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Pulsations in the eclipsing variable system AS Camelopardalis
We performed photoelectric observations of AS Cam in 2002 2004. Five newtimes of minima were obtained. Their positions are consistent with thepreviously found light equation for the system and with the hypothesisthat the difference between the observed (15°/100 yr) andtheoretical (44°/100 yr) rates of apsidal motion results from thepresence of a third body in the system. A Fourier analysis of twoobservational data sets, 1968 1970 and 2002 2004, reveals, with a highsignificance, periodic light variations with a frequency of ω 0 =1.0950 ± 0.0001d-1 and an amplitude of 0 . m 020, which areprobably caused by the radial pulsations of one of the components. Wefound a seasonal phase shift of these oscillations that may be producedby other periodic processes in the system. We show that the fairly largescatter of observed times of minima about the theoretical curve of thelight equation can be explained by the presence of pulsations. Using the2002 and 2004 observations as an example, we show that including thepulsations reduces this scatter.
| New Times of Minima of Eclipsing Binary Systems
We present several photoelectric minima observations of 15 eclipsingbinaries.
| Apsidal motion in the eclipsing binary AS Camelopardalis.
We report several new reliable times of minimum of the eclipsing binaryAS Cam. Using all precise timings found in the literature, the O-Cdiagram is analyzed and improved values for the elements of the apsidalmotion are computed. The discrepancy between observed rotationalvelocity of the line of apsides and the theoretically expected valuestill remains unresolved.
| Apsidal Motion of AS Camelopardalis
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| Takýmyýldýz: | Zurafa |
| Sað Açýklýk: | 05h28m45.66s |
| Yükselim: | +69°20'11.1" |
| Görünürdeki Parlaklýk: | 8.29 |
| Uzaklýk: | 290.698 parsek |
| özdevim Sað Açýklýk: | 11.3 |
| özdevim Yükselim: | -26 |
| B-T magnitude: | 10.309 |
| V-T magnitude: | 8.457 |
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