The neutrino mass from the tritium beta spectrum in valine

Boris, S.; Golutvin, A.; Laptin, L.; Lubimov, V.; Nagovizin, V.; Novikov, E.; Nozik, V.Z.; Soloshenko, V.; Tihomirov, I.; Tretjakov, E.

doi:10.1016/0370-2693(85)90890-1

Cited by 48 publications

(2 citation statements)

References 4 publications

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Section: ¶ñóïâîëêï Aeëóâíñäôíñì ë ïâìñóâðñäôíñì ïâôô ðçìõóëðñunclassified

The nature of neutrino mass and the phenomenon of neutrino oscillations

Герштейн¹,

Kuznetsov²,

Ryabov³

1997

Успехи физических наук

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Section: ¶ñóïâîëêï Aeëóâíñäôíñì ë ïâìñóâðñäôíñì ïâôô ðçìõóëðñunclassified

The nature of neutrino mass and the phenomenon of neutrino oscillations

Герштейн¹,

Kuznetsov²,

Ryabov³

1997

Успехи физических наук

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“…In addition, since the neutrino mass is not well known and, further, it is still not clear if it is non-zero, a number of laboratory experiments have been done to place some upper limits on the value of an electron neutrino (Boris et al 1985(Boris et al , 1987see however Simpson 1986b;Bergkvist 1985a,b;Wilkerson et al 1987-LANL group;Fritschi et al (1986)-Zurich group;INS group 1987; and further claims by the Russian group -Lubimov 1988). Further improvements in various direct measurements have been obtained (INS group 1988;Kundig et al 1988;Lubimov 1988;Daniel et al 1988;Nakamura 1991).…”

Section: Introductionmentioning

confidence: 99%

Kinetic Equation with Neutrino Oscillations in the Early Universe

Granek¹,

McKellar²

1991

Aust. J. Phys.

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This paper considers the kinetic equation for interacting neutrino gas in the context of an expanding early universe. It is suggested that if neutrino oscillations are present and CP violations occur prior to the decoupling of the neutrino gas from the rest of the universe, then lepton number may not be conserved and, in principle, significant permanent neutrino chemical potentials may develop and survive until the present day. This would lead to the wen known effect that if the electron neutrino chemical potential is significantly non-zero, then the primordial abundances of the light elements are affected and differ from those of the standard model. Numerical computation is required to examine the parameter ranges leading to a significant non-zero electron neutrino chemical potential.

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The LMC supernova (SN 1987 A) as a probe for the outcome of stellar collapse

et al. 1987

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Implications from the available information on the supernova SN 1987A are discussed for the supernova models. We derive an upper hound of 10-25 eV for the neutrino rest mass.Aus den fur die Supernova 1987A verfugbaren Informationen werden SchluDfolgerungen fur Supernovamodelle diskutiert. Eine obere Grenze von 10 -25 eV fur die Neutrinoruhmasse wird abgeleitet.Keji ww-ds: supernova models -neutrino rest mass Four well known deep underground neutrino observatories, located in the Mont Blanc tunnel, the Baksan valley, the Morton Salt Mine (IMB), and the Kamioka Mine, respectively, reported recently neutrino signals most probable of astrophysical origin (TRAN THANH VAN 1987). For each neutrino burst the time differences between individual neutrino events and the neutrino energy were measured. (ii) The IMB detector measured eight neutrino events within five seconds in the energy range 20 5 E, 5 44 MeV. (iii) The Baksan neutrino observatory reported three events within six seconds in the energy range 12 5 E, 5 I8 MeV. (iv) Eleven events within thirteen seconds in the energy range 7 5 E,, 5 36 MeV were observed by the Kamiokande experiment. During the night of 2 3~2 4February, 1987 A supernova has been discovered in the nearby Large Magellanic Cloud (KUNKEL, MADORE 1987). Now it is certain that the supernova progenitor is Sanduleak -69202, a blue B3 supergiant. The analysis of the spectrum of SN 1987 A revealed an overall energy distribution which can be ascribed to that of a hot star. Studying the evolution of the optical spectrum of SN 1987 A shows strong spectral lines corresponding to the Balmer series of hydrogen. The shift of the H CI absorption trough with respect to the rest wavelength corresponds to a velocity of the emitting gas cloud of about 17000 km s -' (WOLTJEK et al. 1987). Due to the optical observations the event has to be considered as a supernova of type I1 originating from an exploding star in the mass range 10-25M,.According to the theory of the collapse of massive stars (10-25A4,) leading to the supernova type I T phenomenon, some time before the optical evidence of the event a strong neutrino signal should occur. Indeed, as summarized above, in the Liquid Scintillation Detector (LSD) of the soviet-italian collaboration in the Mont Blanc neutrino observatory five neutrino pulses of finite width, which can be definitely correlated with the optical discovery of the supernova SN 1987 A, were detected on February 23,1987. The burst seen by the Mont Blanc neutrino observatory has had a pulse width of seven seconds and an energy spread of 5 5 E, 5 10 MeV. The detector is sensitive to detect low energy particles with a threshold of (5-7) MeV. The neutrino burst should be originated by the collapse of the massive star to a neutron star.Moreover, the observation of a second event of neutrino pulses approximately five hours after the Mont Blanc observations has been reported by three other neutrino observatories as mentioned above. In the Kamioka experiment altogether eleven neutrino pulses with energies i...

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The neutrino mass from the tritium beta spectrum in valine

Cited by 48 publications

References 4 publications

The nature of neutrino mass and the phenomenon of neutrino oscillations

The nature of neutrino mass and the phenomenon of neutrino oscillations

Kinetic Equation with Neutrino Oscillations in the Early Universe

The LMC supernova (SN 1987 A) as a probe for the outcome of stellar collapse

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