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Taking into account the results obtained from the models and analyses of theBVRI light curves, we discuss the nature of V1464 Aql. The analyses indicatedthat the mass ratio of the system is q=0.71(0.02), while the inclination of thesystem (i) is 38.45(0.22) deg. Taking the primary component's temperature as7420(192) K, we found that the temperature of the secondary is 6232(161) K. Themass of the primary component was found to be 1.74(0.05) Msun, while it is1.23(0.01) Msun for the secondary. The primary component's radius was found tobe 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 thatthe main variation with large amplitude should be caused due to the ellipsoidaleffect. Indeed, the Fourier analysis also supported the result. For the firsttime in the literature, we revealed that the primary component is a delta Scutistar. 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 plottedV1464 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 theplane of log(Porb)-log(Ppulse) for each type binary. Using the linear fit ofeach group, we obtained new calibrations between log(Porb) and log(Ppulse) fordifferent type pulsating stars. In addition, a calibration has been obtainedfor 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 witha delta Scuti component.

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