The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640-4631

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 , the ratio of the total high-energy photon energy to the total rotation energ...

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Bibliographic Details
Published inThe Astrophysical journal Vol. 849; no. 1; pp. 19 - 30
Main Authors Gao, Zhi-Fu, Wang, Na, Shan, Hao, Li, Xiang-Dong, Wang, Wei
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.11.2017
IOP Publishing
Subjects
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Braking
Decay
Decay rate
DIPOLES
Energy
ENERGY CONVERSION
Energy dissipation
Energy loss
ENERGY LOSSES
EQUATIONS OF STATE
ISM: supernova remnants
magnetic field: neutron
MAGNETIC FIELDS
MOMENT OF INERTIA
Moments of inertia
NEUTRONS
POLARIZATION
PULSARS
pulsars: individual (J1640-4631)
Radiation
ROTATION
STAR EVOLUTION
stars: evolution
SUPERNOVA REMNANTS
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Summary: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 , 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, ms, corresponding to the moment of inertia g cm2. Assuming that PSR J1640−4631 has experienced a long-term exponential decay of the dipole magnetic field, we calculate the true age , the effective magnetic field decay timescale , and the initial surface dipole magnetic field at the pole of the pulsar to be 2900−3100 yr, yr, and G, respectively. The measured braking index of for PSR J1640−4631 is attributed to its long-term dipole magnetic field decay and a low magnetic field decay rate, G yr−1. Our model can be applied to both the high braking index ( ) and low braking index ( ) pulsars, tested by the future polarization, timing, and high-energy observations of PSR J1640−4631.
Bibliography:AAS05092
High-Energy Phenomena and Fundamental Physics
ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 14
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa8f49