Journal
JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
Volume 121, Issue 3, Pages 2274-2307Publisher
AMER GEOPHYSICAL UNION
DOI: 10.1002/2015JA021888
Keywords
Jupiter; X-ray; Aurora; CME; Periodicity; Jovian
Categories
Funding
- Science and Technology Facilities Council (STFC)
- NASA
- SAO of NASA [SV3-73016, NAS8-03060]
- UCL-MSSL consolidated grant, from STFC (UK)
- CNES
- Science and Technology Facilities Council Ernest Rutherford Fellowship
- STFC [ST/ I004084/1]
- UK Science and Technology Facilities Council (STFC) [ST/L000563/1]
- Natural and Environmental Research Council (NERC) [NE/L007495/1]
- Japan Society for the Promotion of Science (JSPS)
- Chandra Project
- Science and Technology Facilities Council [ST/L004399/1, ST/K000977/1, ST/N000722/1, 1338302, 1068154, ST/I004084/1, ST/L000563/1] Funding Source: researchfish
- NERC [NE/L007495/1] Funding Source: UKRI
- STFC [ST/I004084/1, ST/L000563/1, ST/L004399/1, ST/N000722/1, ST/K000977/1] Funding Source: UKRI
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We report the first Jupiter X-ray observations planned to coincide with an interplanetary coronal mass ejection (ICME). At the predicted ICME arrival time, we observed a factor of approximate to 8 enhancement in Jupiter's X-ray aurora. Within 1.5h of this enhancement, intense bursts of non-Io decametric radio emission occurred. Spatial, spectral, and temporal characteristics also varied between ICME arrival and another X-ray observation two days later. Gladstone et al. (2002) discovered the polar X-ray hot spot and found it pulsed with 45min quasiperiodicity. During the ICME arrival, the hot spot expanded and exhibited two periods: 26min periodicity from sulfur ions and 12min periodicity from a mixture of carbon/sulfur and oxygen ions. After the ICME, the dominant period became 42min. By comparing Vogt et al. (2011) Jovian mapping models with spectral analysis, we found that during ICME arrival at least two distinct ion populations, from Jupiter's dayside, produced the X-ray aurora. Auroras mapping to magnetospheric field lines between 50 and 70R(J) were dominated by emission from precipitating sulfur ions (S-7+,S-...,S-14+). Emissions mapping to closed field lines between 70 and 120R(J) and to open field lines were generated by a mixture of precipitating oxygen (O-7+,O-8+) and sulfur/carbon ions, possibly implying some solar wind precipitation. We suggest that the best explanation for the X-ray hot spot is pulsed dayside reconnection perturbing magnetospheric downward currents, as proposed by Bunce et al. (2004). The auroral enhancement has different spectral, spatial, and temporal characteristics to the hot spot. By analyzing these characteristics and coincident radio emissions, we propose that the enhancement is driven directly by the ICME through Jovian magnetosphere compression and/or a large-scale dayside reconnection event.
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