The Spatial Structure of Pulsar Emission Sources Determined Using Interstellar Scintillation

Details The Spatial Structure of Pulsar Emission Sources Determined Using Interstellar Scintillation The Spatial Structure of Pulsar Emission Sources Determined Using Interstellar Scintillation

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...462..289s&link_type=abstract

Astrophysical Journal v.462, p.289

Astronomy and Astrophysics

Astronomy

18

Ism: Structure, Stars: Pulsars: General

Scientific paper

Pulsars exhibit variations, or scintillation, of radio emission in time and frequency as a result of electron density inhomogeneities of the interstellar medium. Two sources with transverse separation greater than the size of the diffraction at Earth will produce independent scintillations. We use this idea to resolve pulsar magnetospheres. Here we present new observations at 102.7 MHz for four pulsars: PSR 0834+06, 1133+16, 1237+25, and 1919+21.
To study the decorrelation between pulsar signals at separated longitudes, we have calculated average cross-correlation functions in the time and frequency domains for data taken at the longitude of the leading edge of the pulse profile (as a reference) and at all other longitudes within the pulse. We present the dynamic spectra of pulsars at different longitudes of the mean profile, in which we see obvious decorrelation of the spectra at remote longitudes. From the falling cross-correlation coefficient with increasing longitudinal shift, we obtain the absolute value of the baseline ρ0 between sources. We discuss our results in the framework of different pulsar models.

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