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It has recently been demonstrated analytically that the two-point correlationfunction for pairs of neutrinos may contain information about the size of theproto-neutron star formed in a Galactic core-collapse supernova. Theinformation about the size of the source emerges via the neutrino equivalent ofintensity interferometry originally used by Hanbury-Brown and Twiss withphotons to measure the radii of stars. However the analytic demonstration ofneutrino intensity interferometry with supernova neutrinos made a number ofapproximations: that the two neutrinos had equal energies, the neutrinos wereemitted at simultaneous times from two points and were detected simultaneouslyat two detection points that formed a plane with the emission points. Theseapproximations need to be relaxed in order to better determine the feasibilityof neutrino intensity interferometry for supernovae neutrinos in a morerealistic scenario. In this paper we further investigate the feasibility ofintensity interferometry for supernova neutrinos by relaxing all theapproximations made in the earlier study. We find that, while relaxing any oneassumption reduces the correlation signal, the relaxation of the assumption ofequal times of detection is by far the largest detrimental factor. For neutrinoenergies of order $\sim$15 MeV and a supernova distance of L = 10 kpc, we showthat in order to observe the interference pattern in the two-point correlationfunction of the neutrino pairs, the timing resolution of a detector needs to beon the order of $\lesssim 10^{-21}\;{\rm s}$ if the initial neutrino wavepacket has a size of $\sigma_x \sim 10^{-11}\;{\rm cm}$.

On The Feasibility Of Using Neutrino Intensity Interferometry To Measure Proto-Neutron Star Radii