3D Polarized Imaging of Coronal Mass Ejections: Chirality of a CME

• Published in: The Astrophysical journal 2017-12, Vol.850 (2), p.130
• Main Authors: DeForest, C. E., de Koning, C. A., Elliott, H. A.
• Format: Article
• Language: English
• Subjects: Astrophysics; Background noise; Chirality; Corona; Coronagraphs; Coronal mass ejection; Helicity; Heliosphere; Linear polarization; Magnetic fields; methods: data analysis; Observatories; Photometry; Physics; Polarimetry; polarization; Signal processing; Signal to noise ratio; Solar corona; Solar wind; Spacecraft; Subtraction; Sun: coronal mass ejections (CMEs); techniques: image processing; techniques: polarimetric; Terrestrial environments; Thomson scattering; Weather
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aa94ca

We report on a direct polarimetric determination of the chirality of a coronal mass ejection (CME), using the physics of Thomson scattering applied to synoptic polarized images from the Solar Terrestrial Relations Observatories/COR2 coronagraph. We confirmed the determination using in situ magnetic field measurements of the same CME with the ACE spacecraft. CME chirality is related to the helicity ejected from the solar corona along with the mass and field entrained in the CME. It is also important to prediction of the space-weather-relevant Z component of the CME magnetic field. Hence, remote measurement of CME chirality is an important step toward both understanding CME physics and predicting geoeffectiveness of individual CMEs. The polarimetric properties of Thomson scattering are well known and can, in principle, be used to measure the 3D structure of imaged objects in the solar corona and inner heliosphere. However, reduction of that principle to practice has been limited by the twin difficulties of background subtraction and the signal-to-noise ratio in coronagraph data. Useful measurements of the 3D structure require relative photometry at a few percent precision level in each linear polarization component of the K corona. This corresponds to a relative photometric precision of order 10−4 in direct images of the sky before subtraction of the F corona and related signal. Our measurement was enabled by recent developments in signal processing, which enable a better separation of the photometric signal from noise in the synoptic COR2 data. We discuss the relevance of this demonstration measurement to future instrument requirements, and to the future measurements of 3D structures in CMEs and other solar wind features.