Slow pulsar scintillation and the spectrum of interstellar electron density fluctuations

Details Slow pulsar scintillation and the spectrum of interstellar electron density fluctuations Slow pulsar scintillation and the spectrum of interstellar electron density fluctuations

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.214..519g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 214, June 15, 1985, p. 519-537.

Statistics

Computation

79

Electron Density (Concentration), Interstellar Matter, Pulsars, Scintillation, Approximation, Asymptotic Methods, Inhomogeneity, Integral Equations, Power Spectra

Scientific paper

The fluctuations produced in the observed intensity of a pulsar by electron-density inhomogeneities in the interstellar medium are investigated analytically in the thin-screen approximation, considering the case where the power-law index beta = 4-6. The results of previous computations for beta less than 4, and especially for the Komogorov spectrum (KS) where beta = 11/3, are reviewed; the refractive intensity fluctuations (RIFs) at beta = 4-6 are shown to be large and independent of pulsar distance and observing wavelength; distance and wavelength scaling laws are derived for various observable parameters; and the results are compared with published observational data in graphs. A model with beta = 4.3 is found to be just as consistent with the observed wavelength dependences of the parameters as the KS model, and more consistent with the available data on slow RIFs. The length-scale range of the beta = 4.3 power-law spectrum is estimated as from 10 to the 12th to 10 to the 15th cm, as compared with from 10 to the 9th to 10 to the 15th cm for a KS.

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