# Scattering by regular black holes: Planar massless scalar waves impinging upon a Bardeen black hole

###### Abstract

Singularities are common features of general relativity black holes. However, within general relativity, one can construct black holes that present no singularities. These regular black hole solutions can be achieved by, for instance, relaxing one of the energy conditions on the stress-energy tensor sourcing the black hole. Some regular black hole solutions were found in the context of nonlinear electrodynamics, the Bardeen black hole being the first one proposed. In this paper, we consider a planar massless scalar wave scattered by a Bardeen black hole. We compare the scattering cross section computed using a partial-wave description with the classical geodesic scattering of a stream of null geodesics, as well as with the semiclassical glory approximation. We obtain that, for some values of the corresponding black hole charge, the scattering cross section of a Bardeen black hole has a similar interference pattern to a Reissner-Nordström black hole.

###### pacs:

04.70.-s, 04.70.Bw, 11.80.-m, 04.30.Nk## I Introduction

Black holes (BHs) are among the most interesting objects of general relativity (GR). Although GR is a highly nonlinear theory, BHs come out of it with a very simple structure. Standard GR BH solutions are parameterized by their mass, charge and angular momentum Heusler (1998) (see, e.g., Refs. Herdeiro and Radu (2014); Benone et al. (2014) for interesting counterexamples of the previous statement). Although related to the earliest predictions of GR, the strong field regime of BHs is still an experimental challenge Psaltis (2008); Will (2006); Berti et al. (2015). Notwithstanding, the observational data presently available suggest that BHs populate basically all the galaxies in the Universe Narayan (2005).

Although very successful in explaining the available data, standard GR BHs suffer from one of the main problems of GR: the presence of singularities. Hawking and Penrose indeed showed that, for some hypotheses on the gravitational collapse, the formation of singularities in BHs would be unavoidable Penrose (1965); Hawking and Ellis (1973). These singularities were conjectured by Penrose to be hidden by a horizon Penrose (1969); Wald (1997), and were claimed to be possibly avoided within an improved theory of gravity (extension or modification of GR) Clifton et al. (2012).

The study of BHs without singularities can help us to understand the role played by singularities in astrophysics. Still within GR, one can obtain BHs without singularities — dubbed regular BHs — by relaxing one of the energy conditions on the stress-energy tensor. Bardeen proposed the first regular BH solution Bardeen (1968), which was later identified as a solution for a nonlinear magnetic monopole Ayon-Beato and Garcia (2000). Since then, other regular BHs appeared in the literature, in different scenarios (see, e.g., Refs. Ansoldi (2008); Lemos and Zanchin (2011); Flachi and Lemos (2013), and references therein). Moreover, regular BHs can be relevant in the context of quantum gravity Hayward (2006); De Lorenzo et al. (2015), and some of them reproduce the quantum weak field regime of GR Bjerrum-Bohr et al. (2003).

Studies of scattering by BHs have been extensively made Futterman et al. (1988). Reference Crispino et al. (2009a) presented the results of the scattering of all basic massless (spin 0, 1/2, 1 and 2) fields by Schwarzschild BHs. Moreover, the shadows of BHs Falcke et al. (2000); Huang et al. (2007) may become visible with future telescopes, like the Event Horizon Telescope eve (), and the scattering of light, considering wave and semiclassical approximations, may be important in anticipating subtle characteristics of the shadows. However, a careful study of the scattering of fields by regular BHs is still lacking in the literature ^{1}^{1}1An approximation scheme to compute the scattering cross section of regular BHs was performed in Ref. Huang et al. (2014). The scheme relies on the Wentzel-Kramers-Brillouin (WKB) approximation, using a modification of the effective potential (13), leading to inaccurate results (see, e.g., Ref. Macedo and Crispino (2014))..

The line element of the Bardeen BH can be written as

(1) |

where the lapse function is given by

(2) |

The Bardeen BH has a structure similar to the Reissner-Nordström (RN) BH (see, e.g., Ref. Ansoldi (2008)). For (henceforth, without loss of generality, we shall assume ) the spacetime has two horizons and for the horizons degenerate, characterizing the extremal case. Following Ref. Macedo and Crispino (2014), we shall display our results in terms of the normalized charge ^{2}^{2}2The parameter presented here as can also be interpreted as a natural length when one considers that the Bardeen BH comes from a quantum generalization of GR. See, for instance, Ref. De Lorenzo et al. (2015) for more details..

It is interesting to note that the variation of the charge of the regular BH changes considerably the deflection angle of light rays Zhou et al. (2012). In Fig. 1 we plot null geodesics coming from infinity with an impact parameter of , for different values of the BH charge. The behavior is qualitatively similar to the case of RN BHs Crispino et al. (2009b). We see that, adjusting the BH charge, we can have scattering in basically any direction.

The remainder of this paper is organized as follows: In Sec. II we review the main aspects of the classical geodesic scattering and semiclassical glory approximation to compute the differential scattering cross section. In Sec. III we present the partial-wave method used to compute the scattering cross section of planar massless scalar waves. In Sec. IV we present the results for the scattering of planar massless scalar waves impinging upon a Bardeen regular BH, comparing the three different approaches used to compute the scattering cross section. In Sec. V we end up with our final remarks. Throughout this work we use and metric signature .

## Ii Classical scattering and semiclassical glory

In this section we investigate the scattering by BHs by using two approaches: classical geodesic scattering and the semiclassical glory approximation. These approaches allow us to foresee some of the aspects of the scattering cross section obtained within the full partial-wave analysis.

