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The failure of prompt explosion. Delayed explosion, or how to revive a stalled shock wave?

The failure of prompt explosion. Delayed explosion, or how to revive a stalled shock wave?. 1-D spherically symmetric collapse. let’s see the “movie”. H.-T. Janka, K. Langanke, A. Marek, G. Martnez-Pinedo and B. Muller Phys. Rept. 442 (2007) 38. The properties of the Neutrino flux.

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The failure of prompt explosion. Delayed explosion, or how to revive a stalled shock wave?

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  1. The failure of prompt explosion. Delayed explosion, or howto revive a stalled shock wave?

  2. 1-D spherically symmetric collapse let’s see the “movie” H.-T. Janka, K. Langanke, A. Marek, G. Martnez-Pinedo and B. Muller Phys. Rept. 442 (2007) 38

  3. The properties of the Neutrino flux Cumulative neutrino “light” curve (based on Nadyozhin 1978) Nonthermal e

  4. Liebendoerfer et al. 2003 Solid lines: 40 MSun progenetor dashed: 13 MSun progenetor

  5. The spectral properties of the Neutrino flux Total energyradiated. Characteristic time. Neutrino individual energies (ε). Neutrino flavors.

  6. Neutrino spectra for thermal phase Energy spectra. Fermi−Dirac law: High-energy cutoff (relevant to ):

  7. Core-collapse SNe (all other Types but Ia) The SN outburst is triggered by the gravitational collapse of the “iron” core of a mass MFe=(1.22) Minto a neutron star. About (1015)% MFec2is radiated in the form of neutrinos and antineutrinos of all the flavors (e, , ): The explosion energy (kinetic energy of the envelope expansion): Eexp = (0.52)1051erg it comes from the shock wave created at the boundary between a new-born neutron star and the envelope to be expelled. Rich nucleosynthesis — from neutrino-induced creation of light element in C-O and He shells through synthesis of heavy nuclides by neutron capture at the bottom of expelled envelope

  8. Delayed explosion Wilson J R (1985)Numerical Astrophysics (Boston: Jones and Barlett)

  9. The mechanism of the core-collapse SNe is still under detailed study Spherically-symmetrical collapse. An empiricaltheorem: Spherically-symmetrical models do not result in expulsion of an envelope; the SN outburst does not occur: the envelope falls back on the collapsed core. Corollary: One has to address to 2- and, perhaps, 3-dimensional models to convert the stalled accreting shock into an outgoing blast wave.

  10. Neutrino-convective mechanism of supernova explosion

  11. Convective instability criterion  A Chemically uniform medium is convectively unstable, if  > A For non-uniform media  > A+ 

  12. NEUTRINO-CONVECTIVE MECHANISM 150 и 300 ms after bounce Convective instability condition Liebendoerfer (2011) 10^4

  13. Dynamics of gravitational collapse Expulsion of supernova envelope (how?) neutrinosphere

  14. Janka (2001)

  15. 3-D simulations:

  16. J.M. Blondin, A. Mezzacappa “Pulsar spins from an instability in the accretion shock of SN”

  17. From astrophysical complexity to thesimplicity of a water fountain Foglizzo et al 2018

  18. O’Connor E, Couch S. (2015) A. Marek and H.-T. Janka

  19. Schematic Supernova «light curves»

  20. The failure of prompt explosion. Delayed explosion, or how to revive a stalled shock wave? SN1987A – the only supernova with neutrino signal detected Janka et al, Prog. Theor. Exp. Phys. (2012)

  21. SN1987A – the only supernova with neutrinosignal detected

  22. SN 1987А Image from skyandtelescope.com

  23. Small Magellanic Cloud Milky Way Large Magellanic Cloud Southern Cross SN1987A 23.02.1987 Cerro Tollolo Inter-american Observatory, Chile

  24. The star that exploded on February 23 in the Large Magellanic Cloud (the progenitor of supernova 1987A) has now been identified. It was catalogued by in 1969 as an OB star of 12th magnitude and given the designation Sanduleak-69 202. Observations at the European Southern Observatory in the mid-1970's allowed to classify it as of spectral type B3 I, that is a very hot, supergiant star.Credit:ESO

  25. SN1987A ring evolution

  26. Signals from SN1987A on 23 Feb.1987: Kamioka • water Cerenkov • 2140 tons fiducial • threshold ~6 MeV • 12 events in 12.4 sec. All three detectors saw a cluster ofevents at ~7:35 UT Baksan • 330 tons liquid scint • threshold ~10 MeV • 5 events in 9.1 sec. IMB • water Cerenkov • 5000 tons fiducial • threshold 20 MeV • 8 events in 6 seconds

  27. Baksan Underground Scintillation Telescope 31

  28. +4 +6 +8 +10 +12 Shelton mv McNaught SN 1987А Jones Discovery Mont Blanc Kamioka, IMB, Baksan Radio (21cм) Sk – 69o202 Shelton Feb23 Feb24 Feb25 0h 2h52m 7h36m 9h22m 15h54m

  29. Detection efficiency Kotake et al (2006)

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