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The Nature of V1464 Aql: A New Ellipsoidal Variable with a Delta Scuti Component

Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q=0.71(0.02), while the inclination of the system (i) is 38.45(0.22) deg. Taking the primary component's temperature as 7420(192) K, we found that the temperature of the secondary is 6232(161) K. The mass of the primary component was found to be 1.74(0.05) Msun, while it is 1.23(0.01) Msun for the secondary. The primary component's radius was found to be 2.10(0.05) Rsun, while it was found as 1.80(0.01) Rsun for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a delta Scuti star. The period of pulsation was found to be 58.482(0.002), 58.482(0.001), 60.966(0.002), 60.964(0.003) minutes in BVRI bands, respectively. We plotted V1464 Aql in the plane of log(Porb)-log(Ppulse). Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the plane of log(Porb)-log(Ppulse) for each type binary. Using the linear fit of each group, we obtained new calibrations between log(Porb) and log(Ppulse) for different type pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars from the spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a delta Scuti component.