Stability of circular orbits of spinning particles in Schwarzschild-like space-times

Stability of circular orbits of spinning particles in Schwarzschild-like space-times

Morteza Mohseni
Physics Department, Payame Noor University, 19395-4697 Tehran, Iran
E-mail address:m-mohseni@pnu.ac.ir
Abstract

Circular orbits of spinning test particles and their stability in Schwarzschild-like backgrounds are investigated. For these space-times the equations of motion admit solutions representing circular orbits with particles spins being constant and normal to the plane of orbits. For the de Sitter background the orbits are always stable with particle velocity and momentum being co-linear along them. The world-line deviation equations for particles of the same spin-to-mass ratios are solved and the resulting deviation vectors are used to study the stability of orbits. It is shown that the orbits are stable against radial perturbations. The general criterion for stability against normal perturbations is obtained. Explicit calculations are performed in the case of the Schwarzschild space-time leading to the conclusion that the orbits are stable.

keywords: Stability of orbits, Spinning particles

PACS: 04.20.-q, 04.70.-s, 95.10.Fh

1 Introduction

Orbits of particles in curved space-times have long been a topic of interest in physics and astronomy. In relativistic theories of motion, orbits of particles around astronomical objects have been studied extensively in the past and have resulted in a plethora of phenomena ranging from the perihelion precession and bending of light to more recent ones like the so-called clock effect [1]. Nearly circular orbits have had a especial role in this regard. Their application in theories dealing with accretion discs [2] (see also [3] and references therein) is an example showing their importance. Some of the objects moving on such orbits may have some internal angular momentum. In trying to model the motion of such rotating objects treated as test particles, one is lead to the Mathisson-Papapetrou-Dixon (MPD) equations [4, 5, 6, 7]. According to these equations, in general the trajectories of a spinning particle moving in a curved background differ from the geodesics of the background space-time as a result of a coupling between the particle spin and the space-time curvature and furthermore, its momentum and velocity are not in general parallel.

Being a system of highly coupled differential equations, the MPD equations are usually difficult to solve and only a few analytical solutions to them are known, e.g. the one introduced in [8] in which the motion in the equatorial plane of a Kerr black hole with a fixed particle spin was investigated. Following the ideas presented in the latter reference, solutions describing circular or nearly circular orbits in various black hole space-times have been found. Different aspects of such orbits have been studied in the case of Lense-Thirring space-time in [9], in the case of Schwarzschild space-time in [10, 11, 12, 13, 14] (also in [15] for non-circular orbits), in the case of Kerr black hole in [16, 17, 18, 19, 20, 21, 22, 23, 24], in the case of Reissner-Nordström black hole in [25], and in the case of Weyl space-time in [26]. An alternative framework has been used in [27, 28] and [29] to study orbits of spinning particles in Schwarzschild and Kerr-Newman space-times respectively.

An interesting question is whether these orbits are stable. For the case of (spinless) test particles this question has been considered in [30, 31] where deviation of circular geodesics in static spherically symmetric space-times was studied. The aim of the present work is to investigate this (in)stability for orbits of spinning particles. The technique we use in this regard is to study the growth of perturbations to a given orbit. These perturbations are essentially deviations from a fiducial orbit to adjacent ones. Unbounded growth of a perturbation signals instability of the orbit. A recent application of this technique may be found in [32] in which the geodesic deviation equation is used to study the stability of circular orbits of test particles in Einstein-Gauss-Bonnet gravity. In fact as it has been argued in [33] the deviation vectors may be used to define Lyapunov indices in general relativity for either geodesic or non-geodesics flows. The method of Lyapunov indices has been applied to study the stability of circular or non-circular orbits of spinning particles in [9, 10, 11, 15]. In particular in [11] it was shown that using different supplementary conditions may result in different stability behaviour of spinning particles orbiting the Schwarzchild black hole. The problem of chaotic motion of spinning particles in Schwarzschild space-time has also been studied in [34] but in that work the deviation equations were not used and a numerical scheme based on a time series method was used instead. Chaotic motion of spinning particles around the Schwarzschild black hole has also been studied in [35] from a different perspective. The case of Kerr balck hole has been considered in [36].

