Volume 426, Number 3, November II 2004
|Page(s)||1035 - 1045|
|Published online||18 October 2004|
X-ray spectroscopy of the W UMa-type binary 44 Bootis
European Space Agency, ESTEC – Postbus 299, 2200 AG Noordwijk, The Netherlands e-mail: firstname.lastname@example.org
Accepted: 1 July 2004
44 Boo B, a W UMa-type binary system, was observed in June 2001 during one entire revolution period with the observatory. The count rate in the 0.3 to 2 keV band is constant in average with 5 to 20% count rate increases reminiscent of flares. Spectral fitting of the EPIC spectra indicates a corona configuration with little contribution from quiet regions, similar to the Sun. On the contrary, the (2–9) 106 K temperature range of the “cool” plasma suggests that the active corona around the two companions is densely filled with low-lying loops similar to those found in solar-type active regions. The 44 Boo O VII He-like triplet constrains the electron density to an upper limit ne < 8.6 1010 cm-3. We argue that this low-lying loop system may be overlaid by larger loops. Magnetic reconnection phenomena in this large loops system may explain the characteristic flare decay time in the light curve that implies loop lengths of about 16 109 cm. An extended corona around 44 Boo would explain the absence of eclipses in its X-ray light curve. The average element abundance in 44 Boo corona is found to be lower than the solar photospheric value. The spectral analysis indicates enhanced abundances of oxygen and neon relative to iron which suggest an inverse FIP effect. Compared with other active binary systems such as RSCVn or BY Dra, 44 Boo has relatively less material at temperatures higher than 107 K and the temperature of its hottest plasma component appears to be lower.
Key words: stars: individual: 44 Bootis / stars: activity / stars: coronae / stars: late-type / X-rays: stars / stars: binaries: general
© ESO, 2004
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