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Unusual SN explosion mechanisms

Explore the intriguing mechanisms behind supernova explosions, including neutrino-driven convection, rotation, and magnetic fields, leading to the formation of neutron star binaries and gravitational wave emissions.

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Unusual SN explosion mechanisms

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  1. Unusual SN explosion mechanisms

  2. The mechanism of the collapsed-core SN is still under detailed study An empirical theorem: spherically-symmetrical models do not result in expulsion of envelope; the SN outburst does not occur: the envelope falls back on the collapsed core. One has to go in 2- and, perhaps, 3-dimensional models to convert the stalled accreting shock into an outgoing blast wave.  Large-scale neutrino-driven convection A. Burrows’ group (Arisona); E. Müller, T. Janka (MPA, Garching)  Interaction between rotation and magnetic field G.S. Bisnovatyi-Kogan’s group (SRI, Keldysh IPM, Moscow)  Massivefast-rotating collapsed core followed by rotational fission resulting in formation of a close neutron-star binary that evolves being driven by the emission of gravitational waves and mass-exchange and ends with the explosion of a low-mass neutron star (M0.1M). V.S. Imshennik (Alikhanov ITEP, Moscow)

  3. MAGNETO-ROTATIONAL MECHANISM G. Bisnovatiy-Kogan 1-D calculations of magnetorotational explosion

  4. SN1987А

  5. On the Event Observed in the Mont Blanc Underground Neutrino Observatory during the Occurrence of Supernova 1987a M. Aglietta, G. Badino, G. Bologna, C. Castagnoli, A. Castellina, V. L. Dadykin, W. Fulgione, P. Galeotti, F. F. Kalchukov, B. Kortchaguin, P. V. Kortchaguin, A. S. Malguin, V. G. Ryassny, O.G. Ryazhskaya, O. Saavedra, V. P. Talochkin, G. Trinchero, S. Vernetto, G. T. Zatsepin and V. F. YakushevEuroPhys. Lett. 3  (1987) 1315 LSD • 90 tons liquid scintilator • 220 tons Fe • threshold ~ 5 MeV • 5 events in 7 sec – 2:52 • 2 ev. In 18 sec. – 7:36 Liquid Scintillation Detector, Italy, Mont Blanc 3 of them in the 16 internal tanks, 2 in the 56 external tanks 90 т СnH2n 200 т Fe

  6. O.G. Ryazhskaya, UFN 176, №10, 2006

  7. LSD

  8. H=5200 m.w.e. 72 counters 90 tons of CnH2n 200 tons of Fe Aglietti et al. 1988

  9. Rotational breakup – neutron star explosion scenario Imshennik, Sov. Astron. Lett. 18, 194 (1992)

  10. Fast Facts for RX J0822-4300 in Puppis A:

  11. Birth of neutron star during CCSNThe properties of neutron stars

  12. Adapted from D.G. Yakovlev

  13. Shen, Toki, Oyamatsu, Sumiyoshi

  14. Tolman Oppenheimer Volkoff (TOV) equations

  15. Maximum neutron starmass J.M. Lattimer Annual Review of Nuclear and Particle Science, vol. 62, issue 1, pp. 485-515 (2012)

  16. Rhoades and Ruffini 1974 Hartle 1978 Kalogera and Baym 1996 Glendenning 1999

  17. Neutron star, quark star or hybrid?

  18. Schertler, Greiner, Schaffner-Bielich and Thoma

  19. Composition of a Neutron Star

  20. Signals of the QCD Phase Transition in CCSN Gagert, Fisher, Pagliara, Schaffner-Bielich, Mezzacappa, Thielemann, Liebendoerfer

  21. Fischer, Bastian, Wu, Baklanov, Sorokina, Blinnikov, Typel, Klahn, Blaschke

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