Coronal Magnetic Field Measurements along a Partially Erupting Filament in a Solar Flare

TL;DR

This study measures the magnetic field along a partially erupting solar filament during a flare using microwave imaging spectroscopy, providing direct insights into flux rope magnetic properties during eruptions.

Contribution

It introduces a method to directly measure magnetic field strength along an erupting filament using microwave spectral analysis, aligning observations with magnetic modeling.

Findings

Magnetic field along the filament ranges from 600-1400 Gauss.

Microwave spectral properties are consistent with nonthermal gyrosynchrotron radiation.

Results agree with magnetic field extrapolation models.

Abstract

Magnetic flux ropes are the centerpiece of solar eruptions. Direct measurements for the magnetic field of flux ropes are crucial for understanding the triggering and energy release processes, yet they remain heretofore elusive. Here we report microwave imaging spectroscopy observations of an M1.4-class solar flare that occurred on 2017 September 6, using data obtained by the Expanded Owens Valley Solar Array. This flare event is associated with a partial eruption of a twisted filament observed in H{\alpha} by the Goode Solar Telescope at the Big Bear Solar Observatory. The extreme ultraviolet (EUV) and X-ray signatures of the event are generally consistent with the standard scenario of eruptive flares, with the presence of double flare ribbons connected by a bright flare arcade. Intriguingly, this partial eruption event features a microwave counterpart, whose spatial and temporal evolution closely follow the filament seen in H{\alpha} and EUV. The spectral properties of the microwave source are consistent with nonthermal gyrosynchrotron radiation. Using spatially resolved microwave spectral analysis, we derive the magnetic field strength along the filament spine, which ranges from 600-1400 Gauss from its apex to the legs. The results agree well with the non-linear force-free magnetic model extrapolated from the pre-flare photospheric magnetogram. We conclude that the microwave counterpart of the erupting filament is likely due to flare-accelerated electrons injected into the filament-hosting magnetic flux rope cavity following the newly reconnected magnetic field lines.