Construction Of The Radiation Curve Of Pulsar Corresponding To Emission From Magnetic Dipole Field

In this work we derive the equations for the dipole component of pulsar’s magneticrnfield and construct its radiation curve. This is done following spinning separatedrncharges as an alternative model for generating dipolar pulsar magnetic field fromrnKebede, L.W. 2002. We approach the problem by solving Legendre functions, sphericalrnharmonics theorem (i.e, Ylm(θ, ϕ) for l = m = 1) and Maxwell’s equations to findrnthe equations of the magnetic field strength B. The dipolar magnetic field obtainedrnbased on this model is proportional to the charge Q and the angular frequency ω ofrnthe pulsar (i.e, B ∝ Qω) which has an advantage of accommodating the wide range ofrnneutron stars’s (i.e, both pulsars and magnetars) magnetic field. We have taken datarnfor the parameters such as Q and ω for the seven well studied pulsars to check thernmagnetic field prediction of the model with the observational values, and our result isrnin close confirmation with the observed strength of the magnetic field for these sevenrnwell known pulsars.

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