Photon-neutrino 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.

The main sequence stars and the photon-neutrino coupling theory of weak interactions

To test the photon-neutrino coupling theory of weak interactions as presented by Bandyopadhyay (1968), detailed models of the Main Sequence stars with neutrino emission based on this theory are computed. The models are compared with the observational data, and it is concluded that the photon-neutrino coupling theory would seem to be definitely excluded on astrophysical grounds.

The photon-neutrino coupling theory and stellar models

The effect of the photon-neutrino coupling theory, developed by Bandyopadhyay (1968), on stellar structure is studied by constructing a chemically homogeneous model of one solar mass in thermal equilibrium, and taking into account the neutrinos according to the theory. As anticipated, the effect is large and leads to great difficulties in the understanding of stellar constitution.

Solar energy cycle and its relation to geomagnetic activity

It is suggested that recurrent and nonrecurrent geomagnetic disturbances which are related to the release of solar magnetic energy in the form of unipolar and bipolar magnetic regions respectively, are connected with the variations in the solar energy source. The true beginning of the solar cycle takes place when unipolar magnetic regions start to develop, i.e, when nuclear energy generation becomes dominant over the neutrino energy loss according to the photon-neutrino coupling theory.

Possible origin of cosmic γray flux from pulsars

The flux of celestial gamma rays has been calculated from neutron stars (pulsars) on the basis of the model of neutron stars as developed by Tsuruta and Cameron and the cooling rate calculated by Raychaudhuri taking into account neutrino emission according to the photon-neutrino coupling theory. The result is found to be in good agreement with the experimental results as obtained in OSO III experiments.

Irregular nebular variables and neutrino emission

The suggestion that the less massive star will reach the Main Sequence stage earlier than the massive star due to the effect of neutrino emission according to the photon-neutrino coupling theory is supported by the observed behaviour of H-R diagram of irregular nebular variables. After reaching the Main Sequence stage the star should pulsate with a period due to the effect of neutrino emission which may be a possible explanation of other properties of irregular nebular variables.

Origin of stellar magnetic fields

It is pointed out that the magnetic field of a star is originated from dynamo action associated with the stellar evolution. The magnetic field of a star is related with how much nuclear energy is generated in its phase of evolution. From this we can explain why some stars possess a magnetic field high than that of the Sun. In our case the magnetic field of the star is a by-product of the stars evolution and it has no influence on the internal structure of the star but it does have influence on the flare, chromosphere and coronal activities of the star. Again it is stressed that to confirm the activities of the star, the details of evolution of stars should be calculated according to the photon-neutrino coupling theory.

Neutrino processes in the lepton era of the universe and hot big bang cosmology

The neutrino interactions in the lepton era of the universe have been studied here according to the photon-neutrino coupling theory. It is found that neutrinos were decoupled from electrons from the beginning of the universe and remained so throughout the lepton era of the universe in hot big bang cosmology.

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.

The Sun, C12/C13 abundance ratio and neutrino emission

It is pointed out that the effect of neutrino emission process according to the photonneutrino coupling theory can be taken to interpret the observed ratio of C12/C13 abundance and other solar activities.

Neutrino emission, population II stars and big-bang cosmology

The spectroscopic determination of the helium abundance in the oldest stars of the galaxy is supported by the theory of stellar evolution when neutrino emission is considered according to the photon-neutrino coupling theory, if it is assumed that the population II stars started their life with a low surface helium content.

Effect of neutrino emission in the sun and other main sequence stars

Pontecorvo (1959) suggested that, because of the negligible absorption of neutrino upon interaction with matter, the neutrino emission can play a significant role in stellar evolution. The profound implication of neutrino emission in the case of stellar evolution has been studied by many authors according to the current-current coupling theory which was suggested by Feynman and Gell-Mann (1958) and also by Sudarshan and Marshak (1958). According to the current-current coupling theory neutrino emission processes are only important when the temperature exceeds 4 x 108 K. Recently Bandyopadhyay (1968) has proposed that photons can interact weakly only with neutrinos. Considering this photon-neutrino coupling theory, Ray Chaudhuri (1970) has suggested that plasma neutrino emission process may prevent the helium flash in certain red giant stars. Also from an analysis of plasma neutrino emission (Ray Chaudhuri, 1970b) and neutrino synchrotron radiation (Ray Chaudhuri, 1970c) process Ray Chaudhuri has shown that the observed deficiency of white dwarf mass above 0.9M e can be explained according to the photon neutrino coupling theory. Therefore, from the observational evidence we cannot exclude the photonneutrino coupling theory; though no categorical answer from the terrestrial experiment can be given at present. The direct determination of the existence of the photonneutrino coupling theory using the elastic scattering of electrons by fission antineutrinos as attempted by Reines and Gurr (1970) (Bandyopadhyay and Ray Cbaudhurl, 1970) as well as by detection of solar neutrinos using knock on electrons produced in the neutrino electron scattering has been discussed by Ray Chaudhuri and Bandyopadhyay (1969). Again Bandyopadhyay et al. (1969) have considered the photon-neutrino elastic scattering on the basis of this photon-neutrino coupling theory and have shown that the cross section for the process v +p ~ v +p is at least an order smaller than that of the process f +p ~ n+ e + which is well within the experimental upper limit. Assuming that this type of neutrino emission processes do occur in reality, we wish to point out that the neutrino emission can also play a significant role in the Main Sequence stage (i.e. hydrogen burning); and from the balance of energy generation we point out the possible nuclear process which may be active in that stage.

