The light and period changes of RT Andromedae
The light and period changes of RT Andromedae
复制标题
DOI:
10.1051/0004-6361:20011357
复制
发表时间:
2001-12
影响因子:
6.5
通讯作者:
A. Erdem;O. Demircan;M. Güre
中科院分区:
文献类型:
--
作者:
A. Erdem;O. Demircan;M. Güre
The nature of the long-term orbital period variation and the light level variation of RT And was studied based on all available photometric observations. The (O{C) diagram formed by all available times of eclipse minima could be either of a quasi-sinusoidal form superimposed on a parabolic form, or a long period sinusoidal form. The quasi-sinusoidal form with an amplitude of 0.002 days and a period of 65 years could be due to a cyclic magnetic activity modulation on the orbital period of the system. Applegate's theory (Applegate 1992), in this case, predicts an3 kG mean subsurface magnetic eld for the primary component of the system. The parabolic form corresponds to a secular period decrease of about 3 10 9 m yr 1 caused by mass loss from the system, and the long-period sinusoidal form with an amplitude of 0.02 days and a period of 105 years corresponds to a secular period change caused by the light-time eect due to an unseen third star in the system. It was estimated that the unseen third star should be a low mass (lower than 0:6 m) and faint (5: m fainter than the system RT And) star, whose detection is almost impossible. Future data will add information on the nature of the secular (O{C) variation. Secular light level variation of the system was found to be irregular and no correlation was detected with the orbital period variation.