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Neutrino oscillations at supernova core bounce generate the strongest gravitational-wave bursts

Jul, 2004
10 pages
Published in:
  • Int.J.Mod.Phys.D 13 (2004) 1297-1308
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20072008200901
Abstract: (arXiv)
During the core bounce of a supernova collapse resonant active-to-active (νa→νa\nu_a \to \nu_a), as well as active-to-sterile (νa→νs\nu_a \to \nu_s) neutrino (ν\nu) oscillations can take place. Besides, over this phase weak magnetism increases antineutrino (νˉ\bar{\nu}) mean free paths, and thus its luminosity. Because the oscillation feeds mass-energy into the target ν\nu species, the large mass-squared difference between species (νa→νs\nu_a \to \nu_s) implies a huge amount of power to be given off as gravitational waves (LGWs∼1049ergsL_{\textrm{GWs}} \sim 10^{49}erg s^{-1}),duetoanisotropicbutcoherent), due to anisotropic but coherent \nuflowovertheoscillationlength.Thisanisotropyinthe flow over the oscillation length. This anisotropy in the \nu−fluxisdrivenbyboththeuniversalspin−rotationandthespin−magneticcoupling.Thenewspacetimestrainestimatedthiswayisstillseveralordersofmagnitudelargerthanthosefrom-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 \nu$ 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.
  • Elementary particles
  • neutrino
  • gravitational waves
  • supernova
  • talk: Olinda 2003/10/12
  • neutrino: oscillation
  • neutrino: sterile
  • supernova
  • neutrino: mass difference
  • neutrino: flux