Orbital fingerprints of ultralight scalar fields around black holes
Ultralight scalars have been predicted in a variety of scenarios, and advocated as a possible component of dark matter. These fields can form compact regular structures known as boson stars, or—in the presence of horizons—give rise to nontrivial time-dependent scalar hair and a stationary geometry. Because these fields can be coherent over large spatial extents, their interaction with “regular” matter can lead to very peculiar effects, most notably resonances. Here we study the motion of stars in a background describing black holes surrounded by non-axially symmetric scalar field profiles. By analyzing the system in a weak-field approach, we find that the presence of a scalar field gives rise to secular effects akin to ones existing in planetary and accretion disks. Particularly, the existence of resonances between the orbiting stars and the scalar field may enable angular momentum exchange between them, providing mechanisms similar to planetary migration. Additionally, these mechanisms may allow floating orbits, which are stable radiating orbits. We also show, in the full relativistic case, that these effects also appear when there is a direct coupling between the scalar field and the stellar matter, which can arise due to the presence of a scalar core in the star or in alternative theories of gravity.
- I Introduction
- II Framework
- III Quasi-circular orbits
- IV Non-minimal effects of scalar fields on orbital motion
- V Discussion and final remarks
- A Weak-field analysis
- B Gravitational field of the scalar cloud
- C Analytical expression for the perturbation to the circular orbit at corotation
Scalar fields are ubiquitous models to describe complex phenomena, and are frequently used as effective descriptions or to capture what is thought to be the essentials of new interactions. The examples are too many to describe in any useful detail, and include models of dark matter halos Hui et al. (2016); Ureña López et al. (2017), fields assisting inflation during the early stages of the universe, or even strong-gravity effects such as scalarization in the interior of compact stars Berti et al. (2015).
Among the consequences of the existence of scalar fields are self-gravitating structures, like boson stars and oscillatons which exist when the field is complex or real, respectively. These structures have been used extensively as models for dark matter and of compact objects Kaup (1968); Ruffini and Bonazzola (1969); Jetzer (1992); Schunck and Mielke (2003); Liebling and Palenzuela (2012); Macedo et al. (2013a); Brito et al. (2016); Seidel and Suen (1991); Okawa et al. (2014a), usually requiring the scalar field to be massive (in order not to disperse to infinity), and time-dependent (in order to create enough pressure to sustain from collapsing). Massive scalar real fields around black holes (BHs) or collapsing stars can lead to very long-lived—for all purposes stationary—configurations Witek et al. (2013); Okawa et al. (2014b); Barranco et al. (2012); Sanchis-Gual et al. (2015a, b), while complex fields may form truly stationary configurations Herdeiro and Radu (2014, 2015); Hod (2012); Benone et al. (2014), also dubbed as clouds, which are kept from being absorbed by the horizon through a process known as superradiance Brito et al. (2015a). In fact, these hairy BH solutions are smoothly connected to spinning boson stars, such that they can be thought of as a spinning boson star, at the center of which a spinning BH (with carefully designed angular velocity) was placed. Notwithstanding, all of the above features can be generalize to massive vector fields instead of scalar ones Witek et al. (2013); Brito et al. (2015b, 2016); Herdeiro et al. (2016).
Structures such as boson stars or scalar-hairy BHs are usually compact, and therefore apt to emit copious amounts of gravitational waves upon collisions or other interactions, which could in turn be used as a tool to discriminate them. Among some of the smoking-gun effects for long-range scalars, it was found that
(i) BHs should have “holes” in the spin-mass plane (also known as Regge-plane), corresponding to the regions where the superradiant instability is effective Brito et al. (2015a, c); Arvanitaki et al. (2016, 2015); Brito et al. (2017a, b). Thus, observations of BHs and accurate estimates of their mass and spin could provide clear indications of the existence of light fields.
(ii) Single BHs can act as sources of monochromatic gravitational waves, potentially detectable by LIGO or LISA, either as resolved events or as a stochastic background Brito et al. (2015a, c); Arvanitaki et al. (2016, 2015); Brito et al. (2017a, b)
(iii) Stars or planets carrying scalar charge, or otherwise interacting non-minimally with it, will probe resonances in the spacetime, where energy extraction from the horizon compensates for losses through gravitational radiation: the orbiting object floats at a fixed angular velocity for large timescales Cardoso et al. (2011); Fujita and Cardoso (2016). The imprint on gravitational waves may be detectable Yunes et al. (2012).