To study perturbations of spinning particles orbits, the geodesic deviation equation is no longer the appropriate equation, instead we should use its generalization as presented in [37] or [38]. A similar set of equations have been obtained in [39] for the case of charged spinning particles. In this work we deploy the machinery developed in [38] to obtain the deviations.

As it has been argued in [40] the test particle approach leading to equations like the MPD equations, is valid only when the particles spins are small compared to the characteristic length of the background they are moving in. Thus throughout this work we assume the particles specific spins (i.e., their spin-to-mass ratios) to be small compared with the mass of the black hole.

The paper is organized as follows. In the next section we give a brief review of the MPD equations and show how a solution describing a circular orbit can be found in a rather general Schwarzschild-like space-time. Although circular orbits in particular spherically symmetric backgrounds have been studied in detail in some of the above mentioned references, that section serves both as a rather unified manner review of the main results essential for the subsequent sections and to fix the notation. The latter is of importance because a variety of notations have been used in the literature. These include the way in which the gauge is fixed and the particle spin tensor is related to the spin vector. The case of de Sitter space-time is simpler and is studied in a separate section as a warm up. Then we solve the world-line deviation equations for circular orbits and use them to study the behaviour of the perturbations. Even though our focus of attention is on orbits in Schwarzschild space-time, we obtain some general criteria under which the orbits are (un)stable in a general Schwarzschild-like space-time. The paper is concluded with a discussion of the results.

2 Circular Orbits

The basic equations governing the motion of a spinning test particle are [7]

(1)
(2)
(3)

in which are the particle velocity, momentum, and spin respectively, with being the covariant derivative, and

represents the space-time curvature tensor. The particle spin is related to its spin vector by [8]

(4)

with being the alternating symbol. In this work we adopt . It should be noted that a different defining equation is sometimes used in this regard (see e.g. equation A1 of [34]). As a consequence of these equations one can show that the particle mass and spin are constant

(5)
(6)

We choose the following gauge fixing relation [7]

(7)

in which the particle instantaneous zero-momentum and zero-velocity frames are simultaneous [41]. This is the gauge in which the velocity-momentum relation [8, 41]

(8)

which is itself a consequence of the equations of motion, takes the simplest form.

We consider the motion of a spinning test particle in a Schwarzschild-like background space-time described in the coordinate system by the line element

(9)

in which the explicit form of is subject to the Einstein field equations. This metric corresponds to Schwarzschild space-time for , to Reissner-Nordström space-time for , to de Sitter space-time , to Schwarzschild-de Sitter space-time for , and to Reissner-Nordström- de Sitter space-time for .

Inspired by the results of [8], we consider a spinning particle moving on a circular orbit in the equatorial plane with a velocity . We take the particle spin vector perpendicular to this plane. Thus we set

(10)

and look for a consistent solution

(11)

of the equations of motion (1) and (2). Note that Eqs. (10) and (11) are consistent with Eq. (3) by construction. Now making use of Eq. (4), we can insert this ansatz into Eq. (1), to obtain

(12)
(13)
(14)

where , and . Similarly, equation (2) leads to

(15)
(16)
(17)

Solving Eqs. (12),(14),(15), and (17) for the components of lead to

(18)
(19)
(20)

Now the remaining two equations, (13) and (16), together with Eqs. (5) and (7) reduce to the following system of algebraic equations

(21)
(22)
(23)
(24)

from which we can obtain the non-vanishing components of and .

3 Motion in de Sitter space-time

To proceed further, we first consider the simplest case where and are parallel, i.e. but . Taking this into account, the above system of algebraic equations are consistent only for an of the form of , being a constant. This corresponds to the well-known de Sitter space-time. Thus we set

(25)

This restriction means that there is no solution describing a circular orbit with velocity and momentum being parallel in other Schwarzschild-like space-times. From the fact that de Sitter space-time is homogeneous we already expected and to be parallel. This is easily confirmed by the above equations resulting in

(26)

The angular velocity of particle is independent of the orbit it moves on.

