Abstract
We study the v\bar v\-pair emission from electrons and protons in a relativistic quantum approach. In this work we calculate the luminosity of the v\bar v\-pairs emitted from neutron-star-matter with a strong magnetic field, and find that this luminosity is much larger than that in the modified Urca process. The v\bar v\-pair emission processes in strong magnetic fields significantly contribute to the cooling of the magnetars.
Highlights
Magnetic fields in neutron stars play important roles in the interpretation of many observed phenomena
We give the νluminosities from the modified Urca (MU) process [6]
We see that the magnetic field has a role to enhance the neutrino emission in the both processes largely
Summary
Magnetic fields in neutron stars play important roles in the interpretation of many observed phenomena. Magnetars, which are associated with super strong magnetic fields [1, 2], have properties different from normal neutron stars. Phenomena related magnetars can provide a lot of information about the physics of the magnetic field. Many authors have paid attention into cooling processes of neutron stars (NS) because it gives important information on neutron star structure [3]. In this work we study two kinds of the processes, the νν-pair synchrotron radiation p(e−) → p(e−) + ν + νby calculating it through the transition between the different Landau levels for protons and electrons [4]
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