Sverkhnovaya 1987A v Bol'shom Magellanovom Oblake: nablyudeniya i teoriya

Neutrino mass problem: the state of the art

“…The explosion of the Supernova 1987A was registered on the night of February 23 ± 24, 1987, at the Las Campanas Observatory in Chile operated by Toronto University (Canada) and was then studied in many observatories [16,82]. At approximately the same time, the researchers at four neutrino laboratories registered 29 neutrino events that could be attributed to the interactions of the neutrinos produced as results of the collapse of this star.…”

“…Among the reviews close to the topics of the various sections in this paper we point out those by Zatsepin and Smirnov [5] and Muto and Klapdor [6] (the general properties of neutrinos), Gelmini and Roulet [7] and Boehm and Vogel [8] (neutrino masses), Wojcicki [9] (neutrino oscillations and the masses of n m and n t ), Moe and Vogel [10,11] and Shchepkin [12] (double beta decay), Borovo|¯and Khakimov [13] (experiments with reactor neutrinos), Weinheimer et al [14] and Belesev et al [15] (the mass of n e ), and Imshennik and Nadezhin [16] (Supernova 1987A). The values of some quantities are those accepted as of April 1997.…”

“…The estimate involved is based on the assumption that the duration of the neutrino signal in the collapse of the star was Of the other results obtained in the studies of the SN 1987A burst [16] we must mention the estimate of the neutrino electric charge q ne`1 0 À17 e and the bound on the magnetic moment, m ne 4 10 À14 À10 À12 m B , where m B is the electron Bohr magneton.…”

“…In Imshennik and Nadezhin's review [16], devoted to SN 1987A, there appears an estimate of the upper bound on the neutrino mass obtained from the data on the neutrino signal from the burst of this supernova:…”

The magnetospheric flare on compact magnetized object (neutron star or white dwarf)model for cosmological gamma-ray burst (GRB)

“…The system consists of a blue giant -supernova progenitor ( M = 20M , R = 50R ) and a magnetized neutron star ( M = 1.4M , R = 10 6 cm, B = 10 12 Gauss ) or a magnetized white dwarf ( M 1M , R = 10 9 cm, B = 10 9 Gauss ). According to the review [3] the parameters of the shock are kinetic energy E kin 10 47 ergs, velocity u 4 · 10 9 cm/sec, density 10 −8 g/cm 3 10 16 protons/cm 3 , width h 10 9 cm.…”