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Resolving the origin of the diffuse soft x-ray background
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Sanders, Wilton T. Smith, Randall K. Edgar, Ricard J. Foster, Adam R. Brickhouse, Nancy S. |
| Copyright Year | 2012 |
| Description | In January 1993, the Diffuse X-ray Spectrometer (DXS) measured the first high-resolution spectrum of the diffuse soft X-ray background between 44-80A. A line-dominated spectrum characteristic of a 10(exp 6)K collisionally ionized plasma' was expected but while the observed spectrum was clearly line-dominated, no model would fit. Then in 2003 the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) launched and observed the diffuse extreme-ultraviolet (EUV) spectrum between 90- 265A. Although many emission lines were again expected; only Fe IX at 171.1A was detected. The discovery of X-rays from comets led to the realization that heavy ions (Z=6-28) in the solar wind will emit soft X-rays as the ions interact via charge exchange with neutral atoms in the heliosphere and geocorona. Using a new model for solar wind charge exchange (SWCX) emission, we show that the diffuse soft X-ray background can be understood as a combination of emission from charge exchange onto the slow and fast solar wind together with a more distant and diffuse hot (10(exp 6)K) plasma. |
| File Size | 1695092 |
| Page Count | 6 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_20120016598 |
| Archival Resource Key | ark:/13960/t3hx6bd1v |
| Language | English |
| Publisher Date | 2012-01-01 |
| Access Restriction | Open |
| Subject Keyword | Astronomy Comets High Temperature Plasmas Heavy Ions Charge Exchange Neutral Atoms Diffusivity Heliosphere X Rays Emission Spectra Extreme Ultraviolet Radiation Solar Wind Background Radiation X Ray Spectrometers Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
