Comparison of Solar X-Ray Line Emission with Microwave Emission during Flares
Abstract
An analysis of X-ray emission at 1.87 A observed during three solar flares by OSO-ITI indicates that maximum line emission is observed to occur 0.5-5 mm after impulsive microwave maximum. The time integral of the centimetric radio burst corresponds best to the 1.87 A line intensity during the rise to maximum X-ray intensity. The constancy of line emission from Fe ix through Fe xv, coupled with strong enhancements in higher ionization stages, suggests that additional material, not originally at coronal temperature, is rapidly heated and elevated to high stages of ionization during the event. Such heating and ionization may be the result of collisional losses by energetic electrons which are also responsible for the impulsive microwave burst
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 1968
- DOI:
- 10.1086/180220
- Bibcode:
- 1968ApJ...153L..59N