2009/04/27 by S. A. Petrova, Svetlana Petrova, Petrova, S. A.
Engineering · Physics and Astronomy · #Astro and Planetary Science #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.0904.4121
4 pages, no figures. To appear in the Proceedings of the Low-Frequency Radio Universe Conference held at NCRA-TIFR, Pune, 8-12 December 2008, eds. D.J. Saikia, D. Green, Y. Gupta, and T. Venturi
arxiv created 2009/04/27 · openalex publication_date 2009/04/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We for the first time propose a physical model of the precursor (PR) and interpulse (IP) components of the radio pulsar profiles. It is based on propagation effects in the secondary plasma flow of a pulsar. The components are suggested to result from the induced scattering of the main pulse (MP) into background. The induced scattering appears efficient enough to transfer a significant part of the MP energy to the background radiation. In the regimes of superstrong and moderately strong magnetic field, the scattered components are approximately parallel and antiparallel to the velocity of the scattering particles and can be identified with the PR and IP, respectively. The spectral evolution, polarization properties, and fluctuation behaviour of the scattered components are examined and compared with the observational results. The perspectives of the complex profile studies are outlined as well.