In addition, possible signs of scalar fields might be imprinted in the way that they affect the bending of light, i.e., in their shadows Vincent et al. (2016a); Cunha et al. (2015); Vincent et al. (2016b) or in ray reflection spectrum from surrounding accretion disks Zhou et al. (2017). Finally, any kind of perturbation around compact objects is likely to excite proper oscillation modes (the quasinormal modes), which can also be used to test the nature of the object Cardoso and Gualtieri (2016). This program however requires detailed knowledge of the response of the scalar field structure to external perturbations, which is still lacking.
Intuitively, it is expected that a spinning BH onto which a scalar field is “fastened” will drag the scalar field, and neighboring matter as well. In other words, there should be correlations between the characteristics of the scalar field and the behavior of stars and planets in its immediate neighborhood. We shall look for these correlations in Extreme-Mass-Ratio-Inspirals (EMRIs)—binary systems composed of a central Super Massive Black Hole (SMBH) orbited by a much lighter object (a white dwarf, neutron star or solar mass BH)—which constitute one of the most promising sources of gravitational radiation to be analyzed by upcoming facilities Amaro-Seoane et al. (2007); Gair et al. (2013); Audley et al. (2017). By considering that the SMBH supports a non-axially symmetric scalar field configuration, we explore the gravitational effects that the presence of the scalar field imposes on the motion of the orbiting body. We argue that the angular momentum imparted in the orbiting body by the scalar field may balance the angular momentum lost by gravitational radiation, given an additional mechanism to enable floating orbits Press and Teukolsky (1972); Cardoso et al. (2011). In addition, we also take into account more speculative channels of interaction between the orbiting body and the scalar field, namely the possibility of it having a scalar charge or of being acted by friction forces. The final aim of the study we initiate here is to fully understand the theoretical aspects of the dynamics of EMRIs in order to use them as probes to the existence of long-lived scalar field configurations surrounding SMBH.
In what follows we focus on an EMRI in which the SMBH supports an ultralight scalar field—we shall abbreviate it to Black Hole-Scalar Field system (BHSFS). We study the impact of the scalar field on the orbital structure of the orbiting body with special emphasis on circular orbits. Our main findings are:
General orbits of the EMRI precess at a rate that depends on the parameters governing the scalar field. This effect adds to the precession caused by general relativistic terms and, therefore, could be probed by measuring carefully any additional amount in rates of precession of satellites;
The existence of the scalar field configuration around the BH gives rise to resonant orbits when its rotation frequency is equal to one of the characteristic frequencies of the system; there are three resonances:
One corotation resonance where, in the absence of other perturbing effects, large numbers of orbiting bodies (such as stars) will tend to pile up at the resonant radius;
Two Lindblad (inner and outer) resonances where, at first order, the scalar field can exchange angular momentum with the orbiting particle, an effect which is associated with orbital migration.
The BHSFS system is introduced with detail in Sec. II, where we discuss the weak field limit and the parameters used in the description of the system. We analyze the stellar orbits around the BHSFS in Sec. III. We also discuss the possibility of adding a non-minimal coupling and friction forces to the system in Sec. IV. Finally, Sec. V fixes an exploratory route for the possibility of using systems of this sort to develop the understanding of the potential influence of scalar structures in astrophysical systems. We shall use, unless stated otherwise, natural units ().
ii.1 The black hole-scalar field system
We are interested in a massive scalar minimally coupled to gravity, and described by the action
We focus on massive, non self-interacting fields. The mass of the boson under consideration is related to the mass parameter above through , and the theory is controlled by the dimensionless coupling
of a massive scalar field on a curved background given by the metric .
We will focus on real scalar from now onwards 111Complex scalars admit solutions where the metric is axisymmetric Herdeiro and Radu (2014, 2015), hence most of our results do not apply to complex fields. However, most of our results do generalize should matter couple non-minimally to the scalar, for example if one considers matter which is charged under the scalar. See Sec. IV.. It can be shown that real scalars on a Kerr background admit nearly-stationary profiles. To a good approximation, which we will take for granted here, the scalar field is described by Brito et al. (2015a, c)
In principle, from the linear analysis of the problem, the amplitude in Eq. (3) can not be constrained. However, the amplitude of the scalar cloud is not arbitrary. We note that it should be set such that it obeys the nonlinear solutions of the Einstein-Klein-Gordon system. In general, we can express it in terms of the scalar field cloud total energy-mass Brito et al. (2015c). For a cloud with and , we have . We take this as our reference value.
