Stars with solar-type activity: GTSh10 catalogue

Гершберг, Р. Е.; Terebizh, A. V.; Shlyapnikov, A. A.

doi:10.3103/s0190271711010062

Cited by 4 publications

(2 citation statements)

References 33 publications

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“…Consequently, there are published many papers on that subject and thousands of red dwarfs were investigated up to now. For few objects the phenomena of flare light variations were observed in the full range of wavelengths [9][10][11]. Our understanding of the nature of such light variations of red dwarfs was extended by the analogy to similar events observed on the Sun.…”

Section: Introductionmentioning

confidence: 98%

Spectral Energy Distribution of Flares in the Variable Star AO Serpentis

Esaenwi

2024

OAJA

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Here we report on the flaring variable star AO Ser which was observed with the 0.4m SBIG optical telescope from Las Cumbres Obervatory Global Telescope Network remotely on 25/09/2022. The Spectrometric analysis was carried out with the SIMBAD Digital Sky Survey (DSS) menu from the VizieR GUI on the Aladin Software to obtain flux density, flare energy, flare wavelength and flare frequency. The light curve of AO Ser shows that the source has a strong presence of flares. Hence, we estimated the flare energy, flare wavelength and flare frequency of AO Ser at peak flares so as to deduce its spectral energy distribution. From the spectral energy distribution, the Aladin software automatically estimated the Flare Energy of AO Ser at(as) 1.09 2 e eV − , the Flare flux density of AO Ser F (ν ) at 3.27 1 e Jy + and Flare Flux Energy of AO Ser F (λ ) at 7.55 12 1 2 1 e erg cm m − −− − µ . We conclude that AO Ser is an eclipsing binary variable flaring stars that is losing mass in form of heat.

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Section: Introductionmentioning

confidence: 98%

Spectral Energy Distribution of Flares in the Variable Star AO Serpentis

Esaenwi

2024

OAJA

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“…Consequently, there are published many papers on that subject and thousands of red dwarfs were investigated up to now. For few objects the phenomena of flare light variations were observed in the full range of wavelengths, see Gershberg et al (1999Gershberg et al ( , 2011 and Katsova et al (1999).…”

Section: Introductionmentioning

confidence: 99%

On global and local magnetic fields of flare stars with YZ CMi and OT Ser as examples

et al. 2017

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Global magnetic fields of flare stars can evolve rapidly, in time scale of hundreds or dozens of days. We believe, that such changes result from rapid superposition of local magnetic fields generated by differential rotation of those stars. We discuss possible mechanisms of generation and dissipation of local and global magnetic fields in sample flare stars OT Ser and YZ CMi. Mechanism of magnetic braking of these stars is proposed here, in which differential rotation generates local magnetic fields, and eventually energy accumulated in local fields is radiated away by flares. We obtained estimates of the rotational energy and the energy of the global magnetic field of OT Ser and YZ CMi. It is shown that the energy of the local magnetic fields dissipated during superflare of YZ CMi on 9 February 2008 (UT 20:22:00) did not influence the global magnetic field of this star.

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Superflares on Red Dwarf EXO 040830-7134.7

Gorbachev

Shlyapnikov

2022

Geomagn. Aeron.

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Stars with solar-type activity: GTSh10 catalogue

Cited by 4 publications

References 33 publications

Spectral Energy Distribution of Flares in the Variable Star AO Serpentis

Spectral Energy Distribution of Flares in the Variable Star AO Serpentis

On global and local magnetic fields of flare stars with YZ CMi and OT Ser as examples

Superflares on Red Dwarf EXO 040830-7134.7

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