We now aim to investigate the stability of these orbits. To this end, we consider the behaviour of perturbations in different directions. Unbounded growth of a perturbation is a signature of instability. A suitable framework to study stabilities is the world-line deviation equations developed in [38]. However, in this case the momentum and velocity four-vectors are co-linear and the equations of motion reduce to the geodesic equation. In fact for maximally symmetric space-times we have

(27)

where is constant. Inserting this into Eq. (1) returns

On the other hand by combining the above relation with Eq. (8) and making use of Eq. (3) we arrive at the previously mentioned result . Thus

i.e. particles move along geodesics and their momentum and spin are parallel. Hence we can deploy the well-known geodesic deviation equation instead of the world-line deviation equations. It reads

(28)

where is the deviation between adjacent trajectories . Applying this equation to the above circular orbits results in

(29)
(30)
(31)
(32)

where

By integrating the first, the third, and the last equation in the above system of equations we obtain

(33)
(34)
(35)

in which are constants. The second equation above shows that the circular orbits considered here are stable against normal (i.e., in the -direction) perturbations. To see the effect of radial perturbations, we first insert the values of into the expression for to get . We then insert this back into Eq. (30) and solve it for with the aid of Eqs. (33) and (34) to obtain

(36)

in which are constants. This leads us to the conclusion that the orbits are stable against radial perturbations.

4 Motion in other Schwarzschild-like space-times

Relaxing the simplifying assumption of the previous section, we now seek general solutions to Eqs. (21)-(24). In general these equations admit two sets of solutions which, roughly speaking, correspond to two senses of rotation with respect to a given spin direction. Labelling the solutions by and respectively, we have

(37)
(38)
(39)
(40)

where

An interesting property of these solutions is that under the absolute values of and change in general. This is due to the spin-dependent character of the force exerted on the particles. Also note that the and solutions do not represent physically distinct situations. This can be easily seen from the above expressions in which interchanges and solutions (up to an overall minus sign). In fact only two of the four possible situations are independent because there is no preferred up or down direction in a spherically symmetric space.

To get more physical insight into the nature of the above solutions we consider the case of Schwarzschild space-time. The functions are depicted in Fig. 1 in which the range of is chosen as to conform with the requirement and the range of is taken as since for , becomes imaginary, i.e. there is no circular orbit for this range. The case needs special care and is discussed later.

Figure 1: The angular velocity of particles (left) and (right) in terms of and .

The asymmetry is obvious in these graphs. They also show that for large values of the two solutions coincides. To ease comparison, the absolute value of is depicted in Fig. 2. It coincides with the left-hand side plot in Fig. 1 upon taking .

Figure 2: The function in terms of and .

We have also depicted the functions in Fig. 3. It shows that for larger values of the difference between and diminishes. This is because a larger results in a value of closer to unity and hence a smaller curvature which in turn results in a smaller spin-curvature coupling.

Figure 3: The non-co-linearity (left) and (right) in terms of and .

To investigate the special case of mentioned earlier, we first consider the case of a particle without spin. For , Eq. (24) is satisfied identically, and the remaining Eqs. (21)-(23) result in

(41)

which for the Schwarzschild space-time implies . When , Eqs. (21)-(24) do admit a solution given by

(42)
(43)
(44)

where and in Eqs. (42) and (44) are chosen according to the sign of .

Two further remarks are in order. First, an ansatz corresponding to particles moving on circular orbits with the spin vector making an arbitrary angle with the plane of the orbit, say , is not in general compatible with the equations of motion. Second, since the Schwarzschild-like space-times are spherically symmetric there is no preferred equatorial plane and hence similar circular orbits on other planes are also allowed.

5 Stability of orbits

In general, orbits of spinning particles are not geodesics of the background they are moving in and we can not use the geodesic deviation equation. In this work we use the world-line deviation equations [38]

(45)
(46)
(47)

where and . The dimensions of various quantities used in these equations are shown in Table 1.

Quantity
Dimension
Table 1: The dimensions of various quantities used in world-line deviation equations. Here abbreviates length, , and

The above equations are the generalization of geodesic deviation equation to world-line deviations of spinning particles of the same specific spins. In fact setting in Eq. (46) immediately results in

in which is a constant. Inserting this back into Eq. (45) we arrive at Eq. (28), the geodesic deviation equation. It is interesting to note that, according to Eq. (45), even if we neglect the direct effect of spin, i.e. the first three terms in the right hand side of that equation, the particles spin still affect the dynamics through in the last term which in turn depends on spin. The following additional equations

(48)
(49)

resulting from the constants of motion Eqs. (5) and (6) respectively are also useful in this regard.

