scholarly journals Stellar flare oscillations: evidence for oscillatory reconnection and evolution of MHD modes

2018 ◽  
Vol 475 (2) ◽  
pp. 2842-2851 ◽  
Author(s):  
J G Doyle ◽  
J Shetye ◽  
A E Antonova ◽  
D Y Kolotkov ◽  
A K Srivastava ◽  
...  
Keyword(s):  
Stellar Flare

Comparison of solar and stellar flare ultraviolet continua

1991 ◽  
Vol 34 ◽  
pp. 277-280
Author(s):  
K.J.H. Phillips ◽  
G.E. Bromage ◽  
J.G. Doyle
Keyword(s):  
Stellar Flare

Magnetic reconnection and energy release in a long-duration stellar flare

1986 ◽  
Vol 6 (8) ◽  
pp. 145-148 ◽  
Author(s):  
G. Poletto ◽  
R. Pallavicini ◽  
R.A. Kopp
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Stellar Flare ◽  
Long Duration

scholarly journals A Bright Spot and a Serendipitous Stellar Flare on the Contact-Binary VW Cep

1983 ◽  
Vol 71 ◽  
pp. 481-483
Author(s):  
K.E. Egge ◽  
B.R. Pettersen
Keyword(s):  
Orbital Period ◽  
Triple System ◽  
Bright Spot ◽  
Stellar Flare ◽  
Flare Event ◽  
Main Contributor ◽  
The Third ◽  
Contact Binary ◽  
Photoelectric Observations ◽  
Large Flare

Almost twenty years ago a large flare event was observed on the prototype contact binary W UMa by Kuhi (1964). Similar events have been reported on 44 i Boo (Eggen 1948) and U Peg (Huruhata 1952) . In this paper we present photoelectric observations at three wavelengths of a flare on VW Cep. This is the first event of this kind to be reported for this star. VW Cep is a triple system. The main contributor to the visual flux is the eclipsing binary, consisting of a Kl primary and a G6 secondary (Kopal 1978), classified to be in contact. The orbital period is 6h 41m. Seven per cent of the total flux in the visual filter is due to the third component, a late K type dwarf at a distance of 12 AU from the eclipsing system (Hershey 1975).

scholarly journals Stellar flare diagnostics from multi–wavelength observations

2009 ◽  
Vol 5 (S264) ◽  
pp. 288-291 ◽  
Author(s):  
Alexander V. Stepanov ◽  
Yuri T. Tsap ◽  
Yulia G. Kopylova
Keyword(s):  
Scaling Law ◽  
Electric Circuit ◽  
Plasma Parameters ◽  
Stellar Flare ◽  
Flare Loop ◽  
X Ray ◽  
Stellar Flares ◽  
Flare Loops ◽  
Red Dwarfs ◽  
Multi Wavelength

AbstractQuasi–periodic pulsations in various wavebands are natural manifestations of emission of stellar flares. We suggest a diagnostic tool of stellar flares based on the coronal seismology and the solar–stellar analogy. Two approaches are used: (I) flare loop as a resonator for MHD oscillations and (II) flare loop as an equivalent electric circuit. Using optical, X–ray, and radio data we obtained flare plasma parameters for the red dwarfs EQ Peg, AT Mic, and AD Leo. The characteristic length of stellar flare loops l ~ R* and their electric currents turned out to be one–two orders of magnitude lager than the solar ones. Advantages of proposed diagnostics in comparison to the scaling law methods are given.

scholarly journals The Extreme-Ultraviolet Continuum of a Strong Stellar Flare

2003 ◽  
Vol 593 (2) ◽  
pp. L105-L108 ◽  
Author(s):  
D. J. Christian ◽  
M. Mathioudakis ◽  
D. Jevremovi ◽  
J. Dupuis ◽  
S. Vennes ◽  
...  
Keyword(s):  
Extreme Ultraviolet ◽  
Ultraviolet Continuum ◽  
Stellar Flare

scholarly journals Flare Stars in Star Clusters and Associations

1975 ◽  
Vol 67 ◽  
pp. 1-14 ◽  
Author(s):  
V. A. Ambartsumian ◽  
L. V. Mirzoyan
Keyword(s):  
Stellar Evolution ◽  
Star Clusters ◽  
Open Clusters ◽  
Point Of View ◽  
Flare Activity ◽  
Theoretical Point ◽  
Star Clusters And Associations ◽  
Stellar Flare ◽  
Dwarf Stars ◽  
Flare Stars

The study of stellar evolution can be undertaken either from a purely theoretical point of view or from a more observational approach. The present standpoint is the second one. It starts from the concepts of stellar evolution in associations and open clusters and from stellar flare activity. Statistical considerations show that flare activity is a regular stage in the evolution of stars through which all the dwarf stars go.

scholarly journals Energy Dissipation Mechanisms in Flare Stars

1985 ◽  
Vol 107 ◽  
pp. 245-262
Author(s):  
D. J. Mullan
Keyword(s):  
Solar Flare ◽  
Solar Flares ◽  
Visible Spectrum ◽  
Stellar Disk ◽  
Total Power ◽  
Quiescent State ◽  
Stellar Flare ◽  
Stellar Spectrum ◽  
Flare Stars ◽  
Visible Disk

Flare stars derive their name from intermittent increases in luminosity which have certain characteristics reminiscent of solar flares (e.g. enhanced strengths of emission lines in the stellar spectrum during the outbursts). When a flare star is observed in a filter which transmits, say, the violet part of the visible spectrum, the increase in luminosity during a flare may range from noise level up to perhaps 100 times the quiescent brightness. During a flare, certain spectral features of the quiescent star (e.g. molecular bands) remain visible, indicating that the flare occupies only a fraction of the visible disk. Thus, analagous to a solar flare, a stellar flare is confined to a single active region. However the total power is large enough to affect the integrated light from the stellar disk. In contrast, the largest solar flare (Etot ≈ 1032 ergs) has a rate of energy release (L ≈ 1029 erg/sec) which is so small that a distant observer would record such a flare as a luminosity increase of less than 10−4Lsun. However, even apart from the flares themselves, it has become apparent in recent years that flare stars in their “quiescent state” provide some extreme contrasts with the sun.

Sign in / Sign up

Export Citation Format

Share Document