Spectroscopic Imaging of the Radio Sun with the Murchison Widefield Array Prototype

Details Spectroscopic Imaging of the Radio Sun with the Murchison Widefield Array Prototype Spectroscopic Imaging of the Radio Sun with the Murchison Widefield Array Prototype

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11b1659o&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH11B-1659

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions, [7594] Solar Physics, Astrophysics, And Astronomy / Instruments And Techniques

Scientific paper

We will present an overview of results from recent spectroscopic imaging of the solar corona using the Murchison Widefield Array (MWA) Prototype interferometer. The 32-element MWA Prototype operates between 80-300 MHz and is a precursor to the full 512-element MWA that is currently under construction in Western Australia. The combined high dynamic range imaging capability and the temporal, spectroscopic and angular resolution capabilities afforded by the MWA Prototype are already providing a wealth of new insights into the dynamic nature of the radio Sun. For example, during two separate days in late March 2010 (characterized as "quiet" to "very quiet"), we have detected modest level broad-band bursts that are similar to classic Type III bursts in their duration and peak wavelengths, but show significantly smaller spectral drift rates. On one of these days, we also detected numerous short-lived, narrow-band events whose nature is clearly non-thermal, but whose properties, to our knowledge, do not match those of any other previously reported class of burst. All of these events appear to be linked with two x-ray-bright active regions. In some cases, we also observe circularly polarized emission of opposite polarity at the burst locations, indicative of a magnetic loop structure. Our observations are ongoing, and we will use these and other new results to illustrate the powerful new capabilities for Solar and Heliospheric research that will be provided by the full MWA and other next-generation radio interferometers over the next several years.

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