Theories of weak interactions and astrophysical evidence

It has been proposed in an earlier paper that photons can interact weakly with neutrinos. Assuming this photon-neutrino coupling, the effect of energy loss due to the pair-annihilation process and the photoneutrino process on the evolutionary time scales of a 15.6M⊙ star has been discussed. In the typical model of Hayashi, Hoshi and Sugimoto (HHS), the lifetimes for carbon burning and later phases have been calculated assuming the photon-neutrino coupling, and is compared with the results obtained by HHS according to the (eν)(eν) coupling. In case of the\(\gamma \nu \bar \nu \) coupling, the ratio of the number of blue supergiants (He-burning stars) to red supergiants (stars in C-burning and later stages) is found to be ≲ 10 with the initial concentration of carbonXc=0.5, whereas according to the (eν)(eν) coupling, the corresponding ratio is found to be nearly 33. According to astrophysical observations, this ratio is found to be nearly unity within a factor 1.5. It is noted that the result according to the\(\gamma \nu \bar \nu \) coupling becomes significantly better in comparison with the (eν)(eν) coupling. Also, in view of the uncertatinties regarding the total luminosity in the red-supergiant phase as well as the rate of C+C relation, we can consider the result obtained according to the\(\gamma \nu \bar \nu \) coupling to be in reasonable proximity to the «observed» value. From this, we argue that stars seem to «favour» the photon-neutrino coupling theory rather than the current-current coupling theory of weak interactions.

Astrophysical Exclusion of Photon-Neutrino Weak Coupling

The photon-neutrino coupling theory of weak interactions as presented by Bandyopadhyay is definitely excluded by the astrophysical data for white dwarfs. Furthermore, it is impossible to adjust the photon-neutrino coupling constant so as to reproduce simultaneously the pertinent astrophysical data for white dwarfs and red supergiants.

Neutrino synchrotron radiation

The neutrino synchrotron radiation for a completely relativistic electron gas in the presence of large magnetic field is computed according to the photon neutrino coupling theory of weak interactions. The radiation is also estimated for the non-relativistic case. The neutrino luminosity of several model white dwarfs are computed according to the photon-neutrino coupling theory and compared with that of the current-current coupling theory. It is shown that, according to the photonneutrino coupling theory, the neutrino luminosity is greater than the photon luminosity and, therefore, most likely to have astrophysical significance in the evolution of stars with large electron energies and potentially large magnetic field, such as white dwarfs.

Plasma neutrino emission from stars and its astrophysical evidence

The emission of neutrino pairs by a stellar plasma is calculated according to the photon–neutrino coupling theory and is compared with the result obtained on the basis of the current–current coupling theory of weak interactions. We have also discussed the effect of the plasma neutrino emission on the evolution of white dwarfs. It is observed that the small fraction of the observed white dwarfs with masses above [Formula: see text] can be interpreted when the plasma neutrino emission is considered from the point of view of the photon–neutrino coupling theory.

Photoneutrino energy loss rates

The neutrino energy loss rate due to the photoneutrino process in a hot plasma, including the contributions from positrons in the black body radiation according to the photon–neutrino coupling theory, has been obtained. This is then compared with that obtained on the basis of the current–current coupling theory of weak interactions for a variety of conditions.

Neutrino energy density of the universe

An estimate of the neutrino energy density of the universe has been made on the basis of the photon-neutrino coupling theory of weak interations. It is found that, according to this theory, neutrino energy density is the same as the matter density in the steady-state universe. Finally some cosmological implications of this result have been discussed.