“Constant” eclipsing binary in the instability strip

•Taking into account the results, I discuss the nature of OO Peg.•Analyses of the light and radial curves led to determination of stellar parameters.•I show the location of the components in effective temperature–luminosity diagram.•About six single stars and OO Peg components do not show any pulsational frequencies.•They are apparently constant stars lie within the pulsation instability region.

The eclipsing binary OO Peg consist of two late-A type stars in circular orbit with a period of 2.985 days. I use the high-resolution spectroscopic and extensive light curves from the ASAS and Hipparcos survey to measure the physical properties of the system. Previous attempts to model the light and radial velocity curves of the system have met with limited success, primarily because of the lack of a accurate photometric data. The system shows no signs of stellar activity, it is slowly rotating, has not been detected period changes, and there is no pulsational signs in the photometric data. I show the location of the components in effective temperature vs. luminosity diagram compared to the instability region limits established from eclipsing binary components. While more than 25 system have been plotted to diagram, about six single stars and OO Peg components do not show any pulsational frequencies. They are apparently constant stars lie within the pulsation instability region. I speculate as to the possible causes of this picture.