Author ORCID Identifier
James McAteer:
https://orcid.org/0000-0003-1493-101X
Shuo Wang:
https://orcid.org/0000-0001-5589-0416
Jack Jenkins:
https://orcid.org/0000-0002-8975-812X
Debi Prasad Choudhary:
https://orcid.org/0000-0002-9308-3639
David Long:
https://orcid.org/0000-0003-3137-0277
Valentin Martinez Pillet:
https://orcid.org/0000-0001-7764-6895
Document Type
Journal Article
Journal Article Version
Final Version / Publisher's PDF (peer-reviewed)
Publication Date
4-1-2020
Abstract
The full 3D vector magnetic field of a solar filament prior to eruption is presented. The filament was observed with the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope in the chromospheric He i line at 10830 A on 2017 May 29 and 30. We inverted the spectropolarimetric observations with the Hanle and Zeeman Light code to obtain the chromospheric magnetic field. A bimodal distribution of field strength was found in or near the filament. The average field strength was 24 Gauss, but prior to the eruption we find the 90th percentile of field strength was 435 Gauss for the observations on May 29. The field inclination was about 67 degrees from the solar vertical. The field azimuth made an angle of about 47 degrees-65 degrees to the spine axis. The results suggest an inverse configuration indicative of a flux rope topology. He i intensity threads were found to be coaligned with the magnetic field direction. The filament had a sinistral configuration as expected for the southern hemisphere. The filament was stable on 2017 May 29 and started to rise during two observations on May 30, before erupting and causing a minor coronal mass ejection. There was no obvious change of the magnetic topology during the eruption process. Such information on the magnetic topology of erupting filaments could improve the prediction of the geoeffectiveness of solar storms.
Published in
Astrophysical Journal
DOI
10.3847/1538-4357/ab7380
Keywords
Solar magnetic fields, Quiet solar chromosphere, Solar filament eruptions, Solar filaments
Department / Organizational Unit
Astronomy
Copyright Notice
© 2020 S. Wang, J. Jenkins, V. Pillet, et al., reuse allowed according to Creative Commons license.
License for Reuse
This work is licensed under a Creative Commons Attribution 4.0 International License.
Recommended Citation
Wang, S., Jenkins, J. M., Pillet, V. M., Beck, C., Long, D. M., Choudhary, D. P., Muglach, K., & McAteer, J. (2020). Magnetic structure of an erupting filament. Astrophysical Journal, 892(2). https://doi.org/10.3847/1538-4357/ab7380