Periodic Orbits in the Photogravitational Restricted Problem When the Primaries Are Triaxial Rigid Bodies

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Received 2 December 2015; accepted 26 March 2016; published 30 March 2016

1. Introduction

This paper is the extension of our papers, Mittal et al. [1] - [3] . Charlier [4] and Plummer [5] studied the existence of two families of small periodic motions in the neighborhood of Lagrangian solutions in the plane circular restricted three-body problem, with different values of the parameter μ. Riabov [6] investigated periodic motions analytically. Szebehely [7] has described the results on the periodic motions of circular restricted three-body problem. Deprit and Henrard [8] gave more results on periodic motions in their paper. Markeev and Sokolsky [9] worked on the small periodic motions generated by Lagrangian solutions for all values of μ and for small values of h for which the conditions of holomorphic integral theorem are valid. Hadjidemetriou [10] has discussed the continuation of periodic orbits from the restricted to the general three-body problem. Karimov and Sokolsky [11] have studied the periodic motions generated by Lagrangian solutions of the circular restricted three-body problem by using mobile co-ordinates and by taking displacements along the tangent and the normal. Aggarwal et al. [12] have discussed the non-linear stability of the triangular libration point when both the primaries are radiated axe symmetric rigid bodies in the presence of third and forth order resonance. Abouelmagd et al. [13] have studied the periodic structure of the restricted three-body problem considering the effect of the zonal harmonics J_{2} and J_{4} for the more massive body. They showed that the triangular points in the restricted three-body problem have long or short periodic orbits in the range 0 ≤ µ < µ_{c}. Perdios et al. [14] have studied the equilibrium points and related periodic motions in the restricted three-body problem with angular velocity and radiation effects. Jain and Aggarwal [15] have studied the stability and existence of non-collinear libration points in restricted three-body problem with stokes drag effect when smaller primary is an oblate spheroid.

The celestial bodies are in general axis-symmetric bodies, so its shape should be taken into account as well. The replacement of mass point by rigid-body is quite important because of its wide applications. The re-entry of artificial satellite has shown the importance of periodic orbits.

That is why, we have thought of studying, in this paper, the periodic orbits generated by Lagrangian solutions of the restricted three-body problem when both the primaries are triaxial rigid bodies and source of radiation pressure. We determine the periodic orbits by giving displacements at the mobile co-ordinates along the tangent and normal. We have also determined family of periodic orbits by fixing μ (mass ratio of the two primaries) and changing the values of (parameters of the triaxial rigid bodies), P and (the radiation parameters) and varying h (energy constant). We have also studied the effect of triaxial parameters_{ }and the radiation pressure on the energy constant (h).

Most of the authors have not taken into account the effect of the solar radiation pressure in the motion of the third body whereas we have taken both the primaries as radiating triaxial rigid bodies. Besides taking both the primaries as triaxial rigid bodies and the source of radiation, we have used mobile-coordinates and given the displacement along the normal and the tangent to the orbit which has wider applications in space dynamics. We have drawn the periodic orbits by using the predictor-corrector method which is given in detail in our papers [1] - [3] .

2. Equations of Motion

Following the procedure of our papers [1] - [3] , we consider three masses with and bodies with masses revolve with angular velocity n (say) in circular orbits without rotation about the centre of mass O. Let there be an infinitesimal mass which is moving in the plane of motion of and is being influenced by their motion but not influencing them. Let the line joining be taken as X-axis and O their centre of mass as origin. Let the line through O and perpendicular to OX, and lying in the plane of motion of being Y-axis. Let us consider a synodic system of coordinates O(XYZ), initially coincident with the inertial system O(XYZ), rotating with the angular velocity n about Z-axis; (the Z-axis is coincident with Z-axis). We choose unit of mass such that the unit of distance and unit of time is so chosen that. Using the dimensionless variables, we find the Lagrangian function L and the equations of motion of the infinitesimal mass in the restricted three-body problem when both the primaries are radiating triaxial rigid bodies in the synodic co-ordinate system (Figure 1).

