Journal of Astrophysics

Journal of Astrophysics / 2013 / Article

Research Article | Open Access

Volume 2013 |Article ID 898794 | 11 pages | https://doi.org/10.1155/2013/898794

On Robe's Circular Restricted Problem of Three Variable Mass Bodies

Academic Editor: M. Biesiada
Received25 Mar 2013
Accepted25 Aug 2013
Published22 Oct 2013

Abstract

This paper investigates the motion of a test particle around the equilibrium points under the setup of the Robe’s circular restricted three-body problem in which the masses of the three bodies vary arbitrarily with time at the same rate. The first primary is assumed to be a fluid in the shape of a sphere whose density also varies with time. The nonautonomous equations are derived and transformed to the autonomized form. Two collinear equilibrium points exist, with one positioned at the center of the fluid while the other exists for the mass ratio and density parameter provided the density parameter assumes value greater than one. Further, circular equilibrium points exist and pairs of out-of-plane equilibrium points forming triangles with the centers of the primaries are found. The out-of-plane points depend on the arbitrary constant , of the motion of the primaries, density ratio, and mass parameter. The linear stability of the equilibrium points is studied and it is seen that the circular and out-of-plane equilibrium points are unstable while the collinear equilibrium points are stable under some conditions. A numerical example regarding out-of-plane points is given in the case of the Earth, Moon, and submarine system. This study may be useful in the investigations of dynamic problem of the “ocean planets” Kepler-62e and Kepler-62f orbiting the star Kepler-62.

1. Introduction

The classical restricted three-body problem (RTBP) constitutes one of the most important problems in dynamical astronomy. The study of this problem is of great theoretical, practical, historical, and educational relevance. The investigation of this problem in its several versions has been the focus of continuous and intense research activity for more than two hundred years. The study of this problem in its many variants has had important implications in several scientific fields including, among others, celestial mechanics, galactic dynamics, chaos theory, and molecular physics. The RTBP is still a stimulating and active research field that has been receiving considerable attention of scientists and astronomers because of its applications in dynamics of the solar and stellar systems, lunar theory, and artificial satellites.

A different kind of restricted three-body problem was formulated by Robe [1], a set up in which the first primary is a rigid spherical shell filled with homogenous, incompressible fluid of density , and the second primary is a mass point outside the shell and moving around the first primary in a Keplerian orbit, while the infinitesimal mass is a small sphere of density moving inside the shell and is subject to the attraction of the second primary and the buoyancy force due to the fluid.

In estimating buoyancy force, Robe [1] assumed that the pressure field of the fluid has spherical symmetry around the center of the shell, and he considered only one out of the three components of the pressure field, which is due to the own gravitational field of the fluid .

A. R. Plastino and A. Plastino [2] took into account all these components of pressure field. But in their study, they assumed the hydrostatic equilibrium figure of the first primary as Roche’s ellipsoid. They found that when the density parameter is zero, every point inside the fluid is an equilibrium point; otherwise, the ellipsoid’s center is the only equilibrium point. They also examined the linear stability of equilibrium points. Hallan and Rana [3] investigated the existence of all equilibrium point and their stability in the Robe’s [1] problem. It was seen that the Robe’s elliptic restricted three-body problem has only one equilibrium point for all values of the density parameter and the mass parameter, while the Robe’s circular restricted three-body problem can have two, three, or infinite numbers of equilibrium points. As regards to the stability of these equilibria, they found that the collinear equilibrium points are stable while triangular and circular points are always unstable. Recently, Kaur and Aggarwal [4] investigated the Robe's problem of bodies and applied it to the study of the motion of two submarines in the Earth-Moon system. Singh and Hafsah [5] examined the Robe’s circular restricted three-body problem when the first primary is a fluid in the shape of an oblate spheroid and the second primary is a triaxial rigid body.

The classical restricted three-body problem assumes that the masses of celestial bodies are constant. However, the phenomenon of isotropic radiation or absorption in stars led scientists to formulate the restricted problem of three bodies with variable mass. As an example, we could mention the motion of rockets, black holes formation, motion of a satellite around a radiating star surrounded by a cloud and varying its mass due to particles of the cloud, and comets loosing part or all of their mass as a result of roaming around the Sun (or other stars) due to their interaction with the solar wind which blows off particles from their surfaces. The problem of the motion of astronomical objects with variable mass has many interesting applications in stellar, galactic, and planetary dynamics.