In the limit , the maximum value of the radial profile is attained at given by (cf. discussion around Eq. (7) in Ref. Brito et al. (2015c))
This value can be used as a measure of the size of the scalar “cloud”. This region is far from the BH, meaning that the curvature of spacetime is low and it is valid an analysis of the scalar field using a flat background metric Yoshino and Kodama (2014). Accordingly, we expect that in this limit one can summarize the gravitational effects by a Newtonian gravitational potential given by a Keplerian potential
due to the BH, plus a small distortion
sourced by the scalar field in Eq. (3).
The gravitational potential is one of the effects that can be distilled after a linear analysis of Einstein’s field equations (see Appendix A). To isolate the gravitational potential, one assumes that far from the BH, the metric is given by222Other works have employed this choice of metric - see Refs. Khmelnitsky and Rubakov (2014); Blas et al. (2016).
where is other scalar potential which is irrelevant for non-relativistic dynamics (more details in Appendix A). The stress energy tensor for the scalar field is given by333Notice that the background metric is flat, as mentioned before in the text.
and upon substitution in the Einstein’s equation, the dominant contribution yields, in the non-relativistic regime of Appendix A,
where , and are components of the stress energy tensor defined in Appendix A. We solve Eq. (11) in Appendix B and we obtain that the total gravitational potential due to the presence of the BH and the scalar field is given by
where (see Appendix B for all the details)
In the equatorial plane, , the potential is given by
where are inertial polar coordinates in the plane and the functions and are defined in the aforementioned appendix. A schematic representation of the scalar field profile is shown in Fig. 1. We shall also see that a similar subsides when the orbiting object has a non-minimal coupling with the scalar cloud, leading, however, to different quantitative results.
The above potential has two distinctive features. First, it has a radial dependence, which can modify the structure of bound orbits of the background field, for instance changing Kepler’s law444The new potential will not be proportional to and therefore, according to Bertrand’s theorem Bertrand (1873), not all bound orbits will be closed.. Second, it has a periodic angular dependence on and , breaking the axial symmetry of the gravitational potential. This second feature also appears in planetary motion around disks and galactic formation, and therefore can enrich the kinematics of particles around BHs. For convenience, we will organize the potential in Eq. (12) specialised to the equatorial plane as
making an explicit separation between the angular and non-angular dependent components.
ii.2 Validity of the approximation for the orbital motion
In the spirit of Ref. Macedo et al. (2013b), we will be using Newtonian mechanics to study the motion of a body orbiting a BH supporting a scalar field. Before doing that, we start by comparing the effective radial potential created by a Keplerian potential with the equivalent coming from a Schwarzschild BH555Although the BH that supports the scalar field is rotating, analyzing the non-rotating case is enough because in the limits we are considering the BH rotation is irrelevant.. This approach is supposed to provide an approximate measure of the validity region of the Newtonian approximation.
In the Newtonian approximation, the effective radial potential governing the motion (through ) of a particle orbiting a mass is given by,
Here are the energy and angular momentum per unit rest mass. A counterpart in the relativistic case is hard to define. We will define the analog radial potential in the Schwarzschild case by a straightforward extension using geodesics Cardoso et al. (2009), taking dots to have the same meaning as in flat spacetime and to be the radial coordinate. One finds
To estimate the error of neglecting relativistic effects, we look at the magnitude of the relativistic corrections with respect to the Newtonian potential. Focusing on circular orbits of radius , whose specific angular momentum is given by , the deviation from the relativistic orbit is given by
where is the mass of the central object. In Fig. 2 we plot the ratio of the relativistic correction to the total energy of the classical circular orbit and from there we can see that the relativistic correction for the potential is less than of the total energy for orbits with radii larger than . On the other hand, as we pointed out the scalar is exponentially suppressed at distances . Thus, at very large distances, the relativistic correction dominates. Our results will therefore be valid only for orbiting objects at distances smaller than .
Moreover, in order to treat the scalar field as a perturbation, the magnitude of its gravitational potential must be perturbatively smaller than the magnitude of the potential created by the central BH. In Figure 2, we also plot the relative magnitude of the radial part of the scalar field potential with respect to the BH potential for different values of the mass coupling. It is sufficient to consider the radial part since the angular part is even smaller. For those particular values of mass couplings, the scalar field potential is less than of the BH potential. Thus, the gravitational potential due to the scalar field can indeed be treated as a perturbation to the Keplerian potential sourced by the BH.
