Radio sounding of the circumsolar plasma using polarized pulsar pulses

Details Radio sounding of the circumsolar plasma using polarized pulsar pulses Radio sounding of the circumsolar plasma using polarized pulsar pulses

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009arep...53..252s&link_type=abstract

Astronomy Reports, Volume 53, Issue 3, pp.252-261

Astronomy and Astrophysics

Astronomy

2

96.50.Ci-, 97.60.Gb, 95.85.Bh

Scientific paper

We present the results of radio sounding observations probing the inner solar wind near the minimum of the solar-activity cycle, using polarized pulses from PSR B0525+21 and PSR B0531+21 received when the lines of sight toward these pulsars were close to the Sun. The observations were obtained in June 2005 and June 2007 on the Large Phased Array of the Lebedev Physical Institute at 111 MHz. An upper limit for the scattering of giant pulses from PSR B0531+21 due to their passage through the turbulent solar-wind plasma is determined. The arrival-time delays for pulses from PSR B0531+21 are used to derive the radial dependence of the mean density of the circumsolar plasma. The resulting density distribution indicates that the acceleration of fast, high-latitude solar-wind outflows continues to heliocentric distances of 5-10 R &sun;, where R &sun; is the solar radius. The mean plasma density at heliocentric distances of about 5 R &sun; is 1.4 × 104 cm-3, substantially lower than at the solar-activity maximum. This is associated with the presence of polar coronal holes. The Faraday rotation measure at heliocentric distances of 6-7 R &sun; is estimated. Deviations of the spatial distribution of the magnetic field from spherical symmetry are comparatively modest in the studied range of heliocentric distances.

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