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Identification of Physical Components in Pulsar Emission

Published online by Cambridge University Press:  12 April 2016

J.H. Seiradakis ,
A. Karastergiou ,
M. Kramer  and
D. Psaltis
J.H. Seiradakis
Affiliation:
University of Thessaloniki, Department of Physics, Section of Astrophysics, Astronomy and Mechanics, GR-540 06 Thessaloniki, Greece
A. Karastergiou
Affiliation:
University of Thessaloniki, Department of Physics, Section of Astrophysics, Astronomy and Mechanics, GR-540 06 Thessaloniki, Greece
M. Kramer
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Germany
D. Psaltis
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS. 51, Cambridge, Ma 02138, USA

Abstract

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We have used power spectra analysis on high frequency (1.4 GHz) data, obtained with the Effelsberg 100m radio-telescope in order to investigate the emission characteristics of pulsars. This analysis has not only revealed the prominent periodicities of the fluctuating components, but has also proven a powerful tool for identifying weak and often unresolved components and their longitudinal location within the integrated pulsar profile. Furthermore, close examination of the properties of the fluctuating components indicates physical connections between them, giving new insight to the structure of the emitting region.

Type
Part 3. Studies of Radio Emission
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 177 - 178
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Kramer, M. 1994, A&AS 107, 527 Google Scholar
Seiradakis, J.H., Gil, J.A., Graham, D.A., et al. 1995 A&AS 111, 205 Google Scholar