Iii Quasi-circular orbits
To estimate the impact of the presence of the scalar field on the dynamics of the EMRI, we will quantify the modifications it causes on circular orbits. These orbits are the simplest type of orbits in a standard EMRI and understanding how they change in response to the scalar field is a first step towards understanding how the global structure of the EMRI is modified.
iii.1 General treatment
Under our assumptions, the study of the orbital behavior of a stellar object in the EMRI reduces to the analysis of the Lagrangian
which describes its motion under the influence of the potential of equation (16) in a system of coordinates that is corotating with the scalar field. In regions where , one can obtain some insight into this system by exploring the effect of the azimuthal-dependent part on the stable circular orbits of the Keplerian potential . The perturbative approach is set up by considering the evolution of small deviations and to the radial and angular behavior of a stable circular orbit of radius
where with and, for convenience, we fix the initial condition to be . Neglecting second order terms in and , the equations of motion in the corotating frame are written as
in which all derivatives are evaluated at . To study equations (23) and (24) we consider the additional approximation , i.e., , meaning that we consider the perturbation so small that the angular velocity of the orbit being perturbed dominates. The equations are then written as
whose general solution is given by
where all the quantities are calculated at and are the initial conditions for the radial motion. This kind of solution is long known in problems with non-axisymmetric potentials (see, e.g., Refs. Berman and Mark (1977, 1979); Contopoulos (1973, 1978); Binney and Tremaine (2011)). We can readily see the presence of some singularities in Eqs. (28), (30) and (34). Two of the singularities appear when
These are called Lindblad (inner and outer) resonances. The other singularity, given by
is called co-rotating resonance, because the perturbation is being made to a circular orbit which is synchronized with the potential (in this case with the scalar cloud). When a resonant frequency is approached, the above linear analysis breaks down. We shall look into these particular orbits in the following sections. The radii at which the outer (inner) Lindblack resonance occurs will be termed outer (inner) Lindblad radius . The radius at which the co-rotating resonance occurs is the co-rotation radius .
iii.1.1 Circular orbits
Aside from giving rise to resonant orbits, the angular part of the scalar field potential plays no other role in the dynamics of the system due to its small value (recall that the amplitude of the angular part of the potential is smaller than the radial part). Indeed, the other effects of the presence of the scalar field are an exclusive consequence of the radial part of its gravitational potential. To further explore its effects, we ignore the presence of the -dependent part of the potential in the Eqs. (25) and (26), which means that the angular momentum is exactly conserved, and the solution in given by Eqs. (28) to (31) with and . As in the analysis with the angular part of the potential, the behavior of the perturbations indicates that the circular stable orbits of the BHSFS are not exactly Kleperian. We start with initial conditions at , and initial radius such that the orbit would be circular – for the same central mass – if the scalar cloud did not exist. We find a solution that deviates from the Keplerian circular orbit. This, of course, is expected: given a value of the angular momentum, the corresponding value of the radius of the circular orbit of the total radial potential is different from the radius of the circular orbits of . Quantifying this radial difference is a way of looking into the influence of the scalar field on the orbital structure around the SMBH. We will indicate the radii of the circular orbits of the total potential by ; their values are given, for fixed angular momentum , by
where the derivative is taken at . The stability of these orbits is guaranteed as long as
This inequality is always verified in the range of the mass coupling parameter we are considering, thus all circular orbits of the potential are stable. Notice, however, that the amplitude of the scalar field can be larger—for instance in non-minimal coupling scenarios. Parametrizing the amplitude of the scalar field as
where is the standard amplitude of the scalar field (see Sec. II.1), we observe that for , unstable orbits appear. More precisely, for all circular orbits are stable and for a window of unstable circular orbits with exists. This is shown in Fig. 3, where it is represented the quantity described in Eq. (38). Furthermore, it is also observed that after crossing the boundary imposed by , the range increases with .
