A long-term spectro-temporal study of Jovian X-ray and Ultraviolet response to solar activity

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ID: 317779
2026
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Abstract
Abstract We present results from a multi-decade investigation of solar activity-driven variability in Jupiter’s emissions, using solar X-ray flux and sunspot numbers as activity indicators and ultraviolet (UV) and X-ray observations from the International Ultraviolet Explorer (IUE1978-1996) and the Chandra X-ray Observatory (2011-2021). Analysis of 51 high-SNR UV spectra spanning two solar cycles shows that Jupiter’s Lyα emission contains narrow and broad components, likely associated with the disk and auroral regions, respectively. The Lyα line and the 1330-1400 Åcontinuum flux closely follow variations in solar X-ray flux and sunspot numbers throughout all phases of two consecutive solar cycles, indicating a direct connection with solar irradiation processes, including resonant scattering of solar Lyα photons and photoelectron-driven atmospheric excitation. In contrast, ionised UV lines such as Fe ii (1608 Åand 1575 Å) show no correlation with solar activity over a solar cycle, suggesting an internal or magnetospheric origin, potentially linked to Io-derived charged particles or UV/X-ray radiation. To determine whether Jupiter’s X-ray response resembles its UV response to solar activity, we analysed 29 Chandra/HRC observations obtained during 2014-2021 and two Chandra/ACIS observations from 2011. Significant X-ray flares are detected in both ACIS and HRC lightcurves 7-15 days after major reported coronal mass ejections (CMEs). Post-CME ACIS auroral spectra reveal a significant (≥3σ) Ne8 + emission feature (∼0.94-0.98 keV) near 70-80○ latitude at Jupiter’s north pole. Owing to the high ionisation energy required (∼1.19 keV for the Ne viii to Ne ix bound-bound transition), this feature is unlikely to arise from local interactions, supporting CME-driven auroral excitation on Jupiter.
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Authors Megha Tomer, Mayukh Pahari, Anurag Baruah, Renu Malhotra
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1177
URL
https://doi.org/10.1093/mnras/stag1177
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