Issue |
A&A
Volume 445, Number 2, January II 2006
|
|
---|---|---|
Page(s) | 673 - 680 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20053666 | |
Published online | 16 December 2005 |
A compact flare eclipsed in the corona of SV Camelopardalis
1
Astrophysics Division – Research and Science Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands e-mail: [jsanz;ffavata]@rssd.esa.int
2
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: giusi@astropa.unipa.it
Received:
20
June
2005
Accepted:
30
August
2005
The eclipsing active binary SV Cam (G0V/K6V, d) was observed with XMM-Newton
during two campaigns in 2001 and 2003.
No eclipses in the quiescent emission are clearly identified, but
a flare was eclipsed during the 2001 campaign, allowing us to strongly
constrain, from purely geometrical considerations,
the position and size of the event: the flare is compact
and it is formed at a latitude below 65°. The
size, temperature and Emission Measure of the flare imply an
electron density of
(cm
and a magnetic field of ~65-1400 G in order to confine the
plasma, consistent with the measurements that are obtained
from density-sensitive line ratios in other similar active stars.
Average emission seems to come
from either extended or polar regions because of lack of eclipses.
The Emission Measure
Distribution, coronal abundances and characteristics of
variability are very similar to other active stars such as AB Dor (K1V).
Key words: stars: coronae / stars: abundances / stars: individual: SV Cam / stars: late-type / X-rays: stars / binaries: eclipsing
© ESO, 2005
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