For small values of the angular momentum and mass coupling parameter, the difference between the radius of Keplerian circular orbits, , and the radius of circular orbits of the BHSFS, , is negligible666We keep the angular momentum fixed. This observation shows that close to the SMBH Keplerian circular orbits are good approximations for the circular orbits of the whole system. This reinforces the validity of the results we obtained for the location of the resonant orbits.; however, this difference has a non-trivial evolution once we start to vary those parameters; this can be appreciated in Fig. 4. As the angular momentum increases, the difference between the radii has a behavior which is controlled by the value of the mass coupling parameter: large values of imply a large radii difference for a fixed value of the angular momentum. Notwithstanding, the difference in radii at large distances is due to the fact that now the orbiting particle sees a different effective mass (central object plus the scalar field surrounding it, see Fig. 5). In Fig. 4 we also see that, for each value of the mass coupling parameter, there is a value of the angular momentum for which the radii of the stable circular orbits is equal for both potentials; the corresponding value was numerically determined to be
This value represents the location where the scalar cloud typically peaks Brito et al. (2015c).
Another way of looking at the difference between the circular orbits of an isolated BH and a scalar-surrounded one is to observe that close to the SMBH a potential is dominant, while far from the SMBH the dynamics are dominated by in which is an effective mass value, in units of the mass of the SMBH. It was numerically found that our system has , as can be seen in Fig. 5. This number can be interpreted by looking at Eq. (37) in the form
and observing that for large values of angular momentum and radius it can be written as
where the amplitude of the scalar field was again written as . Using the value for prescribed in Sec. II.1 we obtain
which is close to the value obtained numerically777Recall that the circular orbit of a Keplerian potential with angular momentum has a radius given by .. We see, then, that far from the SMBH the potential governing the dynamics is still Keplerian, but the mass sourcing it is not the SMBH mass. This “effective” mass corresponds to the mass of the SMBH plus the total mass contained the scalar field.
iii.1.2 Rate of precession
Another expected feature of the potential generated by the presence of the scalar field is the precession of the orbits. The apsidal angle of a quasi-circular orbit obtained from a perturbation of a circular orbit of radius is
From this expression, we obtain that in each cycle around the SMBH, the orbit precesses at a rate radians. In this particular case,
where is given by Eq. (33). The dependence of this precession rate on the mass coupling parameter and on the radius of the corresponding orbit is represented in Fig. 6. Two features are instantly noticed: a) the precession rate changes sign, indicating that orbits can precess both clock- and counter-clock wise, and b) there is a maximum and a minimum value of the precession rate that is independent of the mass coupling parameter of the system, indicating that it must be an intrinsic characteristic of the model – it is the distance from the BH at which these extrema occur that depend on the mass coupling parameter. The precession rate changes sign twice: the first time being from a region of positive precession rate to a region of negative precession rate (top-right panel of Fig. 6), the second time being from a region where the precession rate is negative to a region in which the precession rate is positive (bottom panel of Fig. 6). As one moves farther from the SMBH the precession rate stabilizes to zero, meaning that a Keplerian potential is dominating the dynamics888This is confirmed by the results of Fig. 5.. The existence of these localized regions of positive and negative precession rate, each of them with well defined maximum and minimum values offer a good source of phenomenology that may allow for a characterization of the system. We found numerically that both zeros are related with the mass coupling parameter as
iii.2 Resonant orbits
For the rest of this section, we will go back to Eqs. (28) and (29), focusing on the resonant orbits. For a particle near the resonant orbits, the general perturbative approach presented in those equations is not adequate since it gives unphysical behavior for the perturbations999The complete understanding of this problem is out of the scope of our work. More details can be found in Refs. Arnol’d (1963); Henrard (2005).. Our main motivation to pursue a more detailed analysis of these orbits is their important role in the so called angular momentum transfer mechanisms in the context of galactic dynamics Goldreich and Tremaine (1980, 1979); Lynden-Bell and Kalnajs (1972); we suspect that most—if not all—of those results can be generalized to the context of BHs and scalar fields (bearing in mind, naturally, the different lengthscales). In other words, it is possible that BHs anchoring scalar fields may give rise to galactic-like structure on lengthscales of a few hundred Schwarzschild radii.