The study of two bodies with variable masses seems to have been first investigated by Dufour [6] where he examined the astronomical phenomena of variable mass relating the secular variation of lunar acceleration with the increase of the Earth’s mass due to the impact of meteorites. Later, Gylden [7] wrote the differential equations of motion for the problem when the masses are subject to variation. The integrable case to this differential equation was then given by Meshcherskii [8, 9]. The problem was later known as the Gylden-Meshcherskii problem. A characterization of this problem was studied by Singh and Leke [10]. The effect of the isotropic variation of the mass of the star in a planetary system and the possible ejection of a planet from the system were studied by Veras et al. [11]. Recently, Singh and Leke [12] investigated the existence and stability of equilibrium points in the Robe’s restricted three-body problem with variable masses.

Besides the Gylden-Meshcherskii problem, there are other different cases of two bodies with variable masses, which are classified according to the presence or absence of reactive forces, to whether the bodies move in an inertial frame or not, and so on (see [13]). For instance, when the particles are at rest in an inertial coordinate system, this case may be used to study the orbits of a celestial body moving through a static atmosphere, whose particles attach to it or detach from it as it moves. The restricted three-body problem with nonisotropic variation of the masses has been studied by Bekov [14], Bekov et al. [15], and Letelier and Da Silva [16]. A simple example of this kind of problem is the system of two variable primaries and a rocket. In this case, it is the thrust from the rocket that defines the force that acts on the test particle, in addition to the gravitational attraction from the two primaries, while the rocket does not affect the orbits of the primaries.

In this paper, the existence and stability of equilibrium points under the frame of the Robe problem [1], when the participating bodies vary their masses at the same rate, is studied. Here, we assume that the primaries move in a stationary medium, from which they absorb or lose mass; the first primary being a fluid in the shape of a sphere and the test particle which is a small sphere located inside the fluid also gain or lose mass to the fluid. Hence, there is no need to assume a rigid spherical shell. This study may be useful in the investigations of dynamic the problem of water-planetary system discovered by Kepler spacecraft. These “ocean planets” are orbiting the star Kepler-62 and are designated Kepler-62e and Kepler-62f. The existence of these Earth-size planets covered completely by a water envelope (water planets) has long fascinated scientists and the general public. The model of this problem can also be used to study the small oscillation of the Earth’s inner core taking into account the Moon’s attraction during the course of evolution.

This paper is orginzed as follows: Section 2 contains the equations of motion; the equilibrium points are investigated in Section 3; Section 4 investigates the linear stability of the equilibrium points; Section 5 discusses the obtained results and the conclusions.

2. Equations of Motion

Let be the mass of the first primary which is a fluid in the shape of a sphere of radius with center at having density and volume . Also, let be the mass of the second primary with center at which describes a circular orbit around the first one. Both masses are assumed to vary with time as they travel in a static medium which acts as a sink or source of mass. Now, let be the mass of the test particle whose mass is very small compared with the masses of the primaries, with center at , having density and volume . We suppose that its mass varies with time, also as it moves about in the fluid, it gains or loses mass to the medium. Let the positions vector between the center of the fluid and the centers of the second and the test particle be and , respectively, and let that between the test particle and the second primary be . Following Robe [1] and knowing that the masses, distances, and densities vary with time, the forces acting on the third body are the force of attraction of ; the gravitational force exerted by the fluid, that is ; and the buoyancy force exerted by the fluid which is .

We adopt a rotating coordinate system with origin at the center of mass, of the primaries, pointing towards the second primary, and being the orbital plane of . The equations of motion of the test particle, taking into account the forces acting on it, have the following form [1, 14]: where .

The barycentric coordinates and are connected with the distance between the primaries by the following equations: where , , ; , while is the gravitational constant and the over dot denotes differentiation with respect to time .

Now, in order to obtain useful dynamical predictions, we transform to the autonomous form . Following [15], the time dependence of the masses is described [15] by the function As in [14], the particular solutions for the case with variable parameters, and in the form of the Eddington-Jeans laws with indices and is expressed with the help of the function : where , and are constants. The exponent falls in the stellar range while and result, respectively, in the first and second law of Meshcherskii [8, 9] mass variations. Equations of (4) indicate that the laws of variation of the three masses are the same.

Also, the dynamical system has the particular solution of the following type [15, 17]: where is a constant, and is a constant of the area integral.

Finally, in addition, we assume that the densities of the fluid and the test particle vary such that where and are the densities of the medium and the test particle, respectively, at initial time .

Substituting (3) to (6) in (1) and reducing it throughout by , we get where Here, is constant and connects the parameter by the relation

Equations (5) and (9) indicate that the ratio of the product of the distances between the center of the primaries, mass of the test particle and the sum of the masses with the gravitational constant to the constant of the area integral, always remains a constant in both the autonomous and the non autonomous systems.

Now, we choose units for the distance and time, such that at initial time , , , respectively. Putting these in (9), for the unit of sum of the masses, we get .

