We present preliminary results from the analysis of a long duration flare that was observed in a serendipitous XMM-Newton detection of the M star CD-39 7717 B (TWA 11 B), member of the young stellar association TW Hya. Only the rise phase (with a duration of ~35 ks) and possibly the flare peak are present in the light-curve. The decay phase was not monitored. The fluorescent iron emission line at 6.4 keV was observed during this event. As far as we are concerned, since TWA 11 B seems to have no disk, this is only the third detection of Fe photospheric fluorescence. During the flare, the X-ray flux increased a factor of ~4. Taking the light curve and the evolution of the hardness ratio into account, we interpret the rise phase as resulting from the ignition of a first group of loops (part 1) which triggered a subsequent two-ribbon flare (part 2). Part 1 is analysed using the Reale's (2007) model, since it has been assumed to be dominated by a single loop. For part 2, the diagnostic method for two-ribbon flares developed by Kopp & Poletto (1984) is applied. Loop semi-lengths of about 2.5-3.0 stellar radii are obtained. These large structures were previously detected only in very young objects, this is the first time that are detected in a more evolved (~8 Myr) star.

CrespoChacón, I., LópezSantiago, J., Reale, F., Micela, G. (2009). Modeling the long duration rise phase of a flare detected on the M star TWA 11 B. In AIP Conference Proceedings (pp.584-587) [10.1063/1.3099180].

Modeling the long duration rise phase of a flare detected on the M star TWA 11 B

REALE, Fabio;
2009-01-01

Abstract

We present preliminary results from the analysis of a long duration flare that was observed in a serendipitous XMM-Newton detection of the M star CD-39 7717 B (TWA 11 B), member of the young stellar association TW Hya. Only the rise phase (with a duration of ~35 ks) and possibly the flare peak are present in the light-curve. The decay phase was not monitored. The fluorescent iron emission line at 6.4 keV was observed during this event. As far as we are concerned, since TWA 11 B seems to have no disk, this is only the third detection of Fe photospheric fluorescence. During the flare, the X-ray flux increased a factor of ~4. Taking the light curve and the evolution of the hardness ratio into account, we interpret the rise phase as resulting from the ignition of a first group of loops (part 1) which triggered a subsequent two-ribbon flare (part 2). Part 1 is analysed using the Reale's (2007) model, since it has been assumed to be dominated by a single loop. For part 2, the diagnostic method for two-ribbon flares developed by Kopp & Poletto (1984) is applied. Loop semi-lengths of about 2.5-3.0 stellar radii are obtained. These large structures were previously detected only in very young objects, this is the first time that are detected in a more evolved (~8 Myr) star.
2008
COOL STARS, STELLAR SYSTEMS AND THE SUN
St Andrews, Scotland
July 21-25 2008
15
2009
4
CrespoChacón, I., LópezSantiago, J., Reale, F., Micela, G. (2009). Modeling the long duration rise phase of a flare detected on the M star TWA 11 B. In AIP Conference Proceedings (pp.584-587) [10.1063/1.3099180].
Proceedings (atti dei congressi)
CrespoChacón, I; LópezSantiago, J; Reale, F; Micela, G
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10447/46237
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