Coronal emission from the active binary CC Eri
Abstract
The binary star CC Eri (HD 16157) is an active star with a short orbital period of 1.56 days. It was observed for more than 35 ks with XMM-Newton in September 2003, during which it flared several times and showed a high level of X-ray variability. Preliminary analysis of the thermal structure and elemental abundances of the corona of CC Eri will be presented, along with an investigation into variation in the coronal density and opacity during flares. Simultaneous observations with the Optical Monitor, used to make a comparison between UV and X-ray emission during the flares, will also be presented.
- Publication:
-
35th COSPAR Scientific Assembly
- Pub Date:
- 2004
- Bibcode:
- 2004cosp...35.1742K