Birth of a slowly evolving flare.
Abstract
A gradual rise and decline flare with a duration of about one hour was observed on June 10, 1980 in the radio (Toyokawa and VLA) optical (Big Bear) and XUV (SMM satellite) ranges of wavelengths. The flare developed as a large loop connecting two regions of opposite polarity in a pre-existing active region. A model of the differential emission measure of the loop observed at the beginning of the flare is deduced from the analysis of the XUV images in C IV (1549 Å), O VIII (18.97 Å), Ne IX (13.45 Å), Mg XI (9.17 Å) and Si XIII (6.65 Å) emission lines. The differential emission measure as a function of temperature is controlled by the conductive flux via the temperature gradient.
- Publication:
-
Modeling the Stellar Environment: How and Why?
- Pub Date:
- 1989
- Bibcode:
- 1989mse..proc..215C
- Keywords:
-
- Coronal Loops;
- Emission Spectra;
- Solar Flares;
- Solar Maximum Mission;
- Solar Temperature;
- Temporal Distribution;
- Very Large Array (Vla);
- Solar Physics;
- Solar Flares: UV Spectra;
- Solar Flares: Light Curves