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BD+47°819, an A-type Flare Star with Peculiar Spectroscopic Variation

Published online by Cambridge University Press:  12 April 2016

Jun-Jie Wang*
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China

Extract

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Stellar flares are one of the most challenging problems in astrophysics. Up to now, most of the detected flare stars are of late spectral type (e.g. UV Cet type stars etc.). Non-classical flare stars with early spectral type are very rare.

Recently, an A5-type flare star BD+47°819, near the open cluster α Persei, was discovered (Wang 1993). The flare U amplitude was 1m.5 in ten minutes. The V magnitude of the star was 9m.25 during the quiescent state.

On 1993 February 28 and March 1, spectroscopic observations of BD+47°819 were madewithn the 2.16 m telescope of Beijing Astronomical Observatory. A grating with a dispersion of 5nm/mm was used. Figs. 1 (a) and (b) show the observed spectra in the two nights. The exposure time for each spectrum was 15 minutes. Fig. 1 (a) shows a strange feature, an “emission line” at around 676 nm. Is this a real feature?

Type
Flares in Late-type Stars: Radio and Optical
Copyright
Copyright © Springer-Verlag 1995

References

Wang, J.-J., 1993, IBVS 3836Google Scholar