Construction of the Radiation Curve of Pulsar Corresponding to Emission from Magnetic Dipole Field

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dc.contributor.advisorReshid, Remudin (PhD)
dc.contributor.authorKenea, Fekadu
dc.date.accessioned2019-10-09T06:32:17Z
dc.date.accessioned2023-11-09T11:26:13Z
dc.date.available2019-10-09T06:32:17Z
dc.date.available2023-11-09T11:26:13Z
dc.date.issued2017-11-04
dc.description.abstractIn this work we derive the equations for the dipole component of pulsar’s magnetic field and construct its radiation curve. This is done following spinning separated charges as an alternative model for generating dipolar pulsar magnetic field from Kebede, L.W. 2002. We approach the problem by solving Legendre functions, spherical harmonics theorem (i.e, Ylm(θ, ϕ) for l = m = 1) and Maxwell’s equations to find the equations of the magnetic field strength B. The dipolar magnetic field obtained based on this model is proportional to the charge Q and the angular frequency ω of the pulsar (i.e, B ∝ Qω) which has an advantage of accommodating the wide range of neutron stars’s (i.e, both pulsars and magnetars) magnetic field. We have taken data for the parameters such as Q and ω for the seven well studied pulsars to check the magnetic field prediction of the model with the observational values, and our result is in close confirmation with the observed strength of the magnetic field for these seven well known pulsars.en_US
dc.identifier.urihttp://10.90.10.223:4000/handle/123456789/19342
dc.language.isoenen_US
dc.publisherAddis Ababa Universityen_US
dc.subjectPulsars Magnetic Feldsen_US
dc.subjectConstruction of the Radiationen_US
dc.subjectCurve of Pulsaren_US
dc.subjectCorrespondingen_US
dc.subjectEmissionen_US
dc.subjectMagnetic Dipole Fielden_US
dc.titleConstruction of the Radiation Curve of Pulsar Corresponding to Emission from Magnetic Dipole Fielden_US
dc.typeThesisen_US

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