Abstract
The X-ray active RS CVn binary system σ Geminorum was observed during a long-duration flare with XMM-Newton. We compare line emission during the flare with line emission measured from a previous Chandra observation during quiescence, in a model independent way. We find that in addition to an overall 25% flux increase, which can be ascribed to variations in the system's quiescence activity over the 15 months that passed between the observations, there is a hot plasma component of kTe > 1 keV that arises with the flare. The hot component is manifested primarily by high charge states of Fe and by a vast continuum, but with no temperature or abundance effect on the cooler (kTe < 1 keV) plasma, except perhaps for Mg that is anomalously enhanced.
| Original language | English |
|---|---|
| Pages (from-to) | 845-848 |
| Number of pages | 4 |
| Journal | European Space Agency, (Special Publication) ESA SP |
| Issue number | 560 II |
| State | Published - 2005 |
| Event | 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Hamburg, Germany Duration: 5 Jul 2004 → 9 Jul 2004 |
Keywords
- Stars: abundances
- Stars: activity
- Stars: corona
- Stars: flares
- Stars: individual: (σ Geminorum)
- X-rays: stars
ASJC Scopus subject areas
- Aerospace Engineering
- Space and Planetary Science