The neutrino energy loss by electron capture of nuclides ^(55)Co and ^(56)Ni in explosive stellar environments

Using the Shell-Model Monte Carlo method and the Random Phase Approximation theory, we carry out an estimation of neutrino energy loss （NEL） for 55Co and 56Ni by electron capture. We find that the NEL rates increase greatly at some typical stellar conditions, and can even exceed five orders of magnitude （e.g. T9 = 38.5, Ye = 0.42 for 56Ni）. On the other hand, the error factor C shows that the fit is fairly good for two results at higher density and lower temperature, and the max- imum error is - 1.2%. However, the maximum error is ,- 55.60% （e.g. T9 = 18.5, Ye = 0.45） at lower density and higher temperature.

A new study of neutrino energy loss of nuclides ^(53-60)Cr by electron capture in magnetars

Following the theory of relativity, in the presence of an ultrastrong magnetic field （UMF） and utilizing a nuclear shell model, we carry out an estimation of the neutrino energy loss （NEL） rates of nuclides ^53-60Cr, which occur by electron capture in magnetars. The results show that the NEL rates greatly increase when a UMF is present, and can even exceed nine orders of magnitude at relatively lower density and temperature （e.g. ρ7 = 5.86, Ye = 0.47, T9 = 7.33） in the range from 1013 G to 1018 G. However, the increase in rates was no more than six orders of magnitude at relatively higher density and temperature （e.g.ρ7 = 4.86 × 10^8, Ye = 0.39, T9 = 14.35）.

Modification of Constants in the Schrödinger Equation Giving Access to Neutrino Behavior

The paper deals with a study of the Schrödinger equation with an original approach. Recalling the well-known relation: p→iℏΔr. It considers this equation for which the kinetic factor is EKin=p22M=−ℏ22MΔr2. Making the kinetic factor EKin=−Δr2can be obtained if one defines a mass M=ℏ22, very small and close to the accepted mass of a neutrino νe. The Schrödinger equation reduces to: −Δr2ϕ(r)=Eϕ(r). The energy E is that given by Dirac (1927), (c being the light velocity), with his remark that two solutions exist E=±p2c2+M2c4. The body of this paper shows all solutions obtained when solving the simplified Schrödinger equation.

A Model of Fermion Masses and Flavor Mixings with Family Symmetry SU(3)U(1)

The family symmetry SU（3） U（1） is proposed to solve flavor problems about fermion masses and flavor mixings. It is breaking is implemented by some flavon fields at the high-energy scale. In addition a discrete group Z2 is introduced to generate tiny neutrino masses, which is broken by a real singlet scalar field at the middle-energy scale. The low-energy effective theory is elegantly obtained after all of super-heavy fermions are integrated out and decoupling. All the fermion mass matrices are regularly characterized by four fundamental matrices and thirteen parameters. The model can perfectly fit and account for all the current experimental data about the fermion masses and flavor mixings, in particular, it finely predicts the first generation quark masses and the values of θ13and JCp in neutrino physics. All of the results are promising to be tested in the future experiments.

Lepton and quark mixing patterns with generalized CP transformations

In this study,we modify a scenario,originally proposed by Grimus and Lavoura,in order to obtain maximal values for the atmospheric mixing angle and CP,violating the Dirac phase of the lepton sector.To achieve this,we employ CP and some discrete symmetries in a type Ⅱ seesaw model.To make predictions about the neutrino mass ordering and smallness of the reactor angle,we establish some conditions on the elements of the neutrino mass matrix of our model.Finally,we study the quark masses and mixing pattern within the framework of our model.