Analysis of Solar Flare and Sunspots on 4th Jan 2025 and Their Effects on Space Weather

TL;DR

This study analyzes the 4 January 2025 X1.8 solar flare in AR 13947 using a SunPy-based, multi-instrument approach to trace from magnetic precursors to heliospheric consequences. Through GOES X-ray flux, SDO/AIA/HMI, SUIT, STIX, e-CALLISTO, and LASCO data, it reconstructs a coherent eruption sequence featuring impulsive energy release, non-thermal particle acceleration, coronal heating across multiple temperatures, coronal dimming, and a Type II radio burst. The results quantify the flare energetics (E_X ≈ 4πD^2 ∫F dt with E_X ≈ 3×10^29 erg) and constrain the coronal shock speed (≈556 km s^{-1}), while the CME trajectory remains northwest-directed and Earth-ward impact is minimal. The work highlights the importance of multi-instrument data fusion for reliable space-weather forecasting, linking photospheric magnetic evolution and sunspot morphology to eruption dynamics and terrestrial space-weather implications.

Abstract

Solar flares and coronal mass ejections (CMEs) are among the most energetic phenomena in the solar system, often impacting space weather and terrestrial technologies. In this study, we utilize SunPy, an open-source Python library for solar physics, to analyze solar active regions and their correlation with flare and CME events observed on 4th January 2025. Data from GOES, SDO (AIA and HMI), Solar Oribter (STIX), e-CALLISTO, Aditya L1 (SUIT), and SOHO are processed to track flare intensity, active region evolution, shock wave and CME dynamics. The analyzed flare is identified as an X1.8-class event, and our study highlights key magnetic precursors that led to it. This work enhances understanding of solar eruption precursors and supports future predictive models for space weather forecasting.

Figures (15)

• Figure 1: GOES X-ray flux on 4 January 2025, show the two channels:- 1–8$Å$ (red) and 0.5–4.0Å (blue). A peak around 12:47 UTC shows the detection of X1.8 class solar flare.
• Figure 2: Multi-thermal EUV light curves observed by SDO/AIA of the X.18 flare on January 4, 2025. Integrated intensities from 131 Å ($\sim$10 MK),171 Å ($\sim$1 MK), 193 Å ($\sim$1.5 MK), & 304 Å ($\sim$0.05 MK) channels are displayed, presenting the coupled time response of the chromosphere & corona. The 131 Å hot channel peaks around the flare maximum, whereas the cooler choromospheric & coronal channels shows delayed & more gradual evolution, corresponding plasma heating & cooling within the post-flare loop.
• Figure 3: (a)Full disk image observed by SDO/AIA 171 Å at the X1.8 flare peak time on January 4, 2025, governed by emission from the coronal plasma at $\sim$1 MK temperature.(b) Magnified view of the erupting active region (AR13947), revealing the enhanced emission from coronal loop surrounding the flare erupting site. (c) Additional magnified view showing the fine scale morphology of coronal loops & nearby plasma structure at flare peak.
• Figure 4: (a) Full disk image captured by SDO/AIA 193 Å at the X1.8 flare peak time on January 4, 2025, mainly sensitive to coronal plasma at $\sim$1.5 MK temperature, with additional influence from hotter flare plasma. (b) Magnified view of the flaring Active region (AR13947), exhibiting the enhanced coronal emission & arrangement of varying loops surrounding the flare location. (c) Additional magnified view indicating the complex morphology of coronal loops and nearby plasma structures linked with the flare.
• Figure 5: (a) Magnified view of the erupting active region (AR13947), revealing the enhanced chromospheric emission linked with the flare. (b) Additional magnified view showing the fine-scale morphology of the near surface plasma structure & ribbon-like emission emerged during the flare.