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Peer-reviewedCC BY 4.0The Astrophysical Journal

Improving Solar Extreme Ultraviolet Irradiance Modeling with Differential Emission Measure Informed Spectra

  • Courtney L. Peck1,2,3
  • Shah M. Bahauddin2,4,5
  • Daniel B. Seaton1
  • Janet L. Machol2,3
  • Edward M. B. Thiemann2
  • Mark Cheung6
6 affiliations
  1. 1Southwest Research Institute
  2. 2University of Colorado
  3. 3NOAA National Centers for Environmental Information
  4. 4Department of Astronomy, New Mexico State University
  5. 5Independent University
  6. 6CSIRO Space and Astronomy
Open at sourcePDFDOICite

Abstract

Solar extreme ultraviolet (EUV) irradiance predominantly originates from the chromosphere and corona, and variations in EUV irradiance are a significant driver of space weather at Earth, causing increased satellite drag, radio communication disruptions, and reduced GPS accuracy. Since solar EUV irradiance measurements are intermittent and inhomogeneous, models are used to fill spectral and temporal gaps, typically relying on proxy-based methods that utilize linear correlations between emission originating from similar heights or temperatures in the solar atmosphere. Proxy methods can struggle to capture dynamic irradiance variations of the solar corona during flares in part due to the relative infrequency of flares on which to derive correlations and the steep temporal temperature gradients experienced during flares. This paper presents a hybrid method for modeling solar EUV irradiance utilizing forward-modeled physics-informed solar differential emission measures (DEMs) to capture the optically thin coronal emission coupled with traditional proxy-based correlation methods to capture the chromospheric and continuum emission. The model is trained and tested using inputs from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) and EUV Variability Experiment (EVE) and compared against a proxy-only method. The results demonstrate that including information from DEMs into a EUV irradiance model improves accuracy for flaring conditions, particularly for high-temperature coronal lines, where the model error is reduced by up to a factor of 3 for M- and X-class flares compared to a proxy-only model trained on the same data.

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Cite

BibTeXRIS
BibTeX
@article{peck2026improving,
  title = {{Improving Solar Extreme Ultraviolet Irradiance Modeling with Differential Emission Measure Informed Spectra}},
  author = {Courtney L. Peck and Shah M. Bahauddin and Daniel B. Seaton and Janet L. Machol and Edward M. B. Thiemann and Mark Cheung},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-4357/aea6b3},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aea6b3},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Improving Solar Extreme Ultraviolet Irradiance Modeling with Differential Emission Measure Informed Spectra
AU  - Courtney L. Peck
AU  - Shah M. Bahauddin
AU  - Daniel B. Seaton
AU  - Janet L. Machol
AU  - Edward M. B. Thiemann
AU  - Mark Cheung
PY  - 2026
DA  - 2026/10/12
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aea6b3
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aea6b3
AB  - Solar extreme ultraviolet (EUV) irradiance predominantly originates from the chromosphere and corona, and variations in EUV irradiance are a significant driver of space weather at Earth, causing increased satellite drag, radio communication disruptions, and reduced GPS accuracy. Since solar EUV irradiance measurements are intermittent and inhomogeneous, models are used to fill spectral and temporal gaps, typically relying on proxy-based methods that utilize linear correlations between emission originating from similar heights or temperatures in the solar atmosphere. Proxy methods can struggle to capture dynamic irradiance variations of the solar corona during flares in part due to the relative infrequency of flares on which to derive correlations and the steep temporal temperature gradients experienced during flares. This paper presents a hybrid method for modeling solar EUV irradiance utilizing forward-modeled physics-informed solar differential emission measures (DEMs) to capture the optically thin coronal emission coupled with traditional proxy-based correlation methods to capture the chromospheric and continuum emission. The model is trained and tested using inputs from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) and EUV Variability Experiment (EVE) and compared against a proxy-only method. The results demonstrate that including information from DEMs into a EUV irradiance model improves accuracy for flaring conditions, particularly for high-temperature coronal lines, where the model error is reduced by up to a factor of 3 for M- and X-class flares compared to a proxy-only model trained on the same data.
SN  - 0004-637X
SN  - 1538-4357
ER  -