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Supernovae as neutrino and gravitational wave sources

Cosmological Backgrounds of Neutrinos, Photons, And Gravitational Waves. Supernovae as neutrino and gravitational wave sources. G ü nter Sigl GReCO, Institut d’Astrophysique de Paris, CNRS et Fédération de Recherche Astroparticule et Cosmologie, Université Paris 7

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Supernovae as neutrino and gravitational wave sources

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  1. Cosmological Backgrounds of Neutrinos, Photons, And Gravitational Waves • Supernovae as neutrino and gravitational wave sources Günter Sigl GReCO, Institut d’Astrophysique de Paris, CNRS et Fédération de Recherche Astroparticule et Cosmologie, Université Paris 7 http://www2.iap.fr/users/sigl/homepage.html

  2. Onion structure of a supernova Janka, Mueller Convection, turbulence

  3. memory h(t) L(t) q(t) A rotating core collapse model by Müller & Janka Supernovae as Neutrino and Gravitational Wave Sources Anisotropic mass motion and neutrino emission in massive star collapse leads to gravitational wave emission. At low frequencies neutrino emission with luminosity Lν(t) and anisotropy q(t) dominates and leads to dimensionless strain at distance D:

  4. ≥100Msun PopIII 2x10-3 Msun in gw, <q>~3% ordinary SN 10-8 Msun in gw, <q>~0.5% gravitational wave spectra neutrino spectra Simulated individual signals Individual supernovae (SN) in our Galaxy can give prominent signals in neutrinos in Super-Kamiokande, Amanda, ICECUBE, Uno… and in gravitational waves in Virgo/EGO, LIGO…, but are RARE events.

  5. The background is then given by integration over all events The Gaussianity of the signal is given by the “duty factor” which is proportional to the event rate: Where τ(f) is the time scale over which frequency f is emitted “coherently” In a given event. For us: τ(f)~1/f

  6. However, backgrounds from cosmological SN may soon be detectable by gadolinium upgrade of Super-K in neutrinos and by gravitational wave detectors such as the Big Bang Observatory (BBO). Ordinary SN ~ 1/sec + very massive PopIII stars at z ≥ 15 with rate ~ 0.2 (fIII/10-3)/sec, where fIII= baryon fraction cycled thru PopIII stars. future input from SWIFT… SN rate

  7. => diffuse neutrino spectra from ordinary SN close to current sensitivities stochastic gravitational wave background Ando and Sato, astro-ph/0410061 Buonanno, Sigl, Raffelt, Janka, Mueller, Phys.Rev.D 72 (2005) 084001

  8. Pop III fraction of baryons fIIIand infrared background resulting from Lyα emission Madau, Silk., astro-ph/0502304 Dwek et al., astro-ph/0508262 Diffuse infrared background can not be explained by galaxies alone -> may need a Pop III contribution

  9. low metallicity: less cooling, larger progenitor masses, less mass loss, more powerful explosions. Fate of a massive star as function of progenitor mass and metallicity Heger et al., astro-ph/0211062

  10. Fate of a massive star as function of progenitor mass and metallicity Heger et al., astro-ph/0211062

  11. SN and PopIII Compare this with upper limits, sensitivities, and cosmological predictions BBO BBO correlated Giovannini

  12. Consequence: Gravitational Wave Background from type II supernovae and PopIII stars could mask inflationary background

  13. Conclusions There is a deep connection between neutrino and gravitational wave emission by collapsing massive stars. Both signals have good chances to be seen by future experiments.

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