Observations of Magnetospheric Solar Wind Charge Exchange

Ringuette, R.; Kuntz, K. D.; Koutroumpa, D.; Kaaret, P.; LaRocca, D.; Richardson, J.

doi:10.3847/1538-4357/acf3e2

Cited by 3 publications

(3 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Apart from the temporal variations, SWCX also exhibits spatial variations (e.g., Fujimoto et al 2007;Ringuette et al 2023). Here we investigate its correlation in ecliptic latitude by dividing the clean sample into low-latitude (β low ≡ |β| < 30°) and high-latitude (β high ≡ |β| 30°) subsamples.…”

Section: Spatial Dependence Of Swcx On Ecliptic Latitudementioning

confidence: 99%

The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O vii, O viii, and Fe L-shell Transitions

Pan,

Qu,

Bregman

et al. 2024

ApJS

View full text Add to dashboard Cite

The XMM-Newton Line Emission Analysis Program (X-LEAP) is designed to study diffuse X-ray emissions from the Milky Way (MW) hot gas, as well as emissions from the foreground solar wind charge exchange (SWCX). This paper presents an all-sky survey of spectral feature intensities corresponding to the O vii, O viii, and iron L-shell (Fe-L) emissions. These intensities are derived from 5418 selected XMM-Newton observations with long exposure times and minimal contamination from point or extended sources. For 90% of the measured intensities, the values are within ≈2–18 photons cm−2 s−1 sr−1 (line unit (LU)), ≈0–8 LU, and ≈0–9 LU, respectively. We report long-term variations in O vii and O viii intensities over 22 yr, closely correlating with the solar cycle and attributed to SWCX emissions. These variations contribute ∼30% and ∼20% to the observed intensities on average and peak at ≈4 and ≈1 LU during solar maxima. We also find evidence of short-term and spatial variations in SWCX, indicating the need for a more refined SWCX model in future studies. In addition, we present SWCX- and absorption-corrected all-sky maps for a better view of the MW hot gas emission. These maps show a gradual decrease in oxygen intensity moving away from the Galactic center and a concentration of Fe-L intensity in the Galactic bubbles and disk.

show abstract

Section: Spatial Dependence Of Swcx On Ecliptic Latitudementioning

confidence: 99%

The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O vii, O viii, and Fe L-shell Transitions

Pan,

Qu,

Bregman

et al. 2024

ApJS

View full text Add to dashboard Cite

show abstract

“…Regardless of the line of sight, X-ray emission produced by SWCX in interplanetary space contaminates every astrophysical observation. However, the main emission spectral lines of SWCX also happen to be an important diagnostic method for astrophysical plasmas [10].…”

Section: Introductionmentioning

confidence: 99%

Solar Wind Charge-Exchange X-ray Emissions from the O<sup>5+</sup> Ions in the Earth’s Magnetosheath

Zhang,

He,

Zhang

et al. 2024

Preprint

View full text Add to dashboard Cite

The spectra and global distributions of the X-ray emissions generated by the solar wind charge-exchange (SWCX) process in the terrestrial magnetosheath are investigated based on a global hybrid model and a global geocoronal hydrogen model. The solar wind O6+ ions which are the primary charge state for oxygen ions in solar wind are considered. The line emissivity of the charge-exchange born O5+ ions are calculated by Spectral Analysis System for Astrophysical and Lab oratory (SASAL). It is found that the emission lines from the O5+ ranges from 105.607 to 118.291 eV with the strong line at 107.047 eV. We then simulated the magnetosheath X-ray emission intensity distributions with a virtual camera at two positions of north pole and dusk at six stages during the passing of a perpendicular interplanetary shock combined with a tangential discontinuity structure through the Earth’s magnetosphere. During this process, the X-ray emission intensity increases with time, and the maximum value is 27.11 keV cm-2 s-1 sr-1 on the dayside, which is 4.5 times that before the solar wind structure reaches the Earth. A clear shock structure can be seen in the magnetosheath and moves earthward. The maximum emission intensity seen at dusk is always higher than that seen at north pole.

show abstract

“…Ishikawa et al [13] analyzed the high-resolution SWCX X-ray data obtained by the Suzaku satellite during geomagnetic storms and found time-varying changes in diffuse SXR emission related to the solar wind proton flux. Ringuette et al [14] successfully separated SWCX emissions from the X-ray spectrum obtained by HaloSat at low ecliptic latitudes. Zhang et al [15] compared the ROSAT all-sky survey (RASS) data and the Quiet method (a quiet observation data method, which uses the same satellite to observe the same target for a long time) using XMM-Newton when solar wind conditions change dramatically.…”

Section: Introductionmentioning

confidence: 99%

Solar Wind Charge-Exchange X-ray Emissions from the O5+ Ions in the Earth’s Magnetosheath

Zhang,

He,

Zhang

et al. 2024

Remote Sensing

View full text Add to dashboard Cite

The spectra and global distributions of the X-ray emissions generated by the solar wind charge-exchange (SWCX) process in the terrestrial magnetosheath are investigated based on a global hybrid model and a global geocoronal hydrogen model. Solar wind O6+ ions, which are the primary charge state for oxygen ions in solar wind, are considered. The line emissivity of the charge-exchange-borne O5+ ions is calculated by the Spectral Analysis System for Astrophysical and Laboratory (SASAL). It is found that the emission lines from O5+ range from 105.607 to 118.291 eV with a strong line at 107.047 eV. We then simulate the magnetosheath X-ray emission intensity distributions with a virtual camera at two positions of the north pole and dusk at six stages during the passing of a perpendicular interplanetary shock combined with a tangential discontinuity structure through the Earth’s magnetosphere. During this process, the X-ray emission intensity increases with time, and the maximum value is 27.11 keV cm−2 s−1 sr−1 on the dayside, which is 4.5 times that before the solar wind structure reached the Earth. A clear shock structure can be seen in the magnetosheath and moves earthward. The maximum emission intensity seen at dusk is always higher than that seen at the north pole.

show abstract

Observations of Magnetospheric Solar Wind Charge Exchange

Cited by 3 publications

References 40 publications

The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O vii, O viii, and Fe L-shell Transitions

The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O vii, O viii, and Fe L-shell Transitions

Solar Wind Charge-Exchange X-ray Emissions from the O<sup>5+</sup> Ions in the Earth’s Magnetosheath

Solar Wind Charge-Exchange X-ray Emissions from the O5+ Ions in the Earth’s Magnetosheath

Contact Info

Product

Resources

About