Radio propagation and scintillation

Details Radio propagation and scintillation Radio propagation and scintillation

Apr 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ecgou..30..151w&link_type=abstract

Goutelas 2007; Low Frequency Radioastroomy: Instrumentation, Science, Projects. Proceedings of the conference held 4-8 June 2007

Physics

Radio Propagation, Scintillation, Plasma Properties, Non-Magnetized Plasmas, Magnetized Plasmas, Refractive Index, Plasma Frequency, Astrophysical Plasmas, Non-Uniform Plasmas, Temporal Broadening, Phase Screen Model, Weak Scattering, Strong Scattering

Scientific paper

The signals we collect from a celestial radio source have not only had a long journey, they have probably had a rough one. Throughout the trip they have passed through numerous regimes of tenuous but turbulent plasma, including the immediate vicinity of the source itself, possibly the complex interstellar medium, the interplanetary medium and finally the Earth's own ionosphere, and each of these introduces its own imprint on the radiation field. Sometimes these imprints can be obvious, such as the scatter broadening of compact sources, and sometimes subtle, such as the time-frequency correlations in pulsar dynamic spectra. Here we investigate some of the basic physics behind these phenomena and derive some simple `rule-of-thumb' relationships that help the astronomer decide whether propagation effects are important or not for a particular observation.

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