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Rotation induced deep crustal heating of millisecond pulsars

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Figure

Figure 1. Heating rate in the crust normalized to 10 29 erg s −1 as a function of NS mass for three BSk EOSs (left-hand panel) and three PAL EOSs (right-hand panel)
Fig. 2 illustrates the accuracy of the slow-rotation approxima- approxima-tion as a funcapproxima-tion of rotaapproxima-tion rate

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