Volume 404, Number 2, June III 2003
|Page(s)||557 - 567|
|Section||Interstellar and circumstellar matter|
|Published online||02 June 2003|
Measurements of the interstellar turbulent plasma spectrum of PSR B0329+54 using multi-frequency observations of interstellar scintillation
Pushchino Radioastronomy Observatory of Lebedev Physical Institute, 142290 Pushchino, Russia, and Isaac Newton Institute of Chile, Pushchino Branch
2 Hochschule Niederrhein, Reinarzstr. 49, 47805 Krefeld, Germany
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
4 Oberlin College, OH 44074, Oberlin, USA
5 University of Manchester, Jodrell Bank Observatory, Macclesfield SK11 9DL, UK
Corresponding author: W. Sieber, email@example.com
Accepted: 21 March 2003
Interstellar scintillation multi-frequency observations of PSR 0329+54 in the frequency range from 102 MHz to 5 GHz were analysed to estimate the spectrum of interstellar plasma inhomogeneities in the direction of this pulsar. Based on the theory of diffractive scintillation, the composite structure function of phase fluctuations covering a large range of turbulence scales was constructed. We found that the spectrum is well described by a power law with for scales from 106 to 109 m, which differs from the value known for a Kolmogorov spectrum. We can, however, within the accuracy of our data not exclude a Kolmogorov spectrum. It became also clear that angular refraction of emission must be taken into account to fit the data points at all observing frequencies. The size of the irregularities responsible for the angular refraction is estimated to be about m. They can be identified with clouds of neutral hydrogen that can be considered as holes of electron density.
Key words: stars: pulsars: general / turbulence / ISM: structure / stars: pulsars: individual: PSR B0329+54
© ESO, 2003
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