Equations of motion with Lagrangian function L are given by

where

(1)

Figure 1. Configuration of the restricted three-body problem with masses m_{1} and m_{2} as radiating triaxial rigid bodies.

; and are the parameters of triaxial rigid bodies. It may be noted that n is independent of and and P and (the radiation parameters),

,

,

,

,

a, b, c = length of the semi axes of the triaxial body of mass,

= length of the semi axes of the triaxial body of mass,

R = dimensional distance between the primaries,

,

,

U = constant to be so chosen such that h (energy constant) will vanish at (libration point).

The coordinates of (libration) are

,

,

where, , , ,

, , , ,

and

Equations of motion can also be written as

,

(2)

where

The Jacobi integral is

(3)

3. Normal and Tangent Variables

We consider the system of generalized coordinates They depend upon the eight parameters The corresponding differential equations are given by the system of Equation

(2) with Jacobi integral given by (3). We consider the solutions of Equations (2) for which C is zero. If we consider the solutions of Equation (2) given by (4) for some fixed parameters value p then there may exist

another solution given by (5) with another parameter value close to p. We have

(4)

and

(5)

Solution (5) will reduce to Solution (4) as.

Now we give the displacements

and, (where and)

i.e., , , , ,

, , , (6)

and

(6a)

We consider and as small quantities of the same order. Then we have the following variational equations:

(7)

with the integral constructed from Equation (3), retaining the first order terms only, we get

(7a)

The modulus of momentary velocity on the orbit is defined as. We assume that (5)

is not corresponding to the equilibrium state, i.e., and we further assume that on the whole orbit. Therefore, x and y become the mobile co-ordinates. We will, now, use the mobile coordinate system to draw the periodic orbits by resolving one of the axis along the velocity vector and the other axis along the normal vector.

In the new coordinate system, we consider the transition matrix S as follows:

Consider the first column of S as

= the unit vector which is normal to the orbit, i.e., it is orthogonal to the vector s(t).

= the unit vector which is tangent to the orbit and is the last column of the matrix S.

So, we have, dim(r) = 2 × 1, dim(s) = 2 × 1, so that dim(s) = 2 × 2.

It can be easily verified that

It may be noted that,

.

Now, we may further define

, the first line of S^{−}^{1},

, the last line of S^{−1}.

We write, the vector of local coordinates, in the new coordinate system as follows:

where N is displacement along the normal to the orbit and M is displacement along the tangent to the orbit.

Then, the new coordinates are given by

(8)

(9)

Substituting these values into the integral (7a), we have

(10)

Equation (10) can be solved for as

(11)

Equations of motion (2) for the new coordinates are

.

where,

and and are the same as in our papers [1] - [3] .

Since, therefore the equations of motion in normal and tangent co-ordinates can be written as

(12)

and

. (13)

can also be written as

Thus, we have derived the equation in which possesses the remarkable property that the normal coordinate (N) is independent of the tangent coordinate (M). Moreover, instead of the differential equation of the second order (13), we can use the first order differential Equation (11). If the investigated motion (4) is periodic, then the matrix S(t) can be taken as periodic and Equations (12) and (13) will have the periodic coefficients at.

4. Periodic Orbits

For determining the periodic orbits, the required equations of motion and the variational equations are given as:

(14i)

(14ii)

(14iii)

(14iv)

(14v)

. (14vi)

where is the matrix of solutions of a homogeneous system with initial condition and particular solution of the equations with zero initial conditions, i.e.,. The row-vector and are the solutions of Cauchy problem (iv) with (vi) of (14). The order of the above system is thirty-four.

So, for finding the new periodic motion it is necessary to integrate the system (14) of the differential equations from t = 0 and t = T. In the formulae (i) to (vi) of (14), it may be noted that I_{2J} = (e_{1}… e_{2J}), Z = (Z_{1}…Z_{2J}), μ = (μ_{1}, …, μ_{2J}) and the initial conditions x(0), y(0), and are known.

