The Solar Wind Charge-eXchange Contribution to the Local Soft X-ray Background: Model to Data Comparison in the 0.1-1.0 keV Band
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The Solar Wind Charge-eXchange Contribution to the Local Soft X-ray Background: Model to Data Comparison in the 0.1-1.0 keV Band
| Title: | The Solar Wind Charge-eXchange Contribution to the Local Soft X-ray Background: Model to Data Comparison in the 0.1-1.0 keV Band |
| Author: |
Koutroumpa, Dimitra; Lallement, Rosine; Kharchnko, Vasili; Dalgarno, Alexander
Note: Order does not necessarily reflect citation order of authors. |
| Citation: | Koutroumpa, Dimitra, Rosine Lallement, Vasili Kharchenko, and Alex Dalgarno. 2008. The solar wind charge-eXchange contribution to the local soft X-ray background: model to data comparison in the 0.1-1.0 keV band. Space Science Reviews 143(1-4): 217-230. |
| Full Text & Related Files: |
Delgarno - Solar Wind Charge-eXchange.pdf (279.5Kb; PDF) 
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| Abstract: | The major sources of the Soft X-ray Background (SXRB), besides distinct structures as supernovae and superbubbles (e.g. Loop I), are: (i) an absorbed extragalactic emission following a power law, (ii) an absorbed thermal component \((\sim 2×10^6)\) K) from the galactic disk and halo, (iii) an unabsorbed thermal component, supposedly at 106 K, attributed to the Local Bubble and (iv) the very recently identified unabsorbed Solar Wind Charge-eXchange (SWCX) emission from the heliosphere and the geocorona We study the SWCX heliospheric component and its contribution to observed data. In a first part, we apply a SWCX heliospheric simulation to model the oxygen lines \((\frac{3}{4} keV)\) local intensities during shadowing observations of the MBM 12 molecular cloud and a dense filament in the south galactic hemisphere with Chandra, XMM-Newton, and Suzaku telescopes. In a second part, we present a preliminary comparison of SWCX model results with ROSAT and Wisconsin surveys data in the \((\frac{1}{4} keV)\) band. We conclude that, in the \((\frac{3}{4} keV)\) band, the total local intensity is entirely heliospheric, while in the \((\frac{1}{4} keV)\) band, the heliospheric component seems to contribute significantly to the local SXRB intensity and has potentially a strong influence on the interpretation of the ROSAT and Wisconsin surveys data in terms of Local Bubble hot gas temperature. |
| Published Version: | doi:10.1007/s11214-008-9381-9 |
| Other Sources: | http://arXiv.org/pdf/0805.3212 |
| Terms of Use: | This article is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#OAP |
| Citable link to this page: | http://nrs.harvard.edu/urn-3:HUL.InstRepos:5131506 |
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