Figure 61: Neutrino emissivities associated with different mechanisms of neutrino emission acting in
a neutron star crust, versus , at temperature T = 3 109 K. Numbers in parentheses indicate
. Effect of B = 1014 G (and a fortiori – effect of a lower B) on is insignificant.
, , and 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].
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