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<p>We report long duration observations of changes in the 5303&#xa0;Å (Fe XIV) solar coronal emission line parameters at heliocentric distance <InlineEquation ID="IEq1"> <EquationSource Format="MATHML"><math> <mi>r</mi> <mo>≈</mo> <mn>1.07</mn> <msub> <mtext>R</mtext> <mo>⊙</mo> </msub> </math></EquationSource> <EquationSource Format="TEX">$r{\approx }1.07\text{R}_{\odot }$</EquationSource> </InlineEquation>, using data obtained with the Visible Line Emission Coronagraph (VELC) onboard Aditya-L1 in the sit and stare mode. The observed changes are due to a flare near the east limb of the Sun. The intensity and width of the line are enhanced during the event. There is no change in the Doppler velocity. Our analysis indicates that the increase in line width is most likely due to an increase in temperature due to flare heating.</p>

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Spectroscopic Observations of Temporal Changes in the 5303 Å Solar Coronal Emission Line During a Flare

  • 期刊论文

  • 发表日期：

    2025年11月20日

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  • R. Ramesh,
  • V. Muthu Priyal,
  • Jagdev Singh,
  • K. Sasikumar Raja

摘要

We report long duration observations of changes in the 5303 Å (Fe XIV) solar coronal emission line parameters at heliocentric distance r ≈ 1.07 R ⊙ $r{\approx }1.07\text{R}_{\odot }$ , using data obtained with the Visible Line Emission Coronagraph (VELC) onboard Aditya-L1 in the sit and stare mode. The observed changes are due to a flare near the east limb of the Sun. The intensity and width of the line are enhanced during the event. There is no change in the Doppler velocity. Our analysis indicates that the increase in line width is most likely due to an increase in temperature due to flare heating.