The radii of the circular orbits that correspond to the resonant frequencies are obtained by substituting the expressions for the angular frequency and the epicyclic frequency in the equations defining the resonances and solving for the radial coordinate. By doing this, one can immediately see that the smallest of the three resonant radii is the one that corresponds to the inner Lindblad frequency. In order to guarantee that Newtonian mechanics can be used to study the inner Lindblad resonant orbit, its radius should be , see Fig. 2. This scale can be controlled by the mass coupling given that the scalar field rotates with angular frequency ; taking this into account, the inner Lindblad radius is given by
from which one can estimate the maximum value of such that a Newtonian analysis is justified. This is shown in Fig. 7. Once the inner Lindblad radius is sufficiently far from the central BH such that Newtonian mechanics is valid, then the other two resonances (corotation and outer Lindblad resonance) are automatically ensured to be within the same regime. The corotation and outer Lindblad radii are, respectively,
The analytical solutions we shall be presenting for the quasi circular resonant orbits follow from the same assumptions made for the general quasi-circular orbits, i.e., the perturbations and will be considered small. To do this, we take the equations of motion for the perturbations and analyze them separately for each of the three resonant frequencies mentioned previously.
iii.2.1 Lindblad Resonances
which under the same reasoning applied before will allow us to write
The differences between the equations for the inner and the outer Lindblad orbits are the numerical value of the epicyclic frequency, the sign in the equation of motion for (see Eq. (55)) and the functions . The previous equation has a direct analytic solution given by
where and depend on the initial conditions as
Using this expression for the evolution of in
one can derive the expression for .
The solutions for and at Lindblad resonances show a different behavior from the general case (28) and (29), with the radial perturbation growing significantly even when the orbiting body is initially placed in a circular orbit, i.e., when . Note that we chose initial conditions to correspond to a circular orbit in the absence of a scalar cloud. Because of the term proportional to the time parameter in Eq. (III.2.1), the radial perturbation increases at each period of oscillation – see Fig. 8. This behavior results from the fact that up to first order, the perturbation is described by the equation of motion for a harmonic oscillator (with natural frequency given by ) being excited by a harmonic force with the same frequency. This is a classical example of resonance.
While the first order approximation holds, the value of the radial perturbation increases as seen in Fig. 9. Once this approximation stops being valid, which eventually happens if enough time passes, the higher order components of the equations of motion describing and become important and the evolution of the radial perturbation is no longer described by Eq. (III.2.1); the higher order terms force to decrease, as can be seen in Fig. 9, ending up describing a beating pattern. The time that it takes for a complete beat, both at inner and outer Lindblad resonances, depends on the mass coupling parameter and on the amplitude of Eq. (39); we numerically compute this dependence, finding a good fit to be
iii.2.2 Corotation Resonance
Going back to the equation of motion (23) and (24), considering that the circular orbit has a radius given by the corotation radius we see that the zeroth order term vanishes identically and (see equation (22))
Thus, what sets corotation apart from the general orbits and Lindblad orbits is the fact that besides the initial condition of the radial perturbation, also the initial angle is important for the motion, as can be seen in the corotation equations of motion
where the coefficients are computed at the corotation radius. To write these equations, we considered that the angular perturbation is small enough to allow for the expansion of the corresponding sinusoidal functions up to first order. Moreover, we observed that in order for the analytical solution to be valid, the initial condition has to be of the same order as 101010The approach presented here focuses on motions around the point , a stable Lagrangian point. For an alternative approach to the study of the motion at corotation, see Section 3.3 of Ref. Binney and Tremaine (2011).. After all these cautionary remarks, one can advance to the solution of the equation of motion; the method used previously to obtain the expressions describing the motion of the orbiting body is not adequate in this case. One has to employ a more evolved method, described in Appendix C, which in general gives a solution of the form
where depends only on the parameters of the problem—both the scalar field and the mass of the SMBH—and depends on the parameters of the problem and the initial conditions. Comparison with the numerical calculations (see Table 1) shows good agreement with the analytical solutions for an arbitrary range of the time parameter. In general, one of the sinusoidal functions in the solution for and dominates over the other leading to the so called banana orbits Contopoulos and Grosbøl (1989) which can be appreciated in Fig. 10. The width of the banana orbits, which is related to the maximum value attained by the radial perturbation , is dependent on the amplitude of the scalar field but also on the initial angle. The extent of the banana orbit, i.e., the angular range it covers, depends only on the initial conditions of the problem, particularly on the initial angle. Hence, no matter how thin it is, a banana orbit will always be found close to a stable Lagrangian point as a result of an initial angle . On the other hand, the time it takes for an orbiting body to describe a complete banana orbit does not depend on the initial angle, being determined by the mass coupling parameter as
meaning that banana orbits take less time to appear for higher mass couplings111111This timescale is much smaller than the instability time scale of the scalar field we are considering, which is given by Brito et al. (2015c)..
