INTRODUCTION The stellar evolutionary theory, the stellar pulsation and binaries are the three most common ways help astronomers to study celestial objects as well as to study about the universes. The investigation and review by Murphy (2017) pointed out that the existence of the stars in binary and multiple systems outnumber of single stars by at least 2:1 (Murphy et al. 2017). With this work we arrived at the possible way the binarogram helpful to recognize the orbital peaks of low orbit delta Secuti stars from factious peaks with a strong confidence. Then, we obtained two a small kepler binaries with the method by modifying it. DATA AND MATHOD The method which we modified and used for detecting binarity is that of Balona (2014) using Kepler light curves. He discussed that the uniqueness of the method is that a direct periodogram of the orbital frequency is derived using all possible information to extract the time delay from the stellar pulsations. They also suggested that the particular advantage of using the time delay through constructing the binarogram curve in identifying that a Kepler pulsating star has a companion is that the curve displays the orbital frequencies from which all other orbital parameters are determined. The central messages of obtaining equal numerical values of forb at each pulsation frequency is that the causes of the time- delay is the presence of a companion of a Kepler pulsating star. And the reciprocal of this orbital frequency gives the orbital period of a star. RESULT AND DISCUSSION We modified the method through extracting several highest orbital frequencies with their corresponding a(sin(i)) from our final data which provides the banarograms at each pulsation frequencies. This is because of it can avoid several error may introduced during we read the numerical value of orbital frequencies from the graph directly. Then, we have introduced the horizontal vertical lines in previous binarogram so that clarify the how the orbital frequencies at each pulsation frequencies do not show a large variations unlike that of a(sin(i)). Figure-1: The three binarograms of KIC 4150611. The right panel is the modified binarogram which is the first out come of this our present work. The right panel is the modified of the middle one. Then we identified two δ Scuti stars wich has the orbital period of less than 50 d. That is KIC 8042044 and KIC 3952623 are 46.08 d and 19.5d respectively. These are shown in the figure-2 and fgure- 3. Figure-2: The modified binarogram (frequency versus a(sini)) of KIC 3952623 which shows the orbital frequency and period are 0.0217 d- and 46.08 respectively d. Figure-3: The modified binarogram of KIC 8042044 which shows the orbital frequency and period are0.0513 d- and 19.49 d respectively. CONCLUSSION AND FUTURE WORK This study shows that the orbital peak of KIC 8042044 and KIC 3952623 are 46.08 d and 19.5d respectively. The additional peaks in the binaroram of the second object needs further investigations. This shows thatit is possible to determine the orbital period of small orbits for a few binaries. Thus, the modified method is applicable to find a small orbit Kepler Binaries by overcoming others interference limit us to recognize the correct orbital peaks. We also intended to apply this modified binarogram on a plenty of unsolved problems pointed out in Murphy et. al (2017) and similar others. Acknowledgement This task includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. YAM wish to thank the Kepler team for their generosity in allowing the data to be released and for their outstanding efforts which have made these results possible. REFERENCES L.A. Balona, 2014, Binary star detection using the time-delay method: application to 34 Kepler objects of interest, MNRAS 443, 1946–1954 S. Murpy, 2017, Finding binaries from phase modulation of pulsating stars with Kepler, Monthly Notices of the Royal Astron