Neutrino massive

Electronic properties of CNTs, in particular, electronic states, optical spectra, lattice instabilities, and magnetic properties, have been discussed theoretically based on a k p scheme. The motion of electrons in CNTs is described by Weyl s equation for a massless neutrino, which turns into the Dirac equation for a massive electron in the presence of lattice distortions. This leads to interesting properties of CNTs in the presence of a magnetic field including various kinds of Aharonov-Bohm effects and field-induced lattice distortions. 

Confluence of Cosmology, Massive Neutrinos, Elementary Particles Gravitation... 

Three sources have been proposed to produce fluorine in the Galaxy. The first was suggested by Forestini et al. (1992) and refers to production in low-mass stars during the AGB phase while two others are related to massive stars production in Wolf-Rayet stars (Meynet Arnould 2000) and in type II Supernovae, via the neutrino-induced nucleosynthesis (Woosley et al. 1990). 

MARE [32-38], Neutrino oscillation experiments have proved that neutrinos are massive particles, but cannot determine their absolute mass scale. Therefore, the neutrino mass is still an open question in elementary particle physics. An international collaboration is growing around the project of microcalorimeter arrays for a rhenium experiment (MARE) for directly measuring the neutrino mass with a sensitivity of about 0.2eV/c1 2 4. 

In the last decade, neutrino experiments have demonstrated that neutrinos are massive particles which may oscillate among three autostates. Such experiments [77-82] have evidenced the mass difference between the autostates, but not the neutrino mass scale value. The only way to determine the neutrino mass is the knowledge of the shape of the end point of energy spectrum in beta decays. In the hypothesis of the Majorana neutrino (neutrino coincides with antineutrino and its rest mass is different from zero), the measure of the decay half-life in the neutrinoless double-beta decay (DBD) would be necessary. A number of recent theoretical interpretations of neutrino oscillation experiments data imply that the effective Majorana mass of the electron neutrino (as measured in neutrinoless DBD) could be in the range 0.01 eV to the present bounds. 

According to most theoretical analyses of the present neutrino experiment results, next-generation DBD experiments with mass sensitivities of the order of lOmeV may find the Majorana neutrino with a non-zero effective electron neutrino mass, if the neutrino is self-conjugate and the neutrino mass spectrum is of the quasi-degenerate type or it has inverted hierarchy [83], Majorana massive neutrinos are common predictions in most theoretical models, and the value of a few 10 2cV predicted for its effective mass, if reached experimentally, will test its Majorana nature. 

S. P. Mikheyev and A. Yu. Smirnov, 86 Massive Neutrinos in Astrophysics and in Particle Physics, proceedings of the Sixth Moriond Workshop, edited by O. Fackler and J. Tran Thanh Van (Editions Frontieres, Gif-sur-Yvette, 1986), pp. 355. 

These same physicist astronomers, today called astroparticle physicists, are currently setting up and line-tuning traps for neutralinos, hypothesised particles of dark matter. These are just as subtle as neutrinos, but much rarer and much more massive. For the moment, the search has been fruitless, but patience is a virtue in the hunt for the invisible. 

Neutrinos are usually evoked as detonators, triggering or driving the explosion of massive stars. The gravitational energy freed by core collapse of a massive star, some 10 erg, is mainly evacuated by neutrinos. These pour out in such inordinate amounts that if just 1% of their energy is communicated to matter in the envelope, the whole thing will be blasted out of existence. 

The conceptually simplest way of forming a black hole at the heart of a massive star, thereby setting up the conditions of the hypernova model, is to begin by repudiating the traditional explosion model detonated by neutrinos. The iron core then collapses without remission in the space of one second. A black hole prospers, pulling down the rest of the stellar edifice. This may be a common occurrence for stars of 35 to 40 Mq. However, uncertainties remain concerning convection, mass loss and mixing due to rotation, not to mention the explosion mechanism itself. 

Trillions of neutrinos are flying through your body as you read this. Created by the Big Bang, stars, and the collision of cosmic rays with the earth s atmosphere, neutrinos outnumber electrons and protons by 600 million to 1. [For more information, see. Gibbs, W. (1998) A massive discovery. Scientific American. August, 279(2) 18-19.]... 

The prediction of a heavy boson has received preliminary empirical support [92,96] from an anomaly in Z decay widths that points toward the existence of Z bosons with a mass of 812 GeV 1 33j [92,96] within the SO(l) grand unified field model, and a Higgs mechanism of 145 GeV4gj3. This suggests that a new massive neutral boson has been detected. Analysis of the hadronic peak cross sections obtained at LEP [96] implies a small amount of missing invisible width in Z decays. The effective number of massless neutrinos is 2.985 0.008, which is below the prediction of 3 by the standard model of electroweak interactions. The weak charge Qw in atomic parity violation can be interpreted as a measurement of the S parameter. This indicates a new Qw = 72.06 0.44, which is found to be above the standard model pre-... 

Based upon the foregoing experiences, some researchers observed that the same reluctance to interact with matter is responsible for the neutrino s long range and ability to resist detection. Tlios, it was reasoned that an apparatus for detecting neutrinos should be massive and shielded from the interference of other particles and radiation. As a solution to these problems, some researchers proposed a deep underwater muon and neutrino detector (acronym DUMAND). 

As pointed out by M. Turner (University of Chicago), a massive, neutrino would violate every theoretical prejudice we have in particle physics, astrophysics, and cosmology J. Bahcall (Institute of Advanced Study at Princeton) observes, It s a surprise. If it s true, tlien it s pointing us in a different direction than previous physics suggested, ... 

Mohapatra, R.N. and P.B. Pal Massive Neutrinos in Physics and Astrophysics, World Scientific Publishing Company, Inc., River Edge, NJ, 1992. 

In the years following Ya.B. returned several times to this topic. With the emergence of the hypothesis that a significant portion of the Universe s mass is concentrated in massive neutrinos, studies of higher-degree singularities which form in the process of pancake growth became very timely [64]. Analysis of the collisionless model, both theoretical and by means of... 

Another important classification of particle dark matter rests upon its production mechanism. Particles that were in thermal equilibrium in the early Universe, like neutrinos, neutralinos, and most other WIMPs (weakly interacting massive particles), are called thermal relics. Particles which were produced by a non-thermal mechanism and that never had the chance of reaching thermal equilibrium in the early Universe are called non-thermal relics. There are several examples of non-thermal relics axions emitted by cosmic strings, solitons produced in phase transitions, WIMPZILLAs produced gravitationally at the end of inflation, etc. 

On the other hand, Eq. (16.21) can be used in conjunction with inequality (16.18) to obtain a lower bound on the cosmological density in neutrinos. Taking only one massive Majorana flavor,... 

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