Emission Lines: Difference between revisions
Jump to navigation
Jump to search
imported>Schriste No edit summary |
imported>Schriste No edit summary |
||
| Line 1: | Line 1: | ||
[[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.
