Emission Lines
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| - | [[RHESSI]] observes X-rays down to 3 keV which includes a number of emission lines. | + | [[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. |
| - | + | {| border="0" | |
| - | [[Image: | + | |+'''Lines in RHESSI Spectra''' |
| - | [[Image: | + | |- |
| - | [[Image:Chianti rhessi 6to7keV.png]] | + | | valign="top"| |
| - | [[Image:Chianti rhessi 7to10keV.png]] | + | | valign="top"|[[Image:Chianti rhessi 3to30keV.png|300px|thumb]] |
| + | | 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 7to10keV.png|300px|thumb]] | ||
| + | |} | ||
Revision as of 23:06, 19 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.
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