Detection of the unusually blue of flare star HD 269665

1990 ◽  
Vol 167 (1) ◽  
pp. 167-169
Author(s):  
H. M. Tovmassian ◽  
R. Kh. Hovhanessian ◽  
R. A. Efremian ◽  
Yu. M. Khodjayants ◽  
M. N. Krmoyan ◽  
...  
Keyword(s):  
Flare Star

Spectral Observations of the Flare Star HU Del

Astrophysics ◽  
2005 ◽  
Vol 48 (3) ◽  
pp. 279-290
Author(s):  
V. S. Tamazian ◽  
N. D. Melikian ◽  
A. A. Karapetian ◽  
R. Sh. Natsvlishvili
Keyword(s):  
Flare Star

Gliese 825 – a new flare star

1981 ◽  
Vol 195 (2) ◽  
pp. 143-147 ◽  
Author(s):  
Patrick B. Byrne
Keyword(s):  
Flare Star

scholarly journals The Radio Properties of the dMe Flare Star Proxima Centauri

1996 ◽  
Vol 460 ◽  
pp. 976 ◽  
Author(s):  
Jeremy Lim ◽  
Stephen M. White ◽  
O. B. Slee
Keyword(s):  
Flare Star

The Atmosphere of a Probably Very Young by Dra-Type Flare Star

1983 ◽  
pp. 77-77
Author(s):  
R. de la Reza ◽  
C. J. Butler ◽  
C. A. O. Torres ◽  
C. C. Batalha
Keyword(s):  
Flare Star

scholarly journals Photoelectric Observations of AD Leo: 1989-1994

1995 ◽  
Vol 151 ◽  
pp. 87-88
Author(s):  
R. Konstantinova-Antova ◽  
A.P. Antov
Keyword(s):  
Single Channel ◽  
Photon Counting ◽  
Astronomical Observatory ◽  
Program Package ◽  
Flare Star ◽  
The Other ◽  
Integration Time ◽  
Differential Photometry ◽  
Computer Controlled ◽  
Photoelectric Observations

An investigation of the activity of the flare star AD Leo was made using U-band patrol observations. 60 cm computer-controlled telescopes with identical single channel photon-counting photometers at the National Astronomical Observatory at Rozhen and at the Belogradchik Observatory were used. The integration time was 1 sec. Differential photometry was carried out, the AD Leo measurements were made relative to BD+20°2475. The data was reduced with the program package APR (Kirov et al. 1991).Two simultaneous observing runs were made. The results of the first have already been published (Antov etal. 1991). The other was part of the observational campaign in May, 1991 with the ROSAT satellite. In Bulgaria, the observations were carried out at Rozhen in the U-band and at Belogradchik in the B-band. Four flares were detected by both.

scholarly journals High-Speed Photometry of Cluster Flare Stars

1975 ◽  
Vol 67 ◽  
pp. 69-73
Author(s):  
M. Rodonò
Keyword(s):  
High Speed ◽  
Activity Level ◽  
Flare Star ◽  
Solar Neighbourhood ◽  
High Occurrence ◽  
High Speed Photometry ◽  
Flare Stars ◽  
Photoelectric Observations ◽  
Absolute Luminosity

Recent photoelectric observations made at Catania Observatory show a high occurrence of short-lived faint flares on the Hyades member II Tau (H II 2411). Its activity level turns out to be higher than for UV Cet-type stars of equal absolute luminosity.II Tau could represent a transition prototype between UV Cet-type flare star in the solar neighbourhood and cluster ones.The importance of coordinated photoelectric patrol of properly selected flare stars in clusters of different age is emphasized.

scholarly journals Mass and Luminosity Function of the Pleiades

1980 ◽  
Vol 85 ◽  
pp. 157-163 ◽  
Author(s):  
Floor van Leeuwen
Keyword(s):  
Proper Motion ◽  
Total Mass ◽  
Luminosity Function ◽  
Mass Range ◽  
Flare Star ◽  
Central Field ◽  
Photometric Measurement ◽  
Proper Motions ◽  
Total Field ◽  
Factor 20

From a proper motion survey by Pels and photometric measurement of selected stars it was found that the Pleiades cluster extends till at least 496 from the centre, corresponding to 10 pc at a distance of 125 pc. It turns out that the luminosity function of the Pleiades is a function of the distance to the centre, the proportion of faint stars increasing with this distance. Because of this, the luminosity function as it was determined before flattened towards fainter stars, whereas for the total field with a diameter of 20 pc one finds a luminosity function that is still increasing at the faint end. Flare star observations in the Pleiades field show that the increase amounts to at least a factor 20 in the mass range 2 to 0.4 M⊙. Accurate proper motions of stars in the projected central field show a dispersion of velocities in the cluster of 700 m/sec. This could indicate a total mass of the Pleiades cluster of the order of 2000 M⊙.

scholarly journals IUE Spectra of The by Dra/Flare Star AU Mic

1983 ◽  
Vol 71 ◽  
pp. 249-250
Author(s):  
C.J. Butler ◽  
A.D. Andrews ◽  
J.G. Doyle ◽  
P.B. Byrne ◽  
J.L. Linsky ◽  
...  
Keyword(s):  
Light Curve ◽  
Emission Line ◽  
Flare Star ◽  
Emission Lines ◽  
Spectral Variation ◽  
Strong Emission ◽  
Line Intensities ◽  
The Mean ◽  
Phase Interval

A coordinated series of ground-based optical and IUE observations of BY Dra variables was undertaken to follow the spectral variation of these stars over one cycle. In the first series 20 LWR and 19 SWP trailed spectra were taken of AU Mic over a three day period 4-6 August 1980 .In Figure 1 we show the mean integrated fluxes for the strong emission lines in the SWP spectra of AU Mic over the observed phase interval of 0.14 to 0.8 together with an approximate V light curve determined by the FES on IUE. From comparison of the emission line intensities and FES magnitudes in Figure 1 several points emerge.

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