulations of
such regime were carried out with the adaptive-mesh-refinement code FLASH in
two spatial dimensions, including radiative loss by neutrinos and an adequate
equation of state for such regime. From the simulations, we estimate that the
number of thermal neutrinos expected on the Hyper-Kamiokande Experiment is
733$\pm$364. In addition, we compute the flavor ratio on Earth for a progenitor
model.