Next, without loss of generality, we introduce the mass parameter defined as and also assume that the pressure field of the fluid of density maintains a spherical symmetry around the center of the fluid such that . Also, we have and . With the help of these units, the system of (7) takes the following form: where and the dash signifies differentiation with respect to the new time .

Equations (10) are the autonomized equations of motion of the test particle of our problem. These equations are different from that in [18] and analogous to the equations in Hallan and Rana [3] only differing due to the second term that appears in the force function and the parameter .

3. The Equilibrium Points

The equilibrium points represent stationary solutions of the RTBP. These solutions are the singularities of the manifold of the components of the velocity and the coordinates and are found by setting in the equations of motion (10). That is, they are the solutions of the equations , which are The solutions are categorized as follows.(1)The solutions of first equation of (12) with yield the collinear equilibrium points. These points lie on the line joining the center of the first and second primary. (2)When the first and the second equation of (12) are solved with , we get the circular points. These points lie in the spherical fluid and form circles.(3)The solutions of first and the third equations of (12) with results in the out-of-plane equilibrium points. These solutions are valid provided they lie inside the fluid. We shall consider them in Sections 3.1, 3.2, and 3.3, respectively.

3.1. Collinear Points

From first equation of (12), with , we get Hence, (13) has three roots, the first being and is always a solution whether or is not, for . The two remaining roots are found by considering the second equality in (13), which gives where .

Now, the solutions exist only for , however, the second solution is greater than and consequently will lie outside the shell, so we ignore it. The third solution is and is less than , the -coordinate of the second primary. Hence, there are two collinear equilibrium points which lie on the line joining the centers of the primaries. Therefore, the coordinate is always an equilibrium point. For , there exist an equilibrium point which lies to the left or right of the first primary depending upon whether or . When , the only equilibrium point is the center of the shell.

3.2. Circular Points

These solutions are found by solving the first and second equations of (12) with . Solving the second equation of (12) gives Substituting (16) in the first equation of (12) yields and consequently .

Hence, we have the solution which gives the coordinate of any point on the circle (17) with center which is the center of the second primary and radius one which is the distance between the centers of the fluid and the second primary. Thus, the solution gives us an infinite number of equilibrium points, provided they lie inside the fluid.

3.3. Out-of-Plane Points

The out-of-plane equilibrium points are found by solving first and third equations of (12) with . Solving first for in the third equation of (12), we get Substituting (18) in the first equation of (12) and simplifying results in Knowing that , substituting (18) and (19) in it, and solving for , we get Equations (19) and (20) give the position of real out-of-plane equilibrium points provided Should , then no real out-of-plane points exist as (20) turns out to be imaginary or complex quantity. When , these points fully coincide with that of Hallan and Rana [3]. When , (i.e., ), the coordinates of the out-of-plane points become the same with that in Singh and Leke [12]. Hence, it is seen that the equilibrium points are fully analogous to those found by Hallan and Rana [3] except for the out-of-plane equilibrium points which are affected by the parameter , the density parameter, and the mass ratio. The positions of the out-of-plane points are given in Tables 1, 2 and 3 and their graphical representations in Figures 1, 2, and 3 for a test particle in the Earth-Moon system, when the density parameter is negative, zero, and positive, respectively.


Comments

0.010.98009 Real out of plane point do not exist
0.50.4945Complex
0.999Real and negativeComplex
0.999001215.369Real out-of-plane points exist
1 1.91758
1.001 1.3988
1.002 1.12303
1.003 0.932023Real out-of-plane point exist
1.004 0.781521
1.005 0.652458
1.006 0.533794
1.007 0.416357
1.008 0.28657
1.009 0.0755768
Real and negativeImaginaryReal out-of-plane point do not exist


Comments

0.010.9801ComplexReal out of plane point do not exist
0.50.9801
0.9990.00099
0.9990010.00098901
10 Infinity Infinite remote solution
1.001 1.9138Real out-of-plane points exist
1.002 1.39986
1.003 1.12416
1.004 0.933202
1.005 0.782774
1.006 0.653819
1.007 0.535323
1.008 0.418177
1.009 0.289043
1.0091 0.274411
1.01 0.0839973
Real and negativeImaginaryReal out-of-plane point do not exist


Comments

0.010.98011ComplexReal out-of-plane point do not exist
0.50.4955
0.9990.001989
0.9990010.00198801
10.001
1.0010.000011
1.002−0.0009781.92083Real out-of-plane point exist
1.003−0.0019671.40162
1.004−0.0029561.12573
1.005−0.0039450.934716
1.006−0.0049340.784303
1.007−0.0059230.655425
1.008−0.0069120.537083
1.009−0.0079010.420232
1.0091−0.00799990.408219
1.01−0.00990.291786
1.0111−0.00997790.0393474
Real and negativeComplexReal out-of-plane point do not exist

