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Article: Jupiter's X-ray Emission During the 2007 Solar Minimum

TitleJupiter's X-ray Emission During the 2007 Solar Minimum
Authors
KeywordsAurora
Charge Exchange
Jupiter
Solar Cycle
X-ray
XMM-Newton
Issue Date2020
Citation
Journal of Geophysical Research: Space Physics, 2020, v. 125, n. 6, article no. e2019JA027219 How to Cite?
AbstractThe 2007–2009 solar minimum was the longest of the space age. We present the first of two companion papers on Chandra and XMM-Newton X-ray campaigns of Jupiter through February–March 2007. We find that low solar X-ray flux during solar minimum causes Jupiter's equatorial regions to be exceptionally X-ray dim (0.21 GW at minimum; 0.76 GW at maximum). While the Jovian equatorial emission varies with solar cycle, the aurorae have comparably bright intervals at solar minimum and maximum. We apply atomic charge exchange models to auroral spectra and find that iogenic plasma of sulphur and oxygen ions provides excellent fits for XMM-Newton observations. The fitted spectral S:O ratios of 0.4–1.3 are in good agreement with in situ magnetospheric S:O measurements of 0.3–1.5, suggesting that the ions that produce Jupiter's X-ray aurora predominantly originate inside the magnetosphere. The aurorae were particularly bright on 24–25 February and 8–9 March, but these two observations exhibit very different spatial, spectral, and temporal behavior; 24–25 February was the only observation in this campaign with significant hard X-ray bremsstrahlung from precipitating electrons, suggesting this may be rare. For 8–9 March, a bremsstrahlung component was absent, but bright oxygen O6+ lines and best-fit models containing carbon, point to contributions from solar wind ions. This contribution is absent in the other observations. Comparing simultaneous Chandra ACIS and XMM-Newton EPIC spectra showed that ACIS systematically underreported 0.45- to 0.6-keV Jovian emission, suggesting quenching may be less important for Jupiter's atmosphere than previously thought. We therefore recommend XMM-Newton for spectral analyses and quantifying opacity/quenching effects.
Persistent Identifierhttp://hdl.handle.net/10722/334660
ISSN
2023 Impact Factor: 2.6
2023 SCImago Journal Rankings: 0.845
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorDunn, W. R.-
dc.contributor.authorBranduardi-Raymont, G.-
dc.contributor.authorCarter-Cortez, V.-
dc.contributor.authorCampbell, A.-
dc.contributor.authorElsner, R.-
dc.contributor.authorNess, J. U.-
dc.contributor.authorGladstone, G. R.-
dc.contributor.authorFord, P.-
dc.contributor.authorYao, Z.-
dc.contributor.authorRodriguez, P.-
dc.contributor.authorClark, G.-
dc.contributor.authorParanicas, C.-
dc.contributor.authorFoster, A.-
dc.contributor.authorBaker, D.-
dc.contributor.authorGray, R.-
dc.contributor.authorBadman, S. V.-
dc.contributor.authorRay, L. C.-
dc.contributor.authorBunce, E. J.-
dc.contributor.authorSnios, B.-
dc.contributor.authorJackman, C. M.-
dc.contributor.authorRae, I. J.-
dc.contributor.authorKraft, R.-
dc.contributor.authorRymer, A.-
dc.contributor.authorLathia, S.-
dc.contributor.authorAchilleos, N.-
dc.date.accessioned2023-10-20T06:49:44Z-
dc.date.available2023-10-20T06:49:44Z-
dc.date.issued2020-
dc.identifier.citationJournal of Geophysical Research: Space Physics, 2020, v. 125, n. 6, article no. e2019JA027219-
dc.identifier.issn2169-9380-
dc.identifier.urihttp://hdl.handle.net/10722/334660-
dc.description.abstractThe 2007–2009 solar minimum was the longest of the space age. We present the first of two companion papers on Chandra and XMM-Newton X-ray campaigns of Jupiter through February–March 2007. We find that low solar X-ray flux during solar minimum causes Jupiter's equatorial regions to be exceptionally X-ray dim (0.21 GW at minimum; 0.76 GW at maximum). While the Jovian equatorial emission varies with solar cycle, the aurorae have comparably bright intervals at solar minimum and maximum. We apply atomic charge exchange models to auroral spectra and find that iogenic plasma of sulphur and oxygen ions provides excellent fits for XMM-Newton observations. The fitted spectral S:O ratios of 0.4–1.3 are in good agreement with in situ magnetospheric S:O measurements of 0.3–1.5, suggesting that the ions that produce Jupiter's X-ray aurora predominantly originate inside the magnetosphere. The aurorae were particularly bright on 24–25 February and 8–9 March, but these two observations exhibit very different spatial, spectral, and temporal behavior; 24–25 February was the only observation in this campaign with significant hard X-ray bremsstrahlung from precipitating electrons, suggesting this may be rare. For 8–9 March, a bremsstrahlung component was absent, but bright oxygen O6+ lines and best-fit models containing carbon, point to contributions from solar wind ions. This contribution is absent in the other observations. Comparing simultaneous Chandra ACIS and XMM-Newton EPIC spectra showed that ACIS systematically underreported 0.45- to 0.6-keV Jovian emission, suggesting quenching may be less important for Jupiter's atmosphere than previously thought. We therefore recommend XMM-Newton for spectral analyses and quantifying opacity/quenching effects.-
dc.languageeng-
dc.relation.ispartofJournal of Geophysical Research: Space Physics-
dc.subjectAurora-
dc.subjectCharge Exchange-
dc.subjectJupiter-
dc.subjectSolar Cycle-
dc.subjectX-ray-
dc.subjectXMM-Newton-
dc.titleJupiter's X-ray Emission During the 2007 Solar Minimum-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1029/2019JA027219-
dc.identifier.scopuseid_2-s2.0-85085308951-
dc.identifier.volume125-
dc.identifier.issue6-
dc.identifier.spagearticle no. e2019JA027219-
dc.identifier.epagearticle no. e2019JA027219-
dc.identifier.eissn2169-9402-
dc.identifier.isiWOS:000545696000042-

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