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Accreting neutron stars and black holes

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Figure

Figure 1.1: Lines of constant gravitational potential for a binary. Indicated are the positionsof the primary and the secondary star and the center of mass of the system (CM)
Figure 1.2: A plot of the disc’s surface density versus its surface temperature. The S-shapedthermal equilibrium curve forces the disc to follow the limit cycle, see text.
Figure 1.5:A cartoon depicting the evolution of a zero age main sequence (ZAMS) bi-nary system leading to an LMXB and finally the formation of a binary millisecond pulsar.Parameters are given for a scenario leading to the formation of PSR 1855+09
Figure 1.6: Mass-radius curves for neutron stars for typical EOSs (black) and strange quarkmatter EOSs (green)
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