Photon-neutrino Weak-coupling Theory Research Articles

Disintegration of deuteron by neutrino-deuteron scattering and the photon-neutrino weak-coupling theory

We study here disintegration of the deuteron by neutrino-deuteron scattering according to the photon-neutrino coupling theory. It is found that the value of $\ensuremath{\sigma}$ calculated for the transition $^{3}S\ensuremath{\rightarrow}^{1}S$ in the energy range of 50 MeV is of the order of ${10}^{\ensuremath{-}42}$ ${\mathrm{cm}}^{2}$ A comparison is also made here with the predictions of the Salam-Weinberg theory.

Threshold pion production by neutrinos and the photon-neutrino weak-coupling theory

Neutral-lepton-current interactions in the threshold pion production process νn→νpπ- have been studied by the photon-neutrino weak-coupling theory. It is found that the value of dσ/dw, wherew is the ppπ- invariant mass, is of the order of 10−40 cm2/20 MeV and the general shape shows a sharp rise neur threshold before theN* production and, beyond this region, a sharp depletion occurs. These features are in excellent agreement with the experimental observations.

Neutral lepton current, elastic and deep-inelastic neutrino-nucleon scattering and the photon-neutrino weak-coupling theory

Neutral lepton current, elastic and deep-inelastic neutrino-nucleon scattering and the photon-neutrino weak-coupling theory

Muonless neutrino events and the photon-neutrino weak-coupling theory

We discuss here the mounless neutrino events according to the photon-neutrino weak-coupling theory and it is found that recent experimental results conform well with the theoretical predictions. We also point out that strangeness-changing neutral lepton currents are not allowed in this theory and so no unnatural mechanism is needed to interpret the highly stringent limits on the processes like KL0 → μ−μ+ and\(K + \to \pi ^ + \nu \bar \nu \) as observed in experiments.

Elastic scattering of electrons by fission antineutrinos

The scattering cross-sections for the elastic-scattering reaction\(\bar \nu _e + e^ - \to \bar \nu _e + e^ - \) taking into account the energy spectrum of electron-antineutrinos from235U fission have been calculated according to the photon-neutrino weak-coupling theory for several values of minimum electron energy from 1 to 5.5 MeV. The results are then compared with those derived according to theV-A theory. It is found that the present experimental upper limit for the cross-section as reported by Reines and Gurr is about 200 times the cross-section predicted with the photon-neutrino coupling theory. Finally, the arguments put forward by Stothers for the astrophysical exclusion of the photon-neutrino coupling theory are discussed and shown to be invalid in view of various uncertainties entering into the calculation of stellar evolution.

Elastic scattering of electrons by solar neutrinos and weak interaction theories

The counting rate of recoil electrons for the elastic scattering of electrons by solar neutrinos, considering that the CNO cycle is responsible for nuclear energy generation in the sun, is calculated according to the photon-neutrino weak coupling theory as well as the current-current coupling theory. It is suggested that this result can be used to decide which type of weak interaction exists in nature.

Weak interaction of photons and the process ν+Z→ν+Z+λ++λ-

The cross section for the process nu +Z to nu +Z+ lambda ++ lambda -, where lambda +or- represents e+or- or mu +or-, has been calculated form the point of view of the photon-neutrino weak coupling theory. The importance of this process to test the different theories of weak interactions has also been discussed.

Neutrino bremsstrahlung from a degenerate electron gas

The neutrino bremsstrahlung process is studied here according to the photon-neutrino weak coupling theory by considering the electrons as relativistic and degenerate and by adding some lattice effects at high density. The neutrino energy loss rate due to the process is then compared with that obtained according to the current-current coupling theory. It is concluded that the process is important only in cases of high dense stars when the temperature is below 107K.

Cosmic rays, neutron stars and pulsars

The cooling behaviour of neutron stars, taking into account several models proposed by Tsuruta and Cameron, has been studied on the basis of neutrino emission according to the photon-neutrino weak coupling theory. It is shown that the internal energy storage is sufficient to interpret X-ray emission and other cosmic ray activities of neutron stars. Also it is found that only one supernova outburst in 100 years can explain the steady state cosmic ray flux in the galaxy. Finally, some remarks about the possible pulsation of neutron stars are made.

