Emission Lines
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|+'''Lines in RHESSI Spectra''' | |+'''Lines in RHESSI Spectra''' | ||
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- | + | | valign="top"|[[Image:Chianti rhessi 3to30keV.png|300px|thumb|'''Figure 1''': A synthetic thermal spectra created with Chianti showing the thermal continuum along with line emission. The red curve shows what [[RHESSI]] should observe. ]] | |
- | | valign="top"|[[Image:Chianti rhessi 3to30keV.png|300px|thumb]] | + | | valign="top"| [[Image:Kphillips2008 fig1.png|thumb|300px|'''Figure 2''': Figure 1 from Phillips 2008 which shows the Iron and Iron-Nickel complex identifying each line]] |
- | | valign="top"| [[Image:Kphillips2008 fig1.png|thumb|300px|Figure 1 from Phillips 2008]] | + | |- |
- | | valign="top"|[[Image:Chianti rhessi 6to7keV.png|300px|thumb]] | + | | valign="top"|[[Image:Chianti rhessi 6to7keV.png|300px|thumb| '''Figure 3''': A close up of the Iron complex.]] |
- | | valign="top"|[[Image:Chianti rhessi 7to10keV.png|300px|thumb]] | + | | valign="top"|[[Image:Chianti rhessi 7to10keV.png|300px|thumb| '''Figure 4''': A close up of the Iron-Nickel complex along with some higher energy Iron lines. Due to small flux in the higher energy lines, [[RHESSI]] is only likely to observe the Iron-Nickel complex as can be seen from the (red) [[RHESSI]] overlay.]] |
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+ | == References == | ||
+ | * [http://adsabs.harvard.edu/abs/2008A%26A...490..823P Highly ionized Fe X-ray lines at energies 7.7-8.6 keV] by K. Phillips | ||
+ | * [[The SphinX Instrument on CORONAS-PHOTON]] | ||
+ | * [[Vth abun - Variable Thermal, Separate Abundances]] | ||
+ | * [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=84 Flare Plasma Abundances - New X-ray Observations] | ||
+ | * [[The Fe and Fe/Ni line features I]] | ||
+ | * [[The Fe and Fe/Ni line features II]] |
Latest revision as of 01:46, 23 January 2010
RHESSI observes X-rays down to 3 keV which includes a number of emission lines. They consist mostly of highly ionized Fe lines. There are no lines above about 10 keV.