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tokens: that the 3:2 MMR of the orbital periods affect periodic variations of the Keplerian orbital parameters. She has obtained the expansion of disturbing function and identified only two first-order 3:2 resonance term. But we identify ( r + 1): r MMR terms in the expression of disturbing function and obtained the perturbations from the truncated disturbing function. In this manuscript, we have taken three exoplanetary systems namely Kepler-62, HD 200964 and Kepler-11 and as per our knowledge they contain planets in 2:1, 4:3 and 5:4 near MMRs, respectively. We apply theory discussed in Sections 3 and 4 individually in our three exoplanetary systems that we have chosen. This paper is organized as follows. In Section 2, we introduce the general three-body problem and the stability of exoplanetary system. The expansions of the disturbing function and perturbation equations of orbital elements are introduced in Section 3 . In Section 4, we present our secular resonance dynamics of exoplanetary system. Applications of the model for the case of 2:1 resonance are shown in Section 5 for Kepler-62 system. The case of the 4:3 resonance is discussed in Section 6 for HD 200964 system. In Section 7 , the case of 5:4 is discussed for Kepler-11 system. Finally, Section 8 is devoted to conclusions. 2 GENERAL THREE-BODY PROBLEM AND DYNAMICAL STABILITY Suppose the barycentric position vectors of star and two planets be , and , respectively. Let two planets of masses M 1 and M 2 orbiting a star of mass M ⋆ . Let the Jacobi coordinates and be the position of M 1 relative to M ⋆ and position of M 2 relative to the centre of mass M ⋆ and M 1 . We notice that this system is different from the restricted problems in which one of the bodies must have negligible mass. Also we ignore the effects of oblateness of star and the planets. We assume that the planets in all system are coplanar. This approximation of coplanarity makes sense because for exoplanets, their mutual inclination is not known with any precision, and is taken equal to zero (Beaugé, Ferraz-Mello Michtchenko 2003 ). Let a i , e i , λ i and ω i be the semimajor axis, eccentricity, mean longitude and the longitude of the pericentre of the i th planet for i = 1, 2. In the three-body problem, one of the interesting topic is the stability of the Solar system or exoplanetary system. Although, in celestial mechanics it is the unsolved problem till now, many scientist studied this because of its importance in many areas like space science, astronomy and astrophysics. In the context of planets and exoplanets formulation, Graziani Black ( 1981 ) studied conditions under which model planetary systems which consisting of a star and two planets with coplanar and initially circular orbits. Based on their results, they obtained a necessary condition for orbital stability where M 1 and M 2 are masses of planetary companions and M ⋆ is the mass of the star. The parameter Δ is the ratio of the separation distance between the