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Reception of Radio Waves from Pulsars

Published online by Cambridge University Press:  19 July 2016

R. T. Gangadhara
R. T. Gangadhara*
Affiliation:
Indian Institute of Astrophysics, Bangalore — 560034, India

Abstract

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The beamed emission by relativistic sources moving along the magnetic dipolar field lines occurs in the direction of tangents to the field lines. To receive such a beamed radiation, the line of sight must align with the tangent within the beaming angle 1/γ, where γ is the particle Lorentz factor. By solving the viewing geometry, in an inclined and rotating dipole magnetic field, we show that at any given pulse phase the observer can receive the radiation only from specific altitudes. We find that the outer conal emission is received from higher altitudes than the inner conal components including the core. At any pulse phase, low frequency emission comes from the higher altitudes than higher-frequency emission. As an application of our model, we have used it to explain the emission heights of conal components in PSR B0329+54.

Type
Part 7: Observations of Pulsed Emission
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 343 - 344
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Gangadhara, R. T., & Gupta, Y. 2001, ApJ, 555, 31.Google Scholar
Dyks, J., Rudak, B., & Harding, A. K. 2003, ApJ, in press (astro-ph/0307251).Google Scholar
Ruderman, M. A., & Sutherland, P. G. 1975, ApJ, 196, 51.Google Scholar