Radio Remote Sensing of the Solar Corona with the EVLA

Details Radio Remote Sensing of the Solar Corona with the EVLA Radio Remote Sensing of the Solar Corona with the EVLA

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542207w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #422.07; Bulletin of the American Astronomical Society, Vol. 42, p.292

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Scientific paper

A number of studies have used the VLA to measure Faraday rotation due to the solar corona, and thus remotely sense the coronal plasma structure (e.g. ApJ 668, 5202, 2007). However, these studies have been limited to a closest angular approach of about 5 solar radii from the Sun (1.25 degrees). At closer heliocentric distances, the system temperature at the 1.4 GHz observing frequency is unacceptably enhanced due to the Sun in the distant sidelobes. In future studies we would like to use the EVLA to probe the inner corona, from 2-5 solar radii. Observations at 5 GHz will be less affected by solar system temperature increase because of smaller antenna beams. We performed test measurements with EVLA antennas to determine the solar contribution to the system temperature as a function of angular distance from the sun at 5 GHz. We report our results in three regions of interest: at 2-3 solar radii (32-48') the system temperature varies from 100-350 K, at 3-5 solar radii (48-80') the system temperature is 50-100 K, and for separations greater than 5 solar radii (80') the system temperature levels off to the cold-sky EVLA Tsys value of 39 K. We also present a model for the system temperature due to the quiet sun in the sidelobes, which adequately reproduces the measured Tsys values. These results demonstrate the feasibility of future EVLA Faraday rotation, and other propagation measurements in the inner corona. This research was supported at the University of Iowa by grant ATM-0354782 from the National Science Foundation.

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