We summarize our numerical effort as follows. In Table 1, when this implies that . In this case for and , out-of-plane points do not exist, but however exist in the interval . In Table 2, and so . In this case the out-of-plane points exist only when and do not exist in the remaining entire range of , while for Table 3, and so . Here, real out-of-plane solutions exist, for the values of the parameter , in the interval and are nonexistent for any value of outside this range. Hence, though has a large range of values, however, the physically meaningful range is , at which the out-of-plane points exist (see Figure 4). However, these ranges may differ for different density parameters , which are determined by the densities of the fluid and the test particle.

4. Stability of Equilibrium Points

To examine the stability of an equilibrium configuration, that is, its ability to restrain the body motion in its vicinity, we apply small displacement to the coordinates of the third body, to the positions, , and . If its motion rapidly departs from the vicinity of the point, we call such a position of equilibrium an unstable one. If however the body merely oscillates about the point, it is said to be a stable position.

Now, we linearize (10) to obtain the variational equations: where the superscript 0 indicates that the partial derivatives are to be evaluated at the equilibrium points.

4.1. Collinear Points

Robe [1] discussed the stability of the equilibrium point at the center of the shell, and Hallan and Rana [3] have also discussed that in the case of the noncollinear points when . Hence, we shall discuss here the stability of the equilibrium point near the center of the fluid. To do this, we let solutions of the first two equations of (21) be , , where , , and are constants.

Finding first and second derivatives of the solutions, substituting them in the first two equations of (21), and simplifying, we obtain the matrix which has a nonzero solution when Expanding the determinant, we get This is the characteristic equation corresponding to the variational equations (21) when motion is considered in the -plane.

Now, the values of the second order partial derivatives computed at the point , with the substitution are as follow:

where .

When , the equations in system (24) fully coincide with those of Hallan and Rana [3].

Substituting (24) in the variational equations (21), at once gives Now, (26) is independent of (25) and depicts that the motion parallel to the -axis is stable provided .

Now, the characteristic equation (23) using (24) becomes where , .

The roots of (28) are where is the discriminant of (27) and is always positive for any . When , the value of fully coincides with that of Hallan and Rana [3] which ought to be .

Now, since , if in (28) the quantity in parenthesis is positive; that is, , which occurs when we see that . Hence from (28), we have and so both values of are negative and consequently, the roots (28) are distinct pure imaginary. Therefore, the equilibrium point is stable provided equation (30) holds; otherwise, it is unstable.

4.2. Circular Points

These equilibrium points exist only for . The coordinates of any point on the circle , are of the form .

The partial derivatives at these points are When these are substituted in the variational equations (21) with , we have The last equation of (32) shows that motion is stable along the -axis. The characteristic equation of the first two equations of (32) is Its roots are , , and so the equilibrium points are unstable due to multiple zero roots.

4.3. Out-of-Plane Points

For the stability of the out-of-plane equilibrium points, we consider the following partial derivatives: The characteristic equation in this case is gotten by substituting the trial solutions , , in the variational equations (21) to get where Substituting (34) in (35), we at once have Its roots are where, , , .

The roots (37) are computed numerically for motion of a test particle (a submarine) under the gravitational attraction of the Earth-Moon system when and   ( and .) for . Therefore, we take and with the following values in each case following Kaur and Aggarwal [4].

In the case when , we takemass of test particle  kg, density of salt water  kg/m3,density of test particle  kg/m3.

In new units, we have, and so .

Similarly, when , we take mass of test particle  kg, density of salt water  kg/m3,density of submarine  kg/m3.

In new units, we have, , and so .

Aside from these examples, we also consider the case when (see Tables 1 and 3), so that a wider generalization can be reached regarding the characteristic roots (38) which consequently determines whether the equilibrium point is a stable one or not.

Using the software package Mathematica; the six characteristic roots are presented in Tables 4, 5, 6, and 7 numerically for , for different density parameters and a wide range of the parameter . We seek to find the case where all the six roots are pure imaginary quantities or complex figures with negative real parts. If this happens, then the solutions will be bounded and motion will be stable; otherwise, they will be unstable.



0.999001
1
1.001
1.002
1.003
1.004
1.009
1.01
1.0111



0.9990010.0000547723
10.0541419
1.0010.0756118
1.0020.0913455
1.0030.103949
1.0040.114444
1.0090.148257
1.010.152474
1.01110.156379



0.999001
1
1.001
1.0020.0540899
1.0030.0755428
1.0040.0912669
1.0090.137552