Flares of Red Dwarf Stars and Solar Activity [PDF]
Symposium - International Astronomical Union, 1975 The UV Cet-type star flares and the chromospheric flares of the Sun have many important common features. Both types of events are very transient; they occupy only small parts of the stellar surfaces; in both cases the optical as well as the radio emissions of the flares have strong similarities in temporal and spectral characteristics.
R. E. Gersheberg, N. I. Shakhovskaya
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Chromospheric lines in red dwarf flare stars. I - AD Leonis and GX Andromedae
Astrophysical Journal, 1981 B R Pettersen
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Are their flaring specialities associated with their being giant stars? [PDF]
, 2021 Aims. We aim to give a reliable estimate of the number of flaring giant stars in the Kepler field. By analyzing the flaring activity of these stars, we explored their flare statistics and the released flare energies.
Gaulme, P. +19 more
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A confined dynamo: Magnetic activity of the K-dwarf component in the pre-cataclysmic binary system V471 Tauri [PDF]
, 2021 Context. Late-type stars in close binary systems can exhibit strong magnetic activity owing to rapid rotation supported by tidal locking. On the other hand, tidal coupling may suppress the differential rotation which is a key ingredient of the magnetic ...
Seli, Bálint Attila +16 more
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Continuum and line emission of flares on red dwarf stars [PDF]
Astrophysics and Space Science, 2015 The emission spectrum has been calculated of a homogeneous pure hydrogen layer, which parameters are typical for a flare on a red dwarf. The ionization and excitation states were determined by the solution of steady-state equations taking into account the continuum and all discrete hydrogen levels.
Morchenko, Egor +2 more
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AASLD practice guidance on drug, herbal, and dietary supplement–induced liver injury
, 2022 Hepatology, EarlyView.
Robert J. Fontana +6 more
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Flares on Red Dwarf Stars as a Result of the Dynamical Response of the Chromosphere to the Heating [PDF]
International Astronomical Union Colloquium, 1983 The impulsive hard X-ray, EUV and microwave radio bursts always start at or after the onset of a soft X-ray increase - the main phase of a solar flare - before the Hα flare maximum. This hard phase of a solar flare lasts ~ 100 s and consists of several elementary bursts of 10 s duration.
M.M. Katsova, M.A. Livshits
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A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
The Astrophysical Journal, 2023 M-dwarfs are common stellar hosts of habitable-zone exoplanets. Near-UV (NUV) radiation can severely impact the atmospheric and surface conditions of such planets, making the characterization of NUV flaring activity a key aspect in determining ...
Param Rekhi +3 more
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The Astrophysical Journal, 2023 We present light curves and flares from a 7 day, multiwavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data.
Isaiah I. Tristan +15 more
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High Time Resolution Photometry of Red Dwarf Flare Stars II. The Shortest Flare Rise Time [PDF]
International Astronomical Union Colloquium, 1989 AbstractWe have studied the initial phases of 65 optical flares on UV Cet type stars with a time resolution of 3x10–7 s. Ninety per cent of these flares have rapid brightenings shorter than 10 s and several are shorter than 1 s. We detected on UV Cet the shortest flare observed to date with a total duration of 1.7 s and a rise time of 0.3 s.
G.M. Beskin +4 more
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