We now consider a family of circular orbits and take a typical circular orbit of definite radius in the equatorial plane along which the particle spin is constant and orthogonal the plane of orbit, as the fiducial path. Deviations from this orbit can be obtained by solving Eqs. (45) and (46) for but before embarking on that, it would be useful to reduce the number of unknowns by using Eqs. (47)-(49). From Eq. (48) we have

(50)

and from Eq. (49) we have

(51)

Similarly Eq. (47) result in

(52)
(53)
(54)

Now, taking Eqs. (50)-(54) into account, from Eq. (45) with and we obtain

(55)
(56)
(57)
(58)

respectively. Similarly from Eq. (46) with , and we obtain

(59)
(60)
(61)
(62)
(63)

respectively. Note that setting lead to Eq. (59) again.

Eqs. (55), (56), (58), (59), and (61) result in

which is simply separation between two adjacent circular orbits, and

Thus radial perturbations do not lead to instability.

The solutions to Eqs. (57), (60), (62), and (63) are given by

(64)

and similar expressions for . Here are constants,

Note that under we have . Thus for we have oscillatory and terms only and the orbits are stable. For there are both oscillatory and exponential terms and the orbits are not in general stable. Depending on the values of space-time parameters and the particles specific spins , both cases may occur. For the case of Schwarzschild space-time we have depicted in terms of and in Fig. 4. According to this figure both solutions corresponds to stable orbits in Schwarzschild space-time, at least for the range of parameters chosen here.

Figure 4: (left) and (right) in terms of .

6 Discussion

We have studied circular orbits of spinning particles with their spins perpendicular to the plane of motion in spherically symmetric space- times. We have shown that circular orbits of spinning particles with their velocity and momentum being parallel are only allowed in de Sitter case. For other cases the particle velocity and momentum are not parallel. We have obtained general expressions for the particle angular velocities and momenta in terms of the radii of orbits and specific spins. Depending on the sense of rotation with respect to the spin direction, there are in general two physically equivalent sets of such expressions for any given radius. According to these expressions, for a fixed spin direction and orbit, the absolute values of angular velocities of particles orbiting in opposite senses are different. This is due to the spin-dependent force exerted on particles. For the case of Schwarzschild space-time, there is no circular orbit of radius smaller than three (measured in units of the black hole mass). This is in agreement with the results of [10]. The effects due to spin decrease when the radius of the orbits increase because the curvature and hence the spin-curvature coupling decreases with radius.

We have also solved the world-line deviation equations of spinning particles of the same specific spins moving on orbits described above. The resulting deviation vectors have been used to show that the orbits are stable against radial perturbations. We have determined the general condition under which the orbits are stable against normal perturbations. It shows that in general particles orbiting in opposite senses have different deviations which may result in different stability properties. By explicit calculations we have shown that the orbits are stable in Schwarzschild space-time. An advantage of our approach is that some rather general results can be extracted from the equations without resort to detailed numerical calculations. These results might be of interest in studies related to (in)stability of non-geodesic flows. The deviations obtained here enable us to compute the corresponding Lyapunov indices. Although the special case studied here, i.e. exactly circular orbits with a perpendicular spin may not be realized in real astrophysical situations, it can be regarded as a toy model which can be extended to more realistic situations. Possible interesting extensions include a study of stability of spinning particle orbits in a Kerr-type background and charged spinning particles in a Reissner-Nordström space-time.

Acknowledgements

I wish to acknowledge the support of the Abdus Salam ICTP, Trieste, where part of this work was done. I am also indebted to anonymous referees of General Relativity and Gravitation for valuable comments.

