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Origin of the pulsar pulse fine structure

Published online by Cambridge University Press:  20 March 2013

O. M. Ulyanov ,
A. A. Seredkina  and
A. I. Shevtsova
O. M. Ulyanov
Affiliation:
Department of Astrophysics, Institute of Radio Astronomy of NAS of Ukraine, Krasnoznamennaya str.4, Kharkov 61002, Ukraine email: oulyanov@rian.kharkov.ua, seredkina.a@gmail.com, alice.shevtsova@gmail.com
A. A. Seredkina
Affiliation:
Department of Astrophysics, Institute of Radio Astronomy of NAS of Ukraine, Krasnoznamennaya str.4, Kharkov 61002, Ukraine email: oulyanov@rian.kharkov.ua, seredkina.a@gmail.com, alice.shevtsova@gmail.com
A. I. Shevtsova
Affiliation:
Department of Astrophysics, Institute of Radio Astronomy of NAS of Ukraine, Krasnoznamennaya str.4, Kharkov 61002, Ukraine email: oulyanov@rian.kharkov.ua, seredkina.a@gmail.com, alice.shevtsova@gmail.com
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Abstract

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We give a new numerical model of pulsar pulse radiation through the interstellar medium (ISM) considering the propagation effects. It explains the deficit of a scattering measure at the decameter range of frequencies that leads to the possibility of detecting the pulsar pulse fine structure. The results of numerical simulation confirm that the fine structure may be detected at low frequencies and this is qualitatively agreed with the observational data.

Keywords

interstellar medium (ISM)scatteringpulsar
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 527 - 529
Copyright
Copyright © International Astronomical Union 2013

References

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