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Effect of collective neutrino oscillations on the neutrino mechanism of core-collapse supernovae



Effect of collective neutrino oscillations on the neutrino mechanism of core-collapse supernovae



Monthly Notices of the Royal Astronomical Society 425(2)



In the seconds after collapse of a massive star, the newborn protoneutron star (PNS) radiates neutrinos of all flavours. The absorption of electron-type neutrinos below the radius of the stalled shockwave may drive explosions (the neutrino mechanism ). Because the heating rate is proportional to the square of neutrino energy, flavour conversion of ? and ? neutrinos to electron-type neutrinos via collective neutrino oscillations (C?O) may in principle increase the heating rate and drive explosions. In order to assess the potential importance of C?O for the shock revival, we solve the steady-state boundary value problem of spherically symmetric accretion between the PNS surface (r?) and the shock (rS), including a scheme for flavour conversion via C?O. For a given r?, PNS mass (M), accretion rate (M?) and assumed values of the neutrino energies from the PNS, we calculate the critical neutrino luminosity above which accretion is impossible and explosion results. We show that C?O can decrease the critical luminosity by a factor of at most ?1.5, but only if the flavour conversion is fully completed inside rS and if there is no matter suppression. The magnitude of the effect depends on the model parameters (M, M? and r?) through the shock radius and the physical scale for flavour conversion. We quantify these dependencies and find that C?O could lower the critical luminosity only for small M and M?, and large r?. However, for these parameter values C?O are suppressed due to matter effects. By quantifying the importance of C?O and matter suppression at the critical neutrino luminosity for explosion, we show in agreement with previous studies that C?O are unlikely to affect the neutrino mechanism of core-collapse supernovae significantly.

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Accession: 036543538

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DOI: 10.1111/j.1365-2966.2012.21443.x


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