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Coronal Elemental Abundances During A-Class Solar Flares Observed by Chandrayaan-2 XSM

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Abstract

The abundances of low first ionization potential (FIP) elements are three to four times higher in the closed loop active corona than in the photosphere, known as the FIP effect. Observations suggest that the abundances vary in different coronal structures. Here, we use the soft X-ray spectroscopic measurements from the Solar X-ray Monitor (XSM) onboard the Chandrayaan-2 orbiter to study the FIP effect in multiple A-class flares observed during the minimum of Solar Cycle 24. Using time-integrated spectral analysis, we derive the average temperature, emission measure, and the abundances of four elements – Mg, Al, Si, and S. We find that the temperature and emission measure scales with the sub-class of flares while the measured abundances show an intermediate FIP bias for the lower A-flares (e.g. A1), while for the higher A-flares, the FIP bias is near unity. To investigate it further, we perform a time-resolved spectral analysis for a sample of the A-class flares and examine the evolution of temperature, emission measure, and abundances. We find that the abundances drop from the coronal values towards their photospheric values in the impulsive phase of the flares and, after the impulsive phase, they quickly return to the usual coronal values. The transition of the abundances from the coronal to photospheric values in the impulsive phase of the flares indicates the injection of fresh unfractionated material from the lower solar atmosphere to the corona due to chromospheric evaporation. However, explaining the quick recovery of the abundances from the photospheric to coronal values in the decay phase of the flare is challenging.

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Data Availability

The data used in this work is available at https://pradan.issdc.gov.in/ch2/.

Notes

  1. https://www.prl.res.in/ch2xsm/.

  2. https://pradan.issdc.gov.in/pradan/.

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Acknowledgments

XSM was designed and developed by the Physical Research Laboratory (PRL), Ahmedabad, with support from the Space Application Centre (SAC), Ahmedabad, the U. R. Rao Satellite Centre (URSC), Bengaluru, and the Laboratory for Electro-Optics Systems (LEOS), Bengaluru. We thank various facilities and the technical teams of all the above centers and the Chandrayaan-2 project, mission operations, and ground segment teams for their support. The Chandrayaan-2 mission is funded and managed by the Indian Space Research Organisation (ISRO). We are very grateful to Mithun N.P.S and Dr. Santosh Vadawale for the helpful scientific discussions and important suggestions for this work. L. Nama acknowledges the support and resources provided during my visit to Physical Research Laboratory (PRL), Ahmedabad, thanks to Dr. Anil Bhardwaj.

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Authors and Affiliations

  1. Department of Physics and Electronics, Christ (Deemed to be University), Hosur Main Road, Bangalore, India

    Lakshitha Nama & K. T. Paul

  2. Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat, India

    Biswajit Mondal

  3. Space Astronomy Group, U R Rao Satellite Centre, ISRO, Bengaluru, India

    S. Narendranath

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  1. Lakshitha Nama
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Lakshitha Nama and Biswajit Mondal carried out the analysis and wrote the manuscript with support from S. Narendranth. Biswajit Mondal, S. Narendranath, and K.T. Paul supervised the project.

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Appendix

Appendix

Table 2 Plasma parameters obtained from the 1T spectral analysis for all the A-class flares considered in this study. Flare IDs corresponding to peak times of the flares is given in the format SOLyyyy-mm-ddThh:mm. Approximate GOES classes are mentioned according to the peak flux of the flare in the 1 – 8 Å XSM flux. Errors correspond to the 1 \(\sigma\) limits associated with the parameters.
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Figure 9
figure 9

Evolution of temperature for the remaining sets of flares, similar to Figure 8 panels a–c.

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Figure 10
figure 10

Evolution of emission measure for the remaining sets of flares, similar to Figure 7 panels d–f.

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Figure 11
figure 11

Evolution of absolute Mg abundance for the remaining sets of flares, similar to Figure 7 panels g–i.

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Figure 12
figure 12

Evolution of absolute Al abundance for the remaining sets of flares, similar to Figure 7 panels j–l.

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Figure 13
figure 13

Evolution of absolute Si abundance for the remaining sets of flares, similar to Figure 7 panels m–o.

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Figure 14
figure 14

Evolution of absolute S abundance for the last set of flares, similar to Figure 7 panel p.

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Nama, L., Mondal, B., Narendranath, S. et al. Coronal Elemental Abundances During A-Class Solar Flares Observed by Chandrayaan-2 XSM. Sol Phys 298, 55 (2023). https://doi.org/10.1007/s11207-023-02142-5

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