Emission Lines: Difference between revisions
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imported>Schriste m (added reference) |
imported>Schriste m (added some references) |
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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 == | == 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 | * [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] | |||
* [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=13 The Fe and Fe/Ni line features I] | |||
* [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=15 The Fe and Fe/Ni line features II] | |||
Revision as of 20:46, 22 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.
 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. |
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