A plausible third body in RS CVn-type binary: RT Coronae Borealis

作者：Zhang W X^*; Ran M W; Feng Y G

来源：Astrophysics and Space Science, 2014, 354(2): 409-413.

DOI：10.1007/s10509-014-2048-y

• Binaries: eclipsing
• Stars: spots
• Stars: mass-loss
• Stars: individual (RT CrB)

Cyclic period changes, which are usually explained as being caused by the magnetic activity of one or both components or the light travel time effect of a third body, are a typical phenomenon in the RS CVn-type binary. Combining the newly determined eclipsing times with others compiled from literature, we analyzed the cyclic period change in the RS CVn-type binary RT CrB. The result shows that the orbital period of the binary shows a period of 3.47 yr with an amplitude of 0 (d) .0084. The cyclic oscillation can be attributed to the existence of a third body with a lower limit mass of 1.71(+/- 0.19) M (aS (TM)). The third body is cycling the binary at a distance of no more than 2.30(+/- 0.19) AU which would play an important role in the evolution of this system. No detected spectral lines of the third body may suggest that the third component may itself be a close binary of 0.86 M (aS (TM)) stars, or more likely a dark star such as a neutron star.

• 出版日期2014-12
• 单位铜仁学院