During the core bounce of a supernova collapse resonant active-to-active (ν_a →ν_a), as well as active-to-sterile (ν_a →ν_s) neutrino (ν) oscillations can take place. Besides, over this phase weak magnetism increases antineutrino (ν̅) mean free paths, and thus its luminosity. Because the oscillation feeds mass-energy into the target ν species, the large mass-squared difference between species (ν_a →ν_s) implies a huge amount of power to be given off as gravitational waves (L_GWs∼ 10^49erg

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... due to anisotropic but coherent ν flow over the oscillation length. This anisotropy in the ν-flux is driven by both the universal spin-rotation and the spin-magnetic coupling. The new spacetime strain estimated this way is still several orders of magnitude larger than those from ν diffusion (convection and cooling) or quadrupole moments of the neutron star matter. This new feature turns these bursts the more promising supernova gravitational-wave signal that may be detected by observatories as LIGO, VIRGO, etc., for distances far out to the VIRGO cluster of galaxies.