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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4618
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dc.contributor.authorGangadhara, R. T-
dc.date.accessioned2009-07-03T13:56:17Z-
dc.date.available2009-07-03T13:56:17Z-
dc.date.issued2008-
dc.identifier.citationHasan, S. S., Gangadhara, R. T. and Krishan, V. eds., Turbulence, dynamos, accretion disks, pulsars and collective plasma processes, First Kodai-Trieste workshop on plasma astrophysics held at the Kodaikanal Observatory., Astrophysics and space science proceedings., Kodaikanal., India, 2007., pp. 113 - 135en
dc.identifier.isbn978-1-4020-8867-4-
dc.identifier.urihttp://hdl.handle.net/2248/4618-
dc.descriptionRestricted Accessen
dc.descriptionThe original publication is available at springerlink.com-
dc.description.abstractPulsar radio emission is belived to come from relativistic plasma accelerated along the dipolar magnetic field lines in pulsar magnetosphere. The beamed emission by relativistic sources occur in the direction of tangents to the field lines in the corotating frame, but in an inertial (lab) frame it is aberrated toward the direction of rotation. To receive such a beamed emission line-of-sight must align with the source velocity within the beaming angle 1/γ, where γ is the Lorentz factor of the source. By solving the viewing geometry, in an inclined and rotating dipole magnetic field, we find the coordinates of the emission region in corotating frame. Next, give a general expression for the phase shift in the intensity profile in lab frame by taking into account of aberration, retardation and polar cap currents.en
dc.language.isoenen
dc.publisherSpringer Netherlandsen
dc.relation.urihttp://dx.doi.org/10.1007/978-1-4020-8868-1_8en
dc.relation.urihttp://adsabs.harvard.edu/abs/2008tdad.conf..113Gen
dc.rights© Springeren
dc.subjectAstrophysical Turbulenceen
dc.subjectPulsaren
dc.subjectDynamosen
dc.subjectSolar and Space Plasmasen
dc.subjectRadio Emissionen
dc.subjectGeometryen
dc.titlePulsar radio emission geometryen
dc.typeArticleen
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