DOE OSTI2017
In this work, we interpreted the high braking index of PSR J1640−4631 with a combination of the magneto-dipole radiation and dipole magnetic field decay models. By introducing a mean rotation energy conversion coefficient ζ-bar , the ratio of the total high-energy photon energy to the total rotation energy loss in the whole life of the pulsar, and combining the pulsar’s high-energy and timing observations with a reliable nuclear equation of state, we estimate the pulsar’s initial spin period, P{sub 0}∼(17--44) ms, corresponding to the moment of inertia I∼(0.8--2.1)×10{sup 45} g cm{sup 2}. Assuming that PSR J1640−4631 has experienced a long-term exponential decay of the dipole magnetic field, we calculate the true age t{sub age}, the effective magnetic field decay timescale τ{sub D}, and the initial surface dipole magnetic field at the pole B{sub p}(0) of the pulsar to be 2900−3100 yr, 1.07(2)×10{sup 5} yr, and (1.84--4.20)×10{sup 13} G, respectively. The measured braking index of n=3.15(3) for PSR J1640−4631 is attributed to its long-term dipole magnetic field decay and a low magnetic field decay rate, dB{sub p}/dt∼−(1.66--3.85)×10{sup 8} G yr{sup −1}. Our model can be applied to both the high braking index (n>3) and low braking index (n<3) pulsars, tested by the future polarization, timing, and high-energy observations of PSR J1640−4631.
79 ASTRONOMY AND ASTROPHYSICS↗