If the initial angle is precisely at then the resulting orbit is not a banana orbit. This particular initial angle corresponds to an unstable Lagrangian point (see Appendix C) and a particle that starts there will cover the whole angular range. For initial angles bigger than , the banana orbits are recovered, but in this case they will be centered around the stable Lagrangian point .
As this discussion illustrates, one sees that the position of the Lagrangian points determines the shape of corotation orbits. Most notably, the proximity to a given Lagrangian point determines the way the orbiting body reacts to a perturbation: a particle at an unstable Lagrangian point will spend some time at that point, which depends on the mass coupling parameter as
and then it will rapidly move to the other unstable Lagrangian point. On the other hand, a particle at a stable Lagrangian point stays there indefinitely or, in case of a perturbation, librates around it - it is this libration that gives rise to banana orbits.
The libration around stable Lagrangian points may induce an accumulation of orbiting bodies in the surrounding regions. In fact, perturbations to a body sitting exactly at a stable Lagrangian point will force it to librate around it, as shown in Fig. 11, and find itself trapped. A similar effect was obtained in N-body calculations in a galactic setting Ceverino and Klypin (2007) and constitutes a fingerprint of a gravitational potential of the form given in Eq. (15) – structures resembling this trapping mechanism close to BHs may be a smoking gun for this dark matter model based on an ultralight scalar field of this sort.
iii.3 Orbital torque
The fact that the perturbing gravitational potential imposed by the presence of the scalar field has an angular component means that the angular momentum is not exactly conserved (cf. Eq. (24)). The angular momentum of the orbiting body initialized in a circular orbit of radius is given by
and the the torque responsible for this is, up to first order, given by
To get an idea of the magnitude of this effect, we calculate the average value of this quantity over a revolution around the central BH
for the general case,
for the corotation case and
for the inner and outer Lindblad case. The average values are
for the general case,
for the inner (minus sign) and outer (plus sign) Lindblad resonances, where we used , and
for the corotation case, where we considered .
The change in the angular momentum of a particle over a complete orbit around the BH is considerable only when the particle is orbiting at a resonant orbit. Particularly, since the function is overall negative, we see that at the inner Lindblad resonance there is an increase in the angular momentum while at the outer Lindblad resonance there is a decrease. At the corotation resonance the angular momentum transfer depends structurally on the initial angle : explicitly, as argument of sinusoidal functions, and implicitly, affecting the values of the constants and (cf. Appendix C). The latter fact can be seen by calculating the change in the angular momentum of a particle in a stable Lagrangian point or ; if one would care to go though the calculations one would find that .
In any case, in the mass coupling limit we are considering the angular momentum changes only slightly. Be that as it may, the transfer of angular momentum from the scalar cloud can play an important role on the dynamical evolution of the EMRI in more extreme regimes. In the following we will cover some instances in which similar mechanisms are essential for the dynamics of the systems in which they are inserted.
iii.3.1 Comparison with known phenomena and floating orbits
In planetary dynamics, particularly in interactions between planetary rings and satellites, angular momentum can be transferred between the disk and the orbiting object Goldreich and Tremaine (1980, 1979); Lynden-Bell and Kalnajs (1972). This exchange of angular momentum is most effective at the resonances, both corotation and (inner and outer) Lindblad. Angular momentum is removed from the disk when the satellite is at the innermost Lindblad resonance and added to the disk when the satellite is at the outermost Lindblad resonance. Angular momentum is also exchanged at the corotation resonance, in which the rate depends on the gradient of the vorticity per unity of surface density. In general, a disk with background (surface) density has a angular momentum flux induced by the satellite of (dipolar case)
where the quantity in the brackets are computed at the inner or outer Lindblad resonances, , is the gravitational potential generated by the satellite and depends essentially on satellite quantities (see Ref. Goldreich and Tremaine (1980) for details). At the corotation resonances, the angular momentum flux is given by
where is the Oort’s parameter. Expressions (75) and (76) are derived assuming a fluid description for the disk as well as some physical reasonable assumptions for the propagation of the fluid perturbations in the disk.
