Badam Singh Kushvah

Stability regions of equilibrium points in restricted four-body problem with oblateness effects

In this paper, we extend the basic model of the restricted four-body problem introducing two bigger dominant primaries m1 and m2 as oblate spheroids when masses of the two primary bodies (m2 and m3) are equal. The aim of this study is to investigate the use of zero velocity surfaces and the Poincaré surfaces of section to determine the possible allowed boundary regions and the stability orbit of the equilibrium points. According to different values of Jacobi constant C, we can determine boundary region where the particle can move in possible permitted zones. The stability regions of the equilibrium points expanded due to presence of oblateness coefficient and various values of C, whereas for certain range of t (100≤t≤200), orbits form a shape of cote’s spiral. For different values of oblateness parameters A1 (0<A1<1) and A2 (0<A2<1), we obtain two collinear and six non-collinear equilibrium points. The non-collinear equilibrium points are stable when the mass parameter μ lies in the interval (0.0190637,0.647603). However, basins of attraction are constructed with the help of Newton Raphson method to demonstrate the convergence as well as divergence region of the equilibrium points. The nature of basins of attraction of the equilibrium points are less effected in presence and absence of oblateness coefficients A1 and A2 respectively in the proposed model.

Linear stability of equilibrium points in the generalized photogravitational Chermnykh’s problem

The equilibrium points and their linear stability has been discussed in the generalized photogravitational Chermnykh’s problem. The bigger primary is being considered as a source of radiation and small primary as an oblate spheroid. The effect of radiation pressure has been discussed numerically. The collinear points are linearly unstable and triangular points are stable in the sense of Lyapunov stability provided μ<μRouth=0.0385201. The effect of gravitational potential from the belt is also examined. The mathematical properties of this system are different from the classical restricted three body problem.

The effect of radiation pressure on the equilibrium points in the generalized photogravitational restricted three body problem

The existence of equilibrium points and the effect of radiation pressure have been discussed numerically. The problem is generalized by considering bigger primary as a source of radiation and small primary as an oblate spheroid. We have also discussed the PoyntingRobertson(P-R) effect which is caused due to radiation pressure. It is found that the collinear points L1, L2, L3 deviate from the axis joining the two primaries, while the triangular points L4, L5 are not symmetrical due to radiation pressure. We have seen that L1, L2, L3 are linearly unstable while L4, L5 are conditionally stable in the sense of Lyapunov when P-R effect is not considered. We have found that the effect of radiation pressure reduces the linear stability zones while P-R effect induces an instability in the sense of Lyapunov.

Equilibrium points and zero velocity surfaces in the restricted four-body problem with solar wind drag

We have analyzed the motion of an infinitesimal mass in the restricted four-body problem with solar wind drag. It is assumed that the forces which govern the motion are mutual gravitational attractions of the primaries, radiation pressure force and solar wind drag. We have derived the equations of motion and found the Jacobi integral, zero velocity surfaces, and particular solutions of the system. It is found that three collinear points are real when the radiation factor 0<β<0.1 whereas only one real point is obtained when 0.125<β<0.2. The stability property of the system is examined with the help of Poincaré surface of section (PSS) and Lyapunov characteristic exponents (LCEs). It is found that in presence of drag forces LCE is negative for a specific initial condition, hence the corresponding trajectory is regular whereas regular islands in the PSS are expanded.

Trajectories of L4 and Lyapunov Characteristic Exponents in the Generalized Photogravitational Chermnykh-Like problem

The dynamical behaviour of near by trajectories is being estimated by Lyapunov Characteristic Exponents(LCEs) in the Generalized Photogravitational Chermnykh-Like problem. It is found that the trajectories of the Lagrangian point L4 move along the epicycloid path, and spirally depart from the vicinity of the point. The LCEs remain positive for all the cases and depend on the initial deviation vector as well as renormalization time step. It is noticed that the trajectories are chaotic in nature and the L4 is asymptotically stable. The effects of radiation pressure, oblateness and mass of the belt are also examined in the present model. Subject headings: Trajectory:Lagrangian Point:LCEs:Photograviational:ChermnykhLike Problem:RTBP

Periodic orbits in the generalized photogravitational Chermnykh-like problem with power-law profile

The orbits about Lagrangian equilibrium points are important for scientific investigations. Since, a number of space missions have been completed and some are being proposed by various space agencies. In light of this, we consider a more realistic model in which a disk, with power-law density profile, is rotating around the common center of mass of the system. Then, we analyze the periodic motion in the neighborhood of Lagrangian equilibrium points for the value of mass parameter

Existence of equilibrium points and their linear stability in the generalized photogravitational Chermnykh-like problem with power-law profile

0<\mu\leq\frac{1}{2}

Geometry of halo and Lissajous orbits in the circular restricted three-body problem with drag forces

. Periodic orbits of the infinitesimal mass in the vicinity of equilibrium are studied analytically and numerically. In spite of the periodic orbits, we have found some other kind of orbits like hyperbolic, asymptotic etc. The effects of radiation factor as well as oblateness coefficients on the motion of infinitesimal mass in the neighborhood of equilibrium points are also examined. The stability criteria of the orbits is examined with the help of Poincaré surfaces of section (PSS) and found that stability regions depend on the Jacobi constant as well as other parameters.

Poynting-Robertson effect on the linear stability of equilibrium points in the generalized photogravitational Chermnykh’s problem

We consider the modified restricted three body problem with power-law density profile of disk, which rotates around the center of mass of the system with perturbed mean motion. Using analytical and numerical methods, we have found equilibrium points and examined their linear stability. We have also found the zero velocity surface for the present model. In addition to five equilibrium points there exists a new equilibrium point on the line joining the two primaries. It is found that L1 and L3 are stable for some values of inner and outer radius of the disk while other collinear points are unstable, but L4 is conditionally stable for mass ratio less than that of Routh’s critical value. Lastly, we have studied the effects of radiation pressure, oblateness and mass of the disk on the motion and stability of equilibrium points.

Orbital dynamics of exoplanetary systems Kepler-62, HD 200964 and Kepler-11

In this paper, we determine the effect of radiation pressure, Poynting-Robertson drag and solar wind drag on the Sun-(Earth-Moon) restricted three body problem. Here, we take the larger body of the Sun as a larger primary, and Earth+Moon as a smaller primary. With the help of the perturbation technique, we find the Lagrangian points, and see that the collinear points deviate from the axis joining the primaries, whereas the triangular points remain unchanged in their configuration. We also find that Lagrangian points move towards the Sun when radiation pressure increases. We have also analysed the stability of the triangular equilibrium points and have found that they are unstable because of the drag forces. Moreover, we have computed the halo orbits in the third-order approximation using Lindstedt-Poincar