References

  • [1] Cohen, J.M., Mashhoon, B.: Phys. Lett. A 181, 353 (1993)
  • [2] Pringle, J.E.: Ann. Rev. Astron. Astrophys. 19, 137 (1981)
  • [3] Kato, S., Fukue, J., Mineshige, S.: Black-hole Accretion Disks, Kyoto University Press, Kyoto (1998)
  • [4] Mathisson, M.: Acta. Phys. Pol. 6, 163 (1937)
  • [5] Papapetrou, A.: Proc. Roy. Soc. Lond. A 209, 248 (1951)
  • [6] Tulczyjew, W.: Acta. Phys. Pol. 18, 393 (1959)
  • [7] Dixon, W.G.: Proc. Roy. Soc. Lond. A 314, 499 (1970)
  • [8] Tod, K.P., de Felice, F., Calvani, M.: Nuovo Cim. B 34, 365 (1976)
  • [9] Ryabushko, A.P., Bakhankov, A.A.: Gen. Rel. Grav. 19, 351 (1987)
  • [10] Svirskas, K., Pyragas, K., Lozdiené, A.: Astrophys. Space Sci. 149, 39 (1988)
  • [11] Bakhankov, A.A., Ryabushko, A.P.: Ann. Phys. (Leipzig) 501, 605 (1989)
  • [12] Bini, D., de Felice, F. Geralico, A.: Class. Quantum Grav. 21, 5427 (2004)
  • [13] Bini, D., de Felice, F., Geralico, A., Jantzen. R.T.: Class. Quantum Grav. 22, 2947 (2005)
  • [14] Plyatsko, R.: Class. Quantum Grav. 22, 1545 (2005)
  • [15] Bakhankov, A.A., Ryabushko, A.P.: Gen. Rel. Grav. 21, 447 (1989)
  • [16] Semerák, O.: Mon. Not. R. Astron. Soc. 308, 863 (1999)
  • [17] Hartl, M.D.: Phys. Rev. D 67, 024005 (2003)
  • [18] Hartl, M.D.: Phys. Rev. D 67, 104023 (2003)
  • [19] Faruque, S.B.: Phys. Lett. A 327, 95 (2004)
  • [20] Bini, D., de Felice, F., Geralico, A.: Class. Quantum Grav. 21, 5441 (2004)
  • [21] Bini, D., de Felice, F., Geralico, A., Jantzen, R.T.: Class. Quantum Grav. 23, 3287 (2006)
  • [22] Mashhoon, B., Singh. D.: Phys. Rev. D 74, 124006 (2006)
  • [23] Kyrian, K., Semerák, O.: Mon. Not. R. Astron. Soc. 382, 1922 (2007)
  • [24] Singh. D.: Phys. Rev. D 78, 104028 (2008)
  • [25] Bini, D., de Felice, F., Geralico, A.: Int. J. Mod. Phys. D 14, 1793 (2005)
  • [26] Bini, D., De Felice, F., Geralico, A., Lunari, A.: J. Phys. A 38, 1163 (2005)
  • [27] Rietdijk, R.H., van Holten, J.W.: Class. Quantum Grav. 10, 575 (1993)
  • [28] van Holten, J.W., Rietdijk, R.H., J. Geom. Phys. 11, 559 (1993)
  • [29] Gibbons, G.W., Rietdijk, R.H., van Holten, J.W.: Nucl. Phys. B 404, 42 (1993)
  • [30] Shirokov, M.F.: Gen. Rel. Grav. 4, 131 (1973)
  • [31] Fuchs, H.: Astron. Nachr. 311, 271 (1990)
  • [32] Rosa, V.M., Letelier, P.S.: Phys. Rev. D 78, 084038 (2008)
  • [33] Wu, X., Huang, T-Y., Zhang, H. Phys. Rev. D 74, 083001 (2006)
  • [34] Suzuki, S., Maeda, K.: Phys. Rev. D 55, 4848 (1997)
  • [35] Kao, J-K., Cho, H.T.: Phys. Lett. A 336, 159 (2005)
  • [36] Suzuki, S., Maeda, K.: Phys. Rev. D 58, 023005 (1998)
  • [37] Nieto J.A., Saucedo, J., Villanueva, V.M.: Phys. Lett. A 312, 175 (2003)
  • [38] Mohseni, M.: Phys. Lett. B 587, 133 (2004)
  • [39] Heydari-Fard, M., Mohseni, M., Sepangi, H.R.: Phys. Lett. B 626, 230 (2005)
  • [40] Moeller, C.: Commun. Dublin Inst. Adv. Studies A 5, 3 (1949)
  • [41] Ehlers, J., Rudolph, E.: Gen. Rel. Grav. 8, 197 (1977)
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