Pulsar spectra of radio emission

Free access article

Issue		Astron. Astrophys. Suppl. Ser. Volume 147, Number 2, December I 2000


Page(s)		195 - 203
DOI		http://dx.doi.org/10.1051/aas:2000298

DOI: 10.1051/aas:2000298

Astron. Astrophys. Suppl. Ser. 147, 195-203

O. Maron¹ - J. Kijak¹ - M. Kramer^2,3 - R. Wielebinski²

Send offprint request: O. Maron,
e-mail: olaf@astro.ca.wsp.zgora.pl

1 - J. Kepler Astronomical Center, Pedagogical University, Lubuska 2, PL-65-265 Zielona Góra, Poland
2 - Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
3 - University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL, UK

Received April 11; accepted September 7, 2000

Abstract:

We have collected pulsar flux density observations and compiled spectra of 281 objects. The database of Lorimer et al. (1995) has been extended to frequencies higher than 1.4 GHz and lower than 300 MHz. Our results show that above 100 MHz the spectra of the majority of pulsars can be described by a simple power law with average value of spectral index $<\alpha>$ = $-1.8~\pm~0.2$ . A rigorous analysis of spectral fitting revealed only about 10% of spectra which can be modelled by the two power law. Thus, it seems that single power law is a rule and the two power law spectrum is a rather rare exception, of an unknown origin, to this rule. We have recognized a small number of pulsars with almost flat spectrum ( $\alpha \geq -1.0$ ) in the wide frequency range (from 300 MHz to 20 GHz) as well as few pulsars with a turn-over at unusually high frequency ( $\sim$ 1 GHz).

Key words: pulsars: general -- radiation mechanisms: non-thermal

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