Figure 83: X-ray luminosities of SXTs in quiescence vs. time-averaged accretion rates. The heating
curves correspond to different neutron star masses, increasing from the top to the bottom, with a
step of . The EoS of the core is moderately stiff, with [340].
The model of a strong proton and a weak neutron superfluidity is assumed [261]. The highest curve
(hottest stars) corresponds to , and the lowest one (coldest stars) to . The
upper bundle of coalescing curves corresponds to masses , where a star of mass
has a central density equal to the threshold for the direct Urca process. The red dotted
line represents thermal states of a “basic model” (nonsuperfluid core, slow cooling via a modified
Urca process). Total deep heat released per accreted nucleon is . Figure made by
K.P. Levenfish. For a further description of neutron star models and observational data see Levenfish
& Haensel [261].
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