Reconstructing 3D Magnetic Topology of On-disk Prominence Bubbles from Stereoscopic Observations

TL;DR

This study reconstructs the 3D magnetic structure of on-disk prominence bubbles using stereoscopic observations, revealing their magnetic topology and relation to underlying magnetic fields, which was previously unverified.

Contribution

First to analyze and reconstruct the 3D magnetic topology of on-disk prominence bubbles using stereoscopic data from multiple solar observatories.

Findings

Reconstructed 3D structure of a prominence bubble with a maximum height of ~15.6 Mm.

Identified the bubble boundary as an interface between prominence dips and magnetic loops.

Suggested that bubbles form around filament barbs with underlying photospheric magnetic patches.

Abstract

Bubbles, the semi-circular voids below quiescent prominences (filaments), have been extensively investigated in the past decade. However, hitherto the magnetic nature of bubbles cannot be verified due to the lack of on-disk photospheric magnetic field observations. Here for the first time, we find and investigate an on-disk prominence bubble around a filament barb on 2019 March 18 based on stereoscopic observations from NVST, SDO, and STEREO-A. In high-resolution NVST H$\alpha$ images, this bubble has a sharp arch-like boundary and a projected width of $\thicksim$26 Mm. Combining SDO and STEREO-A images, we further reconstruct 3D structure of the bubble boundary, whose maximum height is $\thicksim$15.6 Mm. The squashing factor Q map deduced from extrapolated 3D magnetic fields around the bubble depicts a distinct arch-shaped interface with a height of $\thicksim$11 Mm, which agrees well with the reconstructed 3D structure of the observed bubble boundary. Under the interface lies a set of magnetic loops, which is rooted on a surrounding photospheric magnetic patch. To be more persuasive, another on-disk bubble on 2019 June 10 is presented as a supplement. According to these results obtained from on-disk bubble observations, we suggest that the bubble boundary corresponds to the interface between the prominence dips (barb) and the underlying magnetic loops rooted nearby. It is thus reasonable to speculate that the bubble can form around a filament barb below which there is a photospheric magnetic patch.