TY - JOUR
T1 - Coronal Cavity Magnetic Fields Inferred by DKIST/CryoNIRSP
AU - Wraback, Elizabeth M.
AU - Farid, Samaiyah
AU - Schad, Thomas A.
AU - Bąk-Stȩślicka, Urszula
AU - de Toma, Giuliana
AU - Fan, Yuhong
AU - Gibson, Sarah E.
AU - Paz Miralles, Mari
AU - Zhang, Jie
AU - Dhakal, Suman K.
N1 - Publisher Copyright:
© 2026. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the https://creativecommons.org/licenses/by/4.0/. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
PY - 2026/7/1
Y1 - 2026/7/1
N2 - Coronal cavities are low-density regions in the solar corona surrounding prominences that often erupt into coronal mass ejections. Therefore, understanding the magnetic field in these preeruptive structures is important for understanding the process of magnetic energy storage and release in the solar corona, with implications for space weather modeling and predictions. The Daniel K. Inouye Solar Telescope/CryoNIRSP instrument acquired spectropolarimetric observations of the Fe xiii 10747 Å forbidden emission line in two coronal cavities, one on the northwest limb on 2025 August 8 and the other on the southwest limb on 2025 October 5. For the first time, we detect the circularly polarized emission in the Stokes V parameter in the coronal cavities and their embedded structures, which could be resolved such that the line-of-sight (LOS) magnetic field intensity could be estimated using the weak-field approximation. It is found that the inferred LOS magnetic field strength varies from ∼5 to 20 G in the cavity, with the strongest field strength above the prominence in the hornlike substructure of the cavity.
AB - Coronal cavities are low-density regions in the solar corona surrounding prominences that often erupt into coronal mass ejections. Therefore, understanding the magnetic field in these preeruptive structures is important for understanding the process of magnetic energy storage and release in the solar corona, with implications for space weather modeling and predictions. The Daniel K. Inouye Solar Telescope/CryoNIRSP instrument acquired spectropolarimetric observations of the Fe xiii 10747 Å forbidden emission line in two coronal cavities, one on the northwest limb on 2025 August 8 and the other on the southwest limb on 2025 October 5. For the first time, we detect the circularly polarized emission in the Stokes V parameter in the coronal cavities and their embedded structures, which could be resolved such that the line-of-sight (LOS) magnetic field intensity could be estimated using the weak-field approximation. It is found that the inferred LOS magnetic field strength varies from ∼5 to 20 G in the cavity, with the strongest field strength above the prominence in the hornlike substructure of the cavity.
KW - Quiescent solar prominence (1321)
KW - Solar magnetic fields (1503)
KW - Spectropolarimetry (1973)
UR - https://www.scopus.com/pages/publications/105042525718
U2 - 10.3847/2041-8213/ae7b33
DO - 10.3847/2041-8213/ae7b33
M3 - Article
AN - SCOPUS:105042525718
SN - 2041-8205
VL - 1005
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L8
ER -