Although we cannot directly map the system above into the BHSFS, many of its features must be common to the latter. In order to translate the above picture for the BHSFS one has to solve the perturbation equations of the Einstein-Klein-Gordon system around a hairy BH induced by an orbiting particle. In general, similarly to the disk-satellite interaction Goldreich and Tremaine (1979), there will be modes that are trapped (due to the mass of the scalar field, for instance) and modes that propagate angular momentum and energy away from the system. Since in many scenarios scalar field configurations can be mapped into effective fluid descriptions (see Ref. Boonserm et al. (2015) for instance), one may expect that equations similar to Eqs. (75) and (76) can be obtained from the equations governing the perturbations of stars orbiting hairy BHs. Additional mechanisms, such as superradiant instability, may also be important, depending on the frequency of the orbiting stellar object. The description of perturbations of hairy BHs with scalar field is still an open subject; to improve it one must go beyond weak field approximations—the perturbations experience strong field regions and appropriate boundary conditions have to be set at the event horizon. Therefore, and though the full description is beyond the scope of this paper, we conjecture that orbital resonances may play an important role in the angular momentum transfer between the scalar field and the orbiting objects in such systems.
The exchange of angular momentum between the stellar object and the scalar field halo can also lead to floating orbits, depending on the configuration of the system. Let us, firstly, note that the EMRI binary formed by a BHSFS and a stellar object incidentally loses angular momentum due to the gravitational radiation emitted. For non-relativistic orbits, the energy and angular momentum flux can be approximated using the quadrupole formalism Maggiore (2008). Therefore, the angular momentum flux due to a stellar object in a circular orbit at radius is given by 121212Gravitational wave emission tends to circularize orbits, and therefore it is sufficient for us to consider only circular orbits here.
where is the total mass of the configuration and is the reduced mass. Because the system is losing angular momentum through gravitational waves, the orbit tends to decrease in radius. However, according to the reasoning exposed above, when the system is at the resonances additional angular momentum can be provided to the star [see Eqs. (75) and (76)]. If the angular momentum provided is sufficient to compensate the lost by gravitational waves, the net result is zero and the orbiting object remain with the same angular momentum, even though the system as a whole radiates. This characterizes essentially a floating orbit Misner (1972); Press and Teukolsky (1972); Cardoso et al. (2011); Fujita and Cardoso (2016). Note that differently to what happens in the standard picture—where the energy is provided by the BH’s rotational energy—the energy in the BHSFS is provided by the scalar field. It would be interesting to see whether the order of magnitude between (75) and (77) are the same, which favors the above picture. Nevertheless, to achieve such picture, the BHSFS should have the exact configuration such that (75) equals (77), which in turns depends on the perturbations of the BHSFS.
Iv Non-minimal effects of scalar fields on orbital motion
The stellar object orbiting the BHSFS may be subject to other forces besides the standard gravitational one. Here we comment on the possibility of having an additional scalar force, assuming that the stellar matter has a non-minimal coupling with the scalar field. Moreover, we comment on the effects of the dynamical friction and accretion, using a fluid approximation to describe it.
iv.1 Scalar force
Assuming that the stellar matter is non-minimally coupled with a scalar field, we have that there will be an extra force, which shall depend on the coupling between the scalar field and the stellar matter. A simple way to test the implications of such force, is to assume that the interaction action is such that the motion of the star is described by Poisson et al. (2011); Burko et al. (2002); Warburton and Barack (2010)
where is the (background) scalar field and measures the strength of the interaction. When , the particle follows a geodesic motion. Such kind of coupling may arise in different contexts, such as dimensional reduction or a frame transformation in the action. Using the above action, we find the following equation of motion
where represents the worldline of the particle. We shall use the above setup to determine the features of a force due to a background scalar field. This setup may suit the description of stellar-size objects through clouds surrounding BHs Benone et al. (2014); Herdeiro and Radu (2014, 2015), through dark matter mini-spikes Eda et al. (2013, 2015) or even through compact exotic objects formed by scalar field, such as boson stars Schunck and Mielke (2003); Macedo et al. (2013a, b). Note that the above picture is fully relativistic.
Let us begin, for simplicity, neglecting the gravitational interactions between the scalar field and the star. Therefore, the star will feel the BH spacetime and the additional scalar force will be weighted by the coupling parameter . Assuming a dependence of the field as , and considering a small limit, all quantities can be expanded around the geodesic quantities, just as seen in previously in Sec. III. In this case, considering that at zeroth order the particle is at a circular orbit and that the corrections are small, we have that the motion can be described as
where and are constants obtained from solving the zeroth order problem, and we have chosen that the motion initially starts at and . Using this solution, the equations for , , and and are given by