After solving the above equations of motion (i) and (ii), the variational Equations (iii)-(vi) of (14) and applying the predictor-corrector method, we have determined the periodic orbits.

We have drawn the periodic orbits for the following:

1) for fixed μ = 0.001, A_{1} = 0.0, A_{2} = 0.0, = 0.001, = 0.0, P = 0.0 and = 0.0 (Figure 2);

2) for fixed μ = 0.001, A_{1} = 0.001, A_{2} = 0.0, = 0.001, = 0.0, P = 0.0001 and = 0.00 (Figure 3);

3) for fixed μ = 0.001, A_{1} = 0.001, A_{2} = 0.001, = 0.0, = 0.0, P = 0.0 and = 0.0001 (Figure 4);

4) for fixed μ = 0.001, A_{1} = 0.001, A_{2} = 0.001, = 0.001, = 0.001, P = 0.0001 and = 0.0001 (Figure 5);

5) for fixed μ = 0.001, A_{1} = 0.002, A_{2} = 0.003, = 0.004, = 0.005, P = 0.001 and = 0.001 (Figure 6).

Figure 2. Periodic orbits when μ = 0.001, = 0.0, = 0.0, = 0.001, = 0.0, P = 0.0 and = 0.0.

Figure 3. Periodic orbits when μ = 0.001, = 0.001, = 0.0, = 0.001, = 0.0, P = 0.0001 and = 0.0.

Figure 4. Periodic orbits when μ = 0.001, = 0.001, = 0.001, = 0.0, = 0.0, P = 0.00 and = 0.0001.

Figure 5. Periodic orbits when μ = 0.01, = 0.001, = 0.001, = 0.001, = 0.001, P = 0.0001 and = 0.0001.

Figure 6. Periodic orbits when μ = 0.003, = 0.002, = 0.003, = 0.004, = 0.005, P = 0.001 and = 0.001.

In each figure, we have drawn 5 periodic orbits corresponding to different values of h. These orbits have been numbered 1, 2, 3, 4 and 5 corresponding to different values of h.

The above analysis is summed up in Table 1. By taking both the primaries as radiating triaxial rigid bodies, the difference in the behavior of the values of h is obvious.

5. Conclusions

Karimov and Sokolsky [11] have studied periodic orbits in the restricted three body problem by giving the displacements along the normal and the tangent to the orbit at the mobile co-ordinates. They have taken both the primaries as point masses while in this paper besides taking both the primaries as triaxial rigid bodies, we have also taken both the primaries as source of radiation pressure as well. In this paper, we have again determined

Table 1. The summary analysis of the periodic orbits.

five periodic orbits in a family for fixed value of the mass parameter μ, the triaxial parameters and the radiation parameters P and with varying energy constant h.

We have observed the following effects on the periodic orbits and on the energy constant h due to triaxial rigid bodies and radiation pressure if we compare it with the results of Karimov and Sokolsky [11] and our papers [1] - [3] .

1) The energy constant h increases in a family (for Figure 2 and Figure 3) then it decreases (for Figures 4-6) for fixed trixial parameters and radiation parameters P and.

2) As we increase the radiation parameters P and, the energy constant h increases whereas the periodic orbits shrink a little.

3) The periodic orbits go away from the libration point as we increase triaxial parameters and radiation parameters P and whereas energy constant h decrease.

We have investigated the family up to the member which touches the point. It is observed that the families of periodic orbits in Karimov and Sokolsky [11] terminate at both the triangular equilibrium points simultaneously, while in our case these families are non-symmetrical, so they may continue.

Acknowledgements

We are thankful to the Centre for Fundamental Research in Space Dynamics and Celestial Mechanics (CFRSC), Delhi and the Deanship of Scientific Research, College of Science in Zulfi, Majmaah University, KSA for providing all the research facilities in the completion of this research work.

References

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