Apache Point Observatory (APO)/SMARTS Flare Star Campaign Observations. I. Blue Wing Asymmetries in Chromospheric Lines during Mid-M-Dwarf Flares from Simultaneous Spectroscopic and Photometric Observation Data [PDF]
The Astrophysical Journal, 2023 We conducted the time-resolved simultaneous optical spectroscopic and photometric observations of mid-M-dwarf flare stars YZ CMi, EV Lac, and AD Leo. Spectroscopic observations were obtained using Apache Point Observatory 3.5 m and Small and Moderate ...
Yuta Notsu +14 more
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Continuum and line emission of flares on red dwarf stars [PDF]
Astrophysics and Space Science, 2015 11 pages, 2 figures; accepted for publication in Astrophysics and Space ...
Morchenko, Egor +2 more
semanticscholar +4 more sources
Double-Peaked Flare Events on red Dwarf Stars and Solar ‘Sympathetic’ Flares [PDF]
Symposium - International Astronomical Union, 1976 About 50% of the flare events observed on red dwarfs are at least double-peaked. As the majority of flare stars are members of double or multiple systems, the possibility that time-overlapping flares originate quasi-simultaneously on the individual components is discussed.Assuming a poissonian occurrence of flares in both components, the expected ...
M. Rodonò
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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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High Time Resolution Photometry of Red Dwarf Flare Stars III. The Most Rapid and Faintest Observed Stellar Flares; their Physics and Statistics [PDF]
International Astronomical Union Colloquium, 1989 AbstractHigh time resolution monitoring of the UV Cet type flare stars has enabled as to detect flares with total duration of a few seconds and with energy output comparable to solar subflares. We find that the time scales of decay for such flares correspond to recombination times of optically thin gas or to cooling times of optically thick gas heated ...
G.M. Beskin +5 more
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PHOTOMETRIC STUDY ON STELLAR MAGNETIC ACTIVITY. I. FLARE VARIABILITY OF RED DWARF STARS IN THE OPEN CLUSTER M37 [PDF]
The Astrophysical Journal, 2015 28 pages, 21 figures, 7 tables, Accepted for publication in ...
S.-W. Chang, Y.-I. Byun, J. D. Hartman
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High Time Resolution Photometry of Red Dwarf Flare Stars I. A Search For Fine Structures on the Optical Light Curves of Flares [PDF]
International Astronomical Union Colloquium, 1989 AbstractA detailed analysis of 73 flares on UV Cet type stars observed at the 6 m telescope of the Special Astrophysical Observatory with 3x10–7 s time resolution shows no fine structures on flare light curves with time scales from 10–6 to 10–1 s.
G.M. Beskin +6 more
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Chromospheric lines in red dwarf flare stars. II - EV Lacertae EQ Pegasi A, and V1054 Ophiuchi
The Astrophysical Journal, 1984 On presente des observations de profils de raies avec une resolution spectrale de 0,45 A pour trois etoiles M4e semblables, du voisinage solaire, avec une luminosite de 1/60 du Soleil: EV Lacertae, EQ Pegari A et V 1054 Oph. On donne des resultats pour Hα (λ6563), les raies Na D(λλ5890, 5896), He I (λ5876) et les raies triplet infra-rouge Ca II (λλ8498,
B. R. Pettersen +2 more
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Narrow-band radio flares from red dwarf stars
The Astrophysical Journal, 1986 VLA observations of narrow-band behavior in 20 cm flares from two red dwarf stars, L726 - 8A and AD Leo, are reported. The flare on L726 - 8A was observed at 1415 and 1515 MHz; the flux and the evolution differed significantly at the two frequencies. The flare on AD Leo lasted for 2 hr at 1415 MHz but did not appear at 1515 MHz.
Stephen M. White +2 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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