Figure 61

Figure 61: Neutrino emissivities associated with different mechanisms of neutrino emission acting in a neutron star crust, versus ρ, at temperature T = 3 × 109 K. Numbers in parentheses indicate log10B. Effect of B = 1014 G (and a fortiori – effect of a lower B) on Qpaνir is insignificant. Qplνas, QBνrem, and Qphνot were calculated at B = 0. Label “syn (14)” – synchrotron radiation by electrons in constant magnetic field B = 1014 G, etc. Ground-state composition of the crust is assumed: Haensel & Pichon [183] model for the outer crust, and Negele & Vautherin [303] model for the inner crust. For further explanations see the text. From [428].