Investigating The Solar Corona With Radio Observations Of Pulsars

Details Investigating The Solar Corona With Radio Observations Of Pulsars Investigating The Solar Corona With Radio Observations Of Pulsars

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..78o&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

Physics

Scientific paper

We propose to examine both the magnetic field and electron content of the solar corona via measurement of the Faraday rotation and dispersion evident in observations of background pulsar sources as they are occulted by the Sun. As we will be utilise a number of simultaneous lines of sight, that will cut different paths through the corona as the Sun rotates, we will be able to strongly constrain the global topology of both the plasma and the magnetic field. Pulsars are periodic, broadband, polarised point sources of radio waves. In December 2006 the Sun will occult, or pass close to, a number of pulsars in the Galactic plane. We have proposed to use the Parkes radio telescope in New South Wales, Australia, to observe these pulsars throughout a ten day period a two frequencies simultaneously. The purpose being to detect any excess Faraday rotation and pulse dispersion associated with the Solar corona. Although background sources have been observed through the corona successfully before; our experiment differs due to the accessibility of different simultaneous lines of sight, and our ability to measure the integrated electron content and integrated magnetic field independently. We present an outline of the intended experiments and some predictions of our expected results.

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