  NGC 1068, a nearby type-2 Seyfert galaxy, is reported as the hottest neutrino
spot in the 10-year survey data of IceCube. Although there are several
different possibilities for the generation of high-energy neutrinos in
astrophysical sources, feasible scenarios allowing such emission in NGC 1068
have not yet been firmly defined. We show that the flux level of GeV and
neutrino emission observed from NGC 1068 implies that the neutrino emission can
be produced only in the vicinity of the supermassive black hole in the center
of the galaxy. The coronal parameters, such as magnetic field strength and
corona size, making this emission possible are consistent with the spectral
excess registered in the millimeter range. The suggested model and relevant
physical parameters are similar to those revealed for several nearby Seyferts.
Due to the internal gamma-ray attenuation, the suggested scenario cannot be
verified by observations of NGC 1068 in the GeV and TeV gamma-ray energy bands.
However, the optical depth is expected to become negligible for MeV gamma rays,
thus future observations in this band will be able to prove our model.
