Aditya-L1 and SDO Observations of a Confined X-Class Flare with an EUV Late Phase: Thermal and Nonthermal Emission, Magnetic Topology, and Flux Rope Confinement
- 1Udaipur Solar Observatory
- 2Indian Institute of Technology Gandhinagar
- 3Physical Research Laboratory
Abstract
We study a long-duration, confined X2.0-class solar flare exhibiting three distinct episodes of hard X-ray emission, along with an accompanying EUV late phase. A key highlight of this work is the novel observations from the high-resolution solar X-ray spectrometers Solar Low Energy X-ray Spectrometer and the High Energy L1 Orbiting X-ray Spectrometer on board Aditya-L1, providing insights into the evolution of thermal and nonthermal emissions. Simultaneous EUV observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly in hot channels, combined with multiband X-ray light curves, reveal a two-stage confined eruption of a large magnetic flux rope (MFR), separated by ∼10 minutes. The first stage corresponds to an M4.6 flare, while the overall event reaches X2.0 on the GOES scale. During the first phase, magnetic reconnection beneath the large EUV hot channel causes plasma heating to ∼19 MK, with a nonthermal spectral index of ∼4.3. In the second phase, characterized by external reconnection and confinement of the MFR hot channel, the temperature increases to ∼22 MK, accompanied by further hardening of the spectral index to ∼3.9. Despite MFR expansion during the impulsive phase, accompanied by strong nonthermal and pronounced plasma heating, the MFR fails to erupt because of the strong strapping force exerted by the overlying coronal loops. Importantly, the stalled eruption, together with reconnection in the higher overlying loops, results in enhanced heating within a closed magnetic configuration, with temperatures peaking at up to ∼15 MK during the late phase. The paper also provides the first observations of detectable nonthermal X-ray emission during the early EUV late phase, albeit briefly, providing direct evidence for reconnection-induced heating, likely occurring in the higher overlying coronal loops.
Versions
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BibTeX
@article{singh2026adityal1,
title = {{Aditya-L1 and SDO Observations of a Confined X-Class Flare with an EUV Late Phase: Thermal and Nonthermal Emission, Magnetic Topology, and Flux Rope Confinement}},
author = {Vishwa Vijay Singh and Bhuwan Joshi and N.P.S. Mithun},
journal = {The Astrophysical Journal},
year = {2026},
month = oct,
doi = {10.3847/1538-4357/aea6b9},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/aea6b9},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Aditya-L1 and SDO Observations of a Confined X-Class Flare with an EUV Late Phase: Thermal and Nonthermal Emission, Magnetic Topology, and Flux Rope Confinement
AU - Vishwa Vijay Singh
AU - Bhuwan Joshi
AU - N.P.S. Mithun
PY - 2026
DA - 2026/10/12
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/aea6b9
UR - https://iopscience.iop.org/article/10.3847/1538-4357/aea6b9
AB - We study a long-duration, confined X2.0-class solar flare exhibiting three distinct episodes of hard X-ray emission, along with an accompanying EUV late phase. A key highlight of this work is the novel observations from the high-resolution solar X-ray spectrometers Solar Low Energy X-ray Spectrometer and the High Energy L1 Orbiting X-ray Spectrometer on board Aditya-L1, providing insights into the evolution of thermal and nonthermal emissions. Simultaneous EUV observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly in hot channels, combined with multiband X-ray light curves, reveal a two-stage confined eruption of a large magnetic flux rope (MFR), separated by ∼10 minutes. The first stage corresponds to an M4.6 flare, while the overall event reaches X2.0 on the GOES scale. During the first phase, magnetic reconnection beneath the large EUV hot channel causes plasma heating to ∼19 MK, with a nonthermal spectral index of ∼4.3. In the second phase, characterized by external reconnection and confinement of the MFR hot channel, the temperature increases to ∼22 MK, accompanied by further hardening of the spectral index to ∼3.9. Despite MFR expansion during the impulsive phase, accompanied by strong nonthermal and pronounced plasma heating, the MFR fails to erupt because of the strong strapping force exerted by the overlying coronal loops. Importantly, the stalled eruption, together with reconnection in the higher overlying loops, results in enhanced heating within a closed magnetic configuration, with temperatures peaking at up to ∼15 MK during the late phase. The paper also provides the first observations of detectable nonthermal X-ray emission during the early EUV late phase, albeit briefly, providing direct evidence for reconnection-induced heating, likely occurring in the higher overlying coronal loops.
SN - 0004-637X
SN - 1538-4357
ER -