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<p>The Sun’s differential rotation is a significant phenomenon that sets off the twisting of the magnetic field in loops, which in turn results in the formation of different solar activity indicators, such as sunspots (SSNs), flares, coronal mass ejections (CMEs). In this work, the differential rotation of the solar coronal region is investigated utilizing Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) full-disk images during 2011 and 2021 (including a portion of Solar Cycle 24 and Cycle 25 ascending phase) at the 21.1&#xa0;nm wavelength. The equatorial region exhibits the highest average sidereal rotation rate (14.6°/day) decreasing to 13.6°/day towards the poles of both hemispheres. This study reveals that the average and equatorial rotation rates of the coronal region show patterns similar to solar activity during Solar Cycles 24 and 25. Abrupt variations in these rotation rates seem to correspond with the phases of the solar activity cycle. This indicates that abrupt variations in these rotation rates might be driven by fluctuations in solar activity. The analysis reveals that the 21.1&#xa0;nm EUV corona exhibits a slight change in equatorial rotation rate and rotational gradient as compared to the 19.3&#xa0;nm line. We also noticed that the present work shows negligible north-south asymmetry from 2011 to 2021. Furthermore, the rotational gradient is lower than that of the solar photosphere, suggesting it decreases with increasing altitude/temperature from the photosphere to the corona. We believe that the study of rotational parameters may be essential to map the magnetic behavior of the solar atmosphere. Furthermore, rotational parameters may help train AI models that will eventually be helpful in forecasting solar activity indicators.</p>

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Estimation of the Coronal Differential Rotation Using SDO/AIA 21.1 nm Observations

  • 期刊论文

  • 发表日期：

    2025年11月13日

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  • Jaidev Sharma,
  • Ashok Kumar,
  • Satish Chandra,
  • Hari Om Vats,
  • Sudhansh Sharma

摘要

The Sun’s differential rotation is a significant phenomenon that sets off the twisting of the magnetic field in loops, which in turn results in the formation of different solar activity indicators, such as sunspots (SSNs), flares, coronal mass ejections (CMEs). In this work, the differential rotation of the solar coronal region is investigated utilizing Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) full-disk images during 2011 and 2021 (including a portion of Solar Cycle 24 and Cycle 25 ascending phase) at the 21.1 nm wavelength. The equatorial region exhibits the highest average sidereal rotation rate (14.6°/day) decreasing to 13.6°/day towards the poles of both hemispheres. This study reveals that the average and equatorial rotation rates of the coronal region show patterns similar to solar activity during Solar Cycles 24 and 25. Abrupt variations in these rotation rates seem to correspond with the phases of the solar activity cycle. This indicates that abrupt variations in these rotation rates might be driven by fluctuations in solar activity. The analysis reveals that the 21.1 nm EUV corona exhibits a slight change in equatorial rotation rate and rotational gradient as compared to the 19.3 nm line. We also noticed that the present work shows negligible north-south asymmetry from 2011 to 2021. Furthermore, the rotational gradient is lower than that of the solar photosphere, suggesting it decreases with increasing altitude/temperature from the photosphere to the corona. We believe that the study of rotational parameters may be essential to map the magnetic behavior of the solar atmosphere. Furthermore, rotational parameters may help train AI models that will eventually be helpful in forecasting solar activity indicators.