Neutrino Oscillations at Supernova Core Bounce Generate the Strongest Gravitational-Wave Bursts

During the core bounce of a supernova collapse resonant active-to-active ($ν_a \to ν_a$), as well as active-to-sterile ($ν_a \to ν_s$) neutrino ($ν$) oscillations can take place. Besides, over this phase weak magnetism increases antineutrino ($\barν$) 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 ($ν_a \to ν_s$) implies a huge amount of power to be given off as gravitational waves ($L_{\textrm{GWs}} \sim 10^{49}erg s$^{-1}$), due to anisotropic but coherent$ν$flow over the oscillation length. This anisotropy in the$ν$-flux is driven by both the {\it universal spin-rotation} and the spin-magnetic coupling. The new spacetime strain estimated this way is still several orders of magnitude larger than those from$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.

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