Solar wind charge exchange and local hot bubble X-ray emission with the DXL sounding rocket experiment
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Solar wind charge exchange and local hot bubble X-ray emission with the DXL sounding rocket experiment
The Diffuse X-ray emission from the Local Galaxy (DXL) sounding rocket is a NASA approved mission with a scheduled first launch in December 2012. Its goal is to identify and separate the X-ray emission of the solar wind charge exchange (SWCX) from that of the local hot bubble (LHB) to improve our understanding of both. To separate the SWCX contribution from the LHB, DXL will use the SWCX signat...
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The hot Local Bubble surrounding the solar neighborhood has been primarily studied through observations of its soft X-ray emission. The measurements were obtained by attributing all of the observed local soft X-rays to the bubble. However, mounting evidence shows that the heliosphere also produces diffuse X-rays. The source is solar wind ions that have received an electron from another atom. Th...
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We report an apparent detection of the CVI 4p to 1s transition line at 459 eV, during a long-term enhancement (LTE) in the Suzaku north ecliptic pole (NEP) observation of 2005 September 2. The observed intensity of the line is comparable to that of the CVI 2p to 1s line at 367 eV. This is strong evidence for the charge-exchange process. In addition to the CVI lines, emission lines from OVII, OV...
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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 (∼2×106 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 iden...
متن کاملXMM-Newton Observation of Solar Wind Charge Exchange Emission
We present an XMM-Newton spectrum of diffuse X-ray emission from within the solar system. The spectrum is dominated by probable C VI lines at 0.37 keV and 0.46 keV, an O VII line at 0.56 keV, O VIII lines at 0.65 keV and ∼ 0.8 keV, Ne IX lines at ∼ 0.92 keV, and Mg XI lines at ∼ 1.35 keV. This spectrum is consistent with that expected from charge exchange emission between the highly ionized sol...
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ژورنال
عنوان ژورنال: Astronomische Nachrichten
سال: 2012
ISSN: 0004-6337
DOI: 10.1002/asna.201211665