Issue |
A&A
Volume 458, Number 3, November II 2006
|
|
---|---|---|
Page(s) | 921 - 930 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20065304 | |
Published online | 12 September 2006 |
GALEX high time-resolution ultraviolet observations of dMe flare events
1
Experimental Astrophysics Group, Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720, USA e-mail: bwelsh@ssl.berkeley.edu
2
Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland
3
California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA
4
Solar Physics and Upper-Atmosphere Research Group, Department of Applied Mathematics, University of Sheffield, Sheffield, S3 7RH, USA
Received:
29
March
2006
Accepted:
10
August
2006
Aims.We present near ultraviolet (NUV: 1750–2800 Å) and far ultraviolet
(FUV: 1350–1750 Å) light-curves for flares on 4 nearby dMe-type stars (GJ
3685A, CR Dra, AF Psc and SDSS J084425.9+513830.5) observed with the satellite.
Methods.Taking advantage of the time-tagged events recorded with the
photon counting detectors, we present high temporal resolution (<0.01 s)
analysis of these UV flare data.
Results.A statistical analysis of 700 s of pre-flare quiescence data for both
CR Dra and SDSS J084425.9+513830.5 failed to reveal the presence of
significant micro-flare activity in time bins of 0.2, 1 and 10 s
intervals. Using an appropriate differential emission measure for both the
quiescent and flaring state, it is possible to reproduce the observed FUV:NUV
flux ratios. A major determinant in reproducing this flux ratio is found to be
the value of plasma electron density during the flare. We also searched
the count rate data recorded during each of the four flare events for
periodicity associated with magneto-hydrodynamic oscillations in the active
region coronal loops. Significant oscillations were detected during the
flare events observed on all 4 stars, with
periodicities found in the 30 to 40 s range. Flare oscillations with this
periodicity can be explained as acoustic waves in a
coronal loop of length of cm for an assumed plasma
temperature of
K. This suggests a loop length for these
M-dwarf flares of less than
of the stellar radii. We believe that
this is the first detection of non-solar coronal loop flare oscillations
observed at ultraviolet wavelengths.
Key words: ultraviolet: stars / stars: flare / stars: activity / stars: chromospheres / stars: coronae
© ESO, 2006
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