Abstract
Coronal mass ejections (CMEs) are large eruptions of magnetized plasma from the Sun that play an important role in space weather. The key to understanding the fundamental physics of a CME is measurement of the plasma properties within heliocentric distances of \(< 20~\mathrm{R}_{\odot }\). Faraday rotation, a radioastronomical propagation measurement, is an extremely valuable diagnostic for studying CMEs. Faraday rotation measurements [RM] contain information on the magnetic field in the medium causing the Faraday rotation. Recent observations of CME-induced Faraday rotation (e.g., Howard et al. in Astrophys. J. 831, 208, 2016; Kooi et al. in Solar Phys. 292, 56, 2017; Bisi et al. in EGU General Assembly Conference Abstracts, 13243, 2017) have all been restricted to a single line of sight (LOS) and, therefore, limited to providing estimates of the magnetic field strength. Modeling by Liu et al. (Astrophys. J. 665, 1439, 2007) and Jensen and Russell (Geophys. Res. Lett. 35, L02103, 2008) demonstrated that multiple LOS are necessary to recover the magnetic field strength and structure of the observed CME. We report the first successful observations of Faraday rotation through a CME using multiple lines of sight: 13 LOS across seven target radio fields. We made these radio observations using the Karl G. Jansky Very Large Array (VLA) at \(1-2\) GHz frequencies in the triggered operation mode on 31 July 2015, using a constellation of cosmic radio sources through the solar corona at heliocentric distances of \(8.2-19.5~\mathrm{R}_{\odot }\). For LOS within \(10~\mathrm{R}_{\odot }\), the CME’s contribution to the measured RM was \(\approx 0\) to −20 rad m−2, a significant enhancement over the coronal contribution. We assumed a force-free flux-rope structure for the CME’s magnetic field and explored three separate models for the CME’s plasma density: constant density, thin shell, and thick shell. The plasma densities and axial magnetic field strengths for the three models ranged over \(5.4-6.4\times 10^{3}\) cm−3 and \(26-35\) mG, respectively. Further, using all 13 LOS, we successfully determined the CME’s orientation and helicity.
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Acknowledgements
This work was supported at the U.S. Naval Research Laboratory by the Jerome and Isabella Karle Distinguished Scholar Fellowship program and by 6.1 base funding. Student research was supported by the Naval Research Enterprise Internship Program (NREIP), Science and Engineering Apprenticeship Program (SEAP), and NRL Research Internship Program for HBCU/ MI/TCU Undergraduates and Graduates. The Karl G. Jansky Very Large Array is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The SOHO LASCO data used here are produced by a consortium of the Naval Research Laboratory (USA), Max-Planck-Institut fuer Aeronomie (Germany), Laboratoire d’Astronomie (France), and the University of Birmingham (UK). SOHO is a project of international cooperation between ESA and NASA. The authors also thank the referee whose comments and insights improved the final article.
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Kooi, J.E., Ascione, M.L., Reyes-Rosa, L.V. et al. VLA Measurements of Faraday Rotation Through a Coronal Mass Ejection Using Multiple Lines of Sight. Sol Phys 296, 11 (2021). https://doi.org/10.1007/s11207-020-01755-4
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DOI: https://doi.org/10.1007/s11207-020-01755-4