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The Low-Frequency Solar Corona in Circular Polarization

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Abstract

We present spectropolarimetric imaging observations of the solar corona at low frequencies (80 – 240 MHz) using the Murchison Widefield Array (MWA). These images are the first of their kind, and we introduce an algorithm to mitigate an instrumental artifact by which the total intensity signal contaminates the polarimetric images due to calibration errors. We then survey the range of circular polarization (Stokes \(V\)) features detected in over 100 observing runs near solar maximum during quiescent periods. First, we detect around 700 compact polarized sources across our dataset with polarization fractions ranging from less than 0.5% to nearly 100%. These sources exhibit a positive correlation between polarization fraction and total intensity, and we interpret them as a continuum of plasma emission noise storm (Type I burst) continua sources associated with active regions. Second, we report a characteristic “bullseye” structure observed for many low-latitude coronal holes in which a central polarized component is surrounded by a ring of the opposite sense. The central component does not match the sign expected from thermal bremsstrahlung emission, and we speculate that propagation effects or an alternative emission mechanism may be responsible. Third, we show that the large-scale polarimetric structure at our lowest frequencies is reasonably well-correlated with the line-of-sight (LOS) magnetic field component inferred from a global potential field source surface (PFSS) model. The boundaries between opposite circular polarization signs are generally aligned with polarity inversion lines in the model at a height roughly corresponding to that of the radio limb. This is not true at our highest frequencies, however, where the LOS magnetic field direction and polarization sign are often not straightforwardly correlated.

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Acknowledgements

This work was primarily supported by the Australian Government through an Endeavour Postgraduate Scholarship. P. McCauley acknowledges the Asian Office of Aerospace Research and Development (AOARD) of the United States Air Force Office of Scientific Research (AFOSR) for travel support through the Windows on Science (WOS) program. I. Cairns and J. Morgan acknowledge support from AFOSR grants FA9550-18-1-0671 and FA9550-18-1-0473, respectively. We thank Don Melrose and Sarah Gibson for helpful discussions. We also thank the anonymous referee for a careful reading and constructive comments. This scientific work makes use of the Murchison Radio-astronomy Observatory (MRO), operated by the Commonwealth Scientific and Industrial Research Organisation (CSIRO). We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the operation of the MWA is provided by the Australian Government’s National Collaborative Research Infrastructure Strategy (NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the Pawsey Supercomputing Centre, which is supported by the Western Australian and Australian Governments. The SDO is a National Aeronautics and Space Administration (NASA) satellite, and we acknowledge the AIA and HMI science teams for providing open access to data and software. This research has also made use of NASA’s Astrophysics Data System (ADS) and the Virtual Solar Observatory (VSO, Hill et al. 2009).

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McCauley, P.I., Cairns, I.H., White, S.M. et al. The Low-Frequency Solar Corona in Circular Polarization. Sol Phys 294, 106 (2019). https://doi.org/10.1007/s11207-019-1502-y

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