Topic
Orion variable
About: Orion variable is a research topic. Over the lifetime, 4 publications have been published within this topic receiving 8 citations.
Papers
TL;DR: In this paper, photographic, photoelectric, and spectral observations of the flare star PP Ori were performed over a period of about 20 years, and four spectra obtained on the same telescope with a 4° objective prism showed no variation in brightness.
Abstract: We give the results of photographic, photoelectric, and spectral observations of the flare star PP Ori. The 109 photographic observations used, which were obtained on the 40″ Schmidt telescope of the Byurakan Observatory over a period of about 20 years, and four spectra obtained on the same telescope with a4° objective prism show no variation in brightness. Photoelectric observations in the UBVR bands using the 50cm and 60cm telescopes of the high-altitude Maidanak station of the Tashkent Astronomical Institute in 1987 and 1989 give grounds for suspecting a variation in brightness much larger than observational errors. Spectral observations of the star PP Ori made on the 2.6m telescope of the Byurakan Observatory show weak Hα emission. The results of all these observations show that PP Ori is an Orion variable of spectral class K7-M0 with absolute visual magnitude7 ⋅ m 5–8 ⋅ m 5.
3 citations
1 Jan 1969
TL;DR: The first results of a photometric study of the Orion flare stars were presented in this paper using material from the Boyden Observatory, where a 60-inch photoelectric sequence, in U, B, V and R, and a photographic reduction technique developed for ADH Baker-Schmidt plates by C. J. Butler, were utilized to construct colour-magnitude and colour-colour diagrams for flare stars to V = 16m.
Abstract: The first results of a photometric study of the Orion flare stars is presented using material from the Boyden Observatory. A 60-inch photoelectric sequence, in U, B, V and R, and a photographic reduction technique developed for ADH Baker-Schmidt plates by C. J. Butler, are utilized to construct colour-magnitude and colour-colour diagrams for flare stars to V = 16m. The scattre of the flare stars about the main sequence, pointed out by Haro, is confirmed in the B-V/V diagram. However, a fairly well-defined band in the V-R/V diagram is evident, extending from V-R = 1.m0, V = 12.m5 to V-R = 1.m7, V = 16.m0. The classical flare stars appear to fall within the same region of the B-V/V-R diagram but to the red of the majority of Orion flare stars.
1 citations
TL;DR: In this paper, the results of searches for multiple systems among Orion variable stars in the region of the Orion association are given; 22 multiple systems consisting of T Tau stars and nine of flare stars have been found.
Abstract: The results of searches for multiple systems among Orion variable stars in the region of the Orion association are given; 22 multiple systems consisting of T Tau stars and nine of flare stars have been found. It is established that among the discovered multiple stars the majority (20 and seven, respectively) have Trapezium type configurations. It is shown that multiple systems of Trapezium type are encountered more often among stars of T Tau type than among flare stars and that the average dimensions of the systems consisting of flare stars are greater than for the T Tau systems. It is shown that among the multiple stars of Trapezium type consisting of T Tau or flare stars there may be some with positive total energy.
TL;DR: In this article, the results of observations of fuorlike outbursts of the objects Sugano and Chanal in the Orion association are given, and light curves have been constructed, and the outburst amplitudes and color indices have been determined.
Abstract: The results are given of observations of fuorlike outbursts of the objects Sugano and Chanal in the Orion association. Light curves have been constructed, and the outburst amplitudes and color indices have been determined. It was shown that the object Sugano exhibits the behavior of both an Orion variable and a flare star. Estimates of /delta//prime/ and /delta/ show that they are of the same order as in the case of furors. It is conjectured that although outflow is observed in the case of many nonstationary stars there is in the considered case an intensification of the outflow, possibly at the same velocities, of the matter that forms the envelope. The luminosity of P Cyg before its outburst is determined.
Related Topics (5)
Performance Metrics
| Year | Papers |
|---|---|
| 1995 | 1 |
| 1988 | 2 |
| 1969 | 1 |