Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...453..464h&link_type=abstract
Astrophysical Journal v.453, p.464
Astronomy and Astrophysics
Astronomy
85
Stars: Chromospheres, Stars: Flare, Stars: Individual Constellation Name: Ad Leonis, Ultraviolet: Stars
Scientific paper
We report on the first simultaneous Extreme-Ultraviolet Explorer (EUVE) and optical observations of flares on the dMe flare star AD Leonis. The data show the following features:
1. Two flares (one large and one of moderate size) of several hours duration were observed in the EUV wavelength range;
2. Flare emission observed in the optical precedes the emission seen with EUVE;
3. Several diminutions (DIMs) in the optical continuum were observed during the period of optical flare activity.
To interpret these data, we develop a technique for deriving the coronal loop length from the observed rise and decay behavior of the EUV flare. The technique is generally applicable to existing and future coronal observations of stellar flares. We also determine the pressure, column depth, emission measure, loop cross- sectional area, and peak thermal energy during the two EUV flares, and the temperature, area coverage, and energy of the optical continuum emission.
When the optical and coronal data are combined, we find convincing evidence of a stellar "Neupert effect" which is a strong signature of chromospheric evaporation models. We then argue that the known spatial correlation of white-light emission with hard X-ray emission in solar flares, and the identification of the hard X-ray emission with nonthermal bremsstrahlung produced by accelerated electrons, provides evidence that flare heating on dMe stars is produced by the same electron precipitation mechanism that is inferred to occur on the Sun.
We provide a thorough picture of the physical processes that are operative during the largest EUV flare, compare and contrast this picture with the canonical solar flare model, and conclude that the coronal loop length may be the most important factor in determining the flare rise time and energetics.
Cully Scott L.
Deustua Susana E.
Fisher George H.
Hawley Suzanne L.
Jablonski Marek
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