2006
DOI: 10.1051/0004-6361:20065250
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Charge-transfer induced EUV and soft X-ray emissions in the heliosphere

Abstract: Aims. We study the EUV/soft X-ray emission generated by charge transfer between solar wind heavy ions and interstellar neutral atoms and variations of the X-ray intensities and spectra with the line of sight direction, the observer location, the solar cycle phase and the solar wind anisotropies, and a temporary enhancement of the solar wind similar to the event observed by Snowden et al. (2004) during the XMM-Hubble Deep Field North exposure. Methods. Using recent observations of the neutral atoms combined wit… Show more

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Cited by 106 publications
(184 citation statements)
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References 58 publications
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“…Kuntz et al [2015] employed more sophisticated models for heliospheric plasma [Odstrcil, 2003] and neutral [Koutroumpa et al, 2006] densities to reach similar conclusions. For the purpose of magnetospheric imaging, the disparate time scales of the variations allow for the heliospheric contribution to be subtracted off.…”
Section: 1002/2016ja022348mentioning
confidence: 75%
“…Kuntz et al [2015] employed more sophisticated models for heliospheric plasma [Odstrcil, 2003] and neutral [Koutroumpa et al, 2006] densities to reach similar conclusions. For the purpose of magnetospheric imaging, the disparate time scales of the variations allow for the heliospheric contribution to be subtracted off.…”
Section: 1002/2016ja022348mentioning
confidence: 75%
“…(1) Heliospheric Solar Wind Charge Exchange (H-SWCX) and Local Hot Bubble (LHB) (2) Milky Way hot plasma Halo (MWH) (3) Cosmic X-ray Background (CXB) (4) Unresolved High Temperature Plasma (UHTP) (1): the H-SWCX is due to interaction between the Solar wind and neutral atoms in interplanetary space (Cox 1998;Cravens 2000;Koutroumpa et al 2006;Yoshitake et al 2013). The LHB is considered to be the high temperature plasma with the temperature of kT ∼ 0.1 keV (T ∼ 10 6 K) and the density of n H ∼ 0.005 cm −3 embedded in a ∼ 100 pc cavity of the cold interstellar medium in which the Solar System resides (Cox & Anderson 1982;McCammon & Sanders 1990).…”
Section: Spectral Analysis Of the Xdbmentioning
confidence: 99%
“…a typical speed for the slow solar wind is 400 km s −1 ; e.g., Smith et al 2003). Note that the C14 CX data are for ions interacting with H. However, as He is an order of magnitude less abundant than H, and CX cross-sections involving He are typically smaller than those involving H (e.g., Koutroumpa et al 2006, Table 1), neglecting interactions between solar wind ions and He should not adversely affect our results. Note also that, because of the relatively poor spectral resolution of the XMM-Newton detectors at low energies, we did not include lines from N vi or N vii in the C14-SWCX model (these ions' Kα lines lie between those of C vi and O vii).…”
Section: Foreground Model 2: C14-swcxmentioning
confidence: 99%