<p>Large solar flares (GOES M-class or higher) are usually associated with eruptions of material. However, when considering flare irradiance enhancements and dynamics such as chromospheric evaporation, potential contributions from erupted material have historically been neglected. We analyse nine eruptive M- and X-class flares from 2024 to early 2025, quantifying the relative contributions of erupted material to irradiance enhancements during the events. Atmospheric Imaging Assembly (AIA) images from four different channels had ribbon and eruption irradiance contributions separated using a semi-automated masking method. The sample-averaged percentages of excess radiated energy by erupted material over the impulsive phase were <InlineEquation ID="IEq1"> <EquationSource Format="MATHML"><math> <msubsup> <mn>10</mn> <mrow> <mo>−</mo> <mn>4</mn> </mrow> <mrow> <mo>+</mo> <mn>4</mn> </mrow> </msubsup> <mi mathvariant="normal">%</mi> </math></EquationSource> <EquationSource Format="TEX">$10^{+4}_{-4}\%$</EquationSource> </InlineEquation>, <InlineEquation ID="IEq2"> <EquationSource Format="MATHML"><math> <msubsup> <mn>24</mn> <mrow> <mo>−</mo> <mn>14</mn> </mrow> <mrow> <mo>+</mo> <mn>14</mn> </mrow> </msubsup> <mi mathvariant="normal">%</mi> </math></EquationSource> <EquationSource Format="TEX">$24^{+14}_{-14}\%$</EquationSource> </InlineEquation>, <InlineEquation ID="IEq3"> <EquationSource Format="MATHML"><math> <msubsup> <mn>21</mn> <mrow> <mo>−</mo> <mn>10</mn> </mrow> <mrow> <mo>+</mo> <mn>14</mn> </mrow> </msubsup> <mi mathvariant="normal">%</mi> </math></EquationSource> <EquationSource Format="TEX">$21^{+14}_{-10}\%$</EquationSource> </InlineEquation> and <InlineEquation ID="IEq4"> <EquationSource Format="MATHML"><math> <msubsup> <mn>13</mn> <mrow> <mo>−</mo> <mn>9</mn> </mrow> <mrow> <mo>+</mo> <mn>6</mn> </mrow> </msubsup> <mi mathvariant="normal">%</mi> </math></EquationSource> <EquationSource Format="TEX">$13^{+6}_{-9}\%$</EquationSource> </InlineEquation> for the 131 Å, 171 Å, 304 Å and 1600 Å channels, respectively. For three events that were studied in further detail, hard X-ray (HXR) imaging showed little to no signatures of nonthermal heating within the eruptions. Our results suggest that erupted material can be a significant contributor to UV irradiance enhancements during flares, with possible heating mechanisms including nonthermal particle heating, Ohmic heating, or dissipation of MHD waves. Future work may clarify the heating mechanism and evaluate the impact of eruptions on spectral variability, particularly in Sun-as-a-star and stellar flare observations.</p>

Eruption-Related Ultraviolet Irradiance Enhancements Associated with Flares

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2026年1月9日

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Luke Majury,
Marie Dominique,
Ryan Milligan,
Dana-Camelia Talpeanu,
Ingolf Dammasch,
David Berghmans

摘要

Large solar flares (GOES M-class or higher) are usually associated with eruptions of material. However, when considering flare irradiance enhancements and dynamics such as chromospheric evaporation, potential contributions from erupted material have historically been neglected. We analyse nine eruptive M- and X-class flares from 2024 to early 2025, quantifying the relative contributions of erupted material to irradiance enhancements during the events. Atmospheric Imaging Assembly (AIA) images from four different channels had ribbon and eruption irradiance contributions separated using a semi-automated masking method. The sample-averaged percentages of excess radiated energy by erupted material over the impulsive phase were $10_{- 4}^{+ 4} %$ $10^{+4}_{-4}\%$ , $24_{- 14}^{+ 14} %$ $24^{+14}_{-14}\%$ , $21_{- 10}^{+ 14} %$ $21^{+14}_{-10}\%$ and $13_{- 9}^{+ 6} %$ $13^{+6}_{-9}\%$ for the 131 Å, 171 Å, 304 Å and 1600 Å channels, respectively. For three events that were studied in further detail, hard X-ray (HXR) imaging showed little to no signatures of nonthermal heating within the eruptions. Our results suggest that erupted material can be a significant contributor to UV irradiance enhancements during flares, with possible heating mechanisms including nonthermal particle heating, Ohmic heating, or dissipation of MHD waves. Future work may clarify the heating mechanism and evaluate the impact of eruptions on spectral variability, particularly in Sun-as-a-star and stellar flare observations.