Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona

Abstract Routine measurements of the magnetic field of coronal mass ejections (CMEs) have been a key challenge in solar physics. Making such measurements is important both from a space weather perspective and for understanding the detailed evolution of the CME. In spite of significant efforts and multiple proposed methods, achieving this goal has not been possible to date. Here we report the first possible detection of gyroresonance emission from a CME. Assuming that the emission is happening at the third harmonic, we estimate that the magnetic field strength ranges from 7.9 to 5.6 G between 4.9 and 7.5 R ⊙ . We also demonstrate that this high magnetic field is not the average magnetic field inside the CME, but most probably is related to small magnetic islands, which are also being observed more frequently with the availability of high-resolution and high-quality white-light images.

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Publication Details

Journal
The Astrophysical Journal
Published
2025-10-10
DOI
https://doi.org/10.3847/1538-4357/ae061f
Primary Topic
Solar and Space Plasma Dynamics
Type
article
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article

Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona

Grégory Hellbourg, Akshatha K. Vydula, Mark Hodges, Nikita Kosogorov et al.
The Astrophysical Journal
Solar and Space Plasma Dynamics
article

Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona

Grégory Hellbourg, Akshatha K. Vydula, Mark Hodges, Nikita Kosogorov, Charlie Harnach, J. Hickish, Morgan Catha, Xingyao Chen, Kathryn Plant, Jayce Dowell, James W. Lamb, Nivedita Mahesh, Surajit Mondal, Daniel Jacobs, D. P. Woody, Vinand Prayag, Matthew Kolopanis, Gregg Hallinan, G. B. Taylor, Yuping Huang, Larry R. D’Addario, Katherine Elder, Sijie Yu, Dale E. Gary, Peijin Zhang, Ruby Byrne, Mike Virgin, Rick Hobbs, Casey Law, Marin M. Anderson, Sherry Chhabra, Ivey Davis, Scott White, S. Weinreb, Judd D. Bowman, David O. Hodge, A. Romero‐Wolf, Bin Chen, Jun Shi, Brian O’Donnell, Andrea Isella, Travis Powell, Ghislain Kemby, John T. Klinefelter, Andres Rizo, Jordan Trim, Thomas Zentmeyer
article en

Abstract

Abstract Routine measurements of the magnetic field of coronal mass ejections (CMEs) have been a key challenge in solar physics. Making such measurements is important both from a space weather perspective and for understanding the detailed evolution of the CME. In spite of significant efforts and multiple proposed methods, achieving this goal has not been possible to date. Here we report the first possible detection of gyroresonance emission from a CME. Assuming that the emission is happening at the third harmonic, we estimate that the magnetic field strength ranges from 7.9 to 5.6 G between 4.9 and 7.5 R ⊙ . We also demonstrate that this high magnetic field is not the average magnetic field inside the CME, but most probably is related to small magnetic islands, which are also being observed more frequently with the availability of high-resolution and high-quality white-light images.

The Astrophysical JournalVol. 992(1)
New Jersey Institute of Technology (US), California Institute of Technology (US), Jet Propulsion Laboratory (US), George Mason University (US), University of New Mexico (US), University Corporation for Atmospheric Research (US), Cobham (United Kingdom) (GB), Arizona State University (US), Rice University (US), Bournemouth University (GB)
Openalex Percentile: Top 80%
Solar and Space Plasma Dynamics
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