The Photon as a Composite State of a Neutrino-Antineutrino Pair

The possibility that the photon may be a composite state of a neutrino-antineutrino pair has been examined from field-theoretic considerations on the basis of the photon-neutrino weak-coupling theory. It is shown that the difficulties which generally crop up in quantum electrodynamics to describe a photon as a composite state of an electron-positron pair using the ${Z}_{3}=0$ condition are avoided in neutrino dynamics (photon-neutrino weak interaction). In view of this, we conclude that the photon may be taken as a composite state of a neutrino-antineutrino pair when the composite character is described by the vanishing of the wave-function renormalization constant and the nonvanishing of a certain composite coupling constant.

Some remarks on the role of neutrino processes in red giants

It is shown that the plasma neutrino emission rate, when calculated according to the photon–neutrino weak coupling theory, has significant effects on the evolution of red giants.

Some remarks on the possible origin of superheavy nuclei in primary cosmic rays

Neutron stars (pulsars) are here proposed as the sources of superheavy (SH) nuclei Z>or=110 in primary cosmic rays. Taking into account the 1969 result of Berlovich and Novikov that these SH nuclei can be formed by the r process when the temperature is greater than 1.8*10 degrees K and at sufficiently high neutron number density, it is here pointed out at this temperature condition can prevail in a neutron star for approximately for 103 years when the cooling behaviour is governed by the synchrotron radiation of neutrinos according to the photon-neutrino weak coupling theory. On the basis of this result, it is argued that the formation of SH nuclei in the Galaxy can be considered as a continuous event. Finally, some remarks are made about the expected flux of these SH nuclei.

Neutrinos and arrow time in cosmology

The arrow of time in the case of neutrinos is investigated taking into account photon-neutrino weak-coupling theory. It is shown that in both steady state and Einstein-de Sitter cosmological models, the advanced effect can be avoided.

Propagation of Electromagnetic Waves in a Degenerate Neutrino Sea

The propagation of electromagnetic waves in a Fermi sea of neutrinos is investigated on the basis of the photon-neutrino weak-coupling theory and is compared with the result obtained by Royer on the basis of the $(e\ensuremath{\nu})(e\ensuremath{\nu})$ coupling. It is shown that a photon propagating through the neutrino sea satisfies a dispersion relation of the form ${\ensuremath{\omega}}^{2}={{\ensuremath{\omega}}_{0}}^{2}+{k}^{2}{c}^{2}$, where ${(\ensuremath{\hbar}{\ensuremath{\omega}}_{0})}^{2}\ensuremath{\approx}6.2\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}23}$ ${{E}_{F}}^{2}$, ${E}_{F}$ being the Fermi energy of the sea. Finally, some remarks are made as to the possibility of the destruction of a photon when propagating through the sea due to the process $\ensuremath{\gamma}+\ensuremath{\nu}\ensuremath{\rightarrow}\ensuremath{\nu}+\ensuremath{\nu}+\overline{\ensuremath{\nu}}$. It is found that the mean free path corresponding to this process is \ensuremath{\approx} ${10}^{69}$ cm, much larger than the radius of the universe.

Weak interaction of photons and neutrino-electron scattering

The neutrino-electron scattering has been discussed according to the photon-neutrino weak-coupling theory. The results are then compared with those obtained in the current-current coupling theory. The rate for neutrino-electron scattering has also been discussed for nondegenerate and degenerate gases. Astrophysical applications are then made by evaluating the ratio of the neutrino mean free path to the stellar radius. It is shown that, according to the photon-neutrino weak coupling, the neutrino mean free path exceeds the stellar radius for massive stars, white dwarfs and neutron stars. This result is significant in the sense that according to the current-current coupling theory, the ratio of the neutrino mean free path to the stellar radius for neutron stars can be much less than unity, though for other types of stars the neutrino mean free path exceeds the stellar radius. Finally, some remarks are made about the experiment attempted by Reines and Kropp to detect solar neutrinos using knock-on electrons produced in the neutrino-electron scattering.