Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST Journal Article uri icon

Overview

abstract

  • Abstract; We present high-resolution observations of a C4.1-class solar flare (SOL2023-05-03T20:53) in AR 13293 from the Visible Spectro-Polarimeter (ViSP) and Visible Broadband Imager (VBI) instruments at the DKIST. The fast cadence, good resolution, and high polarimetric sensitivity of ViSP data provide a unique opportunity to explore the photospheric magnetic fields before and during the flare. We infer the magnetic field vector in the photosphere from the Fe i 6302 Å line using Milne–Eddington inversions. Combined analysis of the inverted data and VBI images reveals the presence of two opposite polarity pores exhibiting rotational motion both prior to and throughout the flare event. Data-driven simulations further reveal a complex magnetic field topology above the rotating pores, including a null-point-like configuration. We observed a 30% relative change in the horizontal component (δ; F; ; h; ) of Lorentz force at the flare peak time and roughly no change in the radial component. We find that the changes in δ; F; ; h; are the most likely driver of the observed pore rotation. These findings collectively suggest that the back reaction of magnetic field line reconfiguration in the corona may influence the magnetic morphology and rotation of pores in the photosphere on a significantly smaller scale.

publication date

  • September 1, 2024

has restriction

  • gold

Date in CU Experts

  • October 16, 2024 9:13 AM

Full Author List

  • Yadav R; Kazachenko MD; Afanasyev AN; Cauzzi G; Reardon K

author count

  • 5

Other Profiles

International Standard Serial Number (ISSN)

  • 2041-8205

Electronic International Standard Serial Number (EISSN)

  • 2041-8213

Additional Document Info

start page

  • L10

end page

  • L10

volume

  • 973

issue

  • 1