Emission Lines
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* [[Vth abun - Variable Thermal, Separate Abundances]] | * [[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=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.