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Coronal magnetic fields are well known to be one of the crucial parametersdefining coronal physics and space weather. However, measuring the globalcoronal magnetic fields remains challenging. The polarization properties ofcoronal radio emissions are sensitive to coronal magnetic fields. While theycan prove to be useful probes of coronal and heliospheric magnetic fields,their usage has been limited by technical and algorithmic challenges. Wepresent a robust algorithm for precise polarization calibration and imaging oflow-radio frequency solar observations and demonstrate it on data from theMurchison Widefield Array, a Square Kilometer Array (SKA) precursor. Thisalgorithm is based on the Measurement Equation framework, which forms the basisof all modern radio interferometric calibration and imaging. It delivers highdynamic range and fidelity full Stokes solar radio images with instrumentalpolarization leakages $<1\%$, on par with general astronomical radio imaging,and represents the state-of-the-art. Opening up this rewarding, yet unexplored,phase space will enable multiple novel science investigations and offerconsiderable discovery potential. Examples include detection of low-level ofcircularly polarization from thermal coronal emission to estimate large-scalequiescent coronal fields; polarization of faint gyrosynchrotron emissions fromcoronal mass ejections for robust estimation of plasma parameters; anddetection of the first-ever linear polarization at these frequencies. Thismethod has been developed with the SKA in mind and will enable a new era ofhigh fidelity spectro-polarimetric snapshot solar imaging at low-radiofrequencies.

Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: The Algorithm