### ii.1 Geodesic scattering

The analysis of null geodesics in the Bardeen spacetime can be seen in Ref. Macedo and Crispino (2014). For the classical approximation of the scattering we may consider a stream of parallel null geodesics coming from infinity. In this case, the analysis of Ref. Collins et al. (1973) suits the problem of classical scattering by Bardeen BHs. The classical scattering cross section is given by

(3) |

where is the impact parameter associated with a scattering angle . The summation in Eq. (3) is such that we also consider the case in which the null geodesic rotates (one or many times) around the BH before going to infinity (for instance, see the solid curve of Fig. 1). It is interesting to note that the classical scattering formula given by Eq. (3) describes very well the planar-wave case for small scattering angles, although it gives discrepant results for moderate-to-high scattering angles, as we shall see in Sec. IV.

Let us now obtain through a geodesic analysis. Without loss of generality, we shall restrict the geodesic motion to the plane . From the line element (1), we can write, for null geodesics

(4) |

where we have defined , is the impact parameter given in terms of the constants of motion

(5) |

and the overdot denotes differentiation with respect to an affine parameter of the curve.

Differentiating Eq. (4) with respect to , we obtain

(6) |

Solving Eq. (6) with the appropriate boundary conditions, one can obtain the geodesics followed by massless particles, such as the ones shown in Fig. 1. The smallest positive root of the right-hand side of Eq. (6) corresponds to the radius of the critical orbit for null geodesics, . Substituting its value in the right-hand side of Eq. (4) and setting it to zero, we obtain the impact parameter associated with the critical orbits, . Going in the other way around, i.e., choosing a value , the smallest root of the right-hand side of Eq. (4) is , where is the turning point — or the radius of maximum approximation — of the geodesic.

Finally, by integrating Eq. (4) in the case of scattered geodesics, we obtain

(7) |

The deflection angle following directly from Eq. (7) is given by

(8) |

By inverting Eq. (8), one obtains , and substituting it in Eq. (3), one obtains the classical scattering cross section. Plots of the classical scattering cross section obtained by Eq. (3) are exhibited in Fig. 2, where we compare the Bardeen cases with the Schwarzschild one. We see from Fig. 2 that the increase of the BH charge contributes to an increase of the BH classical scattering cross section.

### ii.2 Glory scattering

The interference that occurs between scattered partial waves with different angular momenta is not taken into account by the classical formula (3). In order to obtain a scattering cross section that takes into account the interference processes, we need to perform a wave analysis of the problem. Before going into the full wave analysis, however, it is interesting to apply an approximate method that works remarkably well for high scattering angles () and that captures some key features of the scattering cross section in this regime, including the interference process: the semiclassical glory approximation Matzner et al. (1985). Indeed, one of the main advantages of this semiclassical approximation is that one can find an analytical formula that gives some physical insight for the width of interference fringes in the scattering cross section as well as the intensity of the scattered flux for . As a semiclassical approximation, it is valid for , although it can still reproduce remarkably well some results for .

The semiclassical formula for the glory scattering by spherically symmetric BHs is given by Matzner et al. (1985)

(9) |

where is the impact parameter of backscattered rays (), is the Bessel function of the first kind (of order ), and is the wave spin. In our case, since we are considering a scalar wave, . We note that there are multiple values of corresponding to the multiple values of the deflection angle, namely , with , that result on back-scattered rays. All the rays scattered close to the the backward direction () contribute to the glory scattering, but the most important contribution comes from the case. The next contribution, , has an intensity that is about 0.2 % of the one in the Schwarzschild case, and about 0.8 % in the case of the extreme Bardeen BH. This is a consequence of the derivative in Eq. (9) getting rapidly suppressed as increases. In fact, the values of for rays that pass multiple times around the BH are very close to each other and also to . Here, we consider only the most important contribution to the glory scattering.

Once we have the knowledge of the glory scattering formula, Eq. (9), we only need to determine and in order to obtain the glory scattering cross section. Therefore, we apply Newton’s method and numerical integration to obtain the parameters and . Numerical results for , , and are presented in Fig. 3. From these results and Eq. (9), we may expect that (i) interference fringes get wider and (ii) backscattered flux intensity is enhanced for higher values of the BH charge. Expectation (i) comes from the fact that the interference fringe width is inversely proportional to , as indicated by the argument of the Bessel function in Eq. (9). Moreover, Fig. 3 shows that decreases monotonically as increases. We also note from Eq. (9) that the scattering intensity is proportional to , and to the wave frequency. As shown in Fig. 3, although decreases monotonically with the increase of , increases monotonically with , justifying expectation (ii).

The above analysis may be compared with the results for the glory scattering from RN BHs Crispino et al. (2009b). In the latter case, decreases monotonically with the increase of the BH charge, while increases monotonically (cf. Fig. 9 of Ref. Crispino et al. (2009b)). Therefore, considering the change of the BH charge, the behavior of the parameters and are qualitatively the same for Bardeen and RN BHs. In the case of RN BHs, however, the combination does not increase monotonically with the charge — as it happens for Bardeen BHs. Instead, the glory scattering amplitude as a function of presents a local minimum in the RN case (cf. Fig. 10 of Ref. Crispino et al. (2009b)).

## Iii Planar wave scattering

Planar massless scalar waves, represented by the wave function , are described by the Klein-Gordon equation

(10) |

Here we shall be interested in monochromatic plane waves. We have

(11) |

where are the scalar spherical harmonics. Substituting Eq. (11) into Eq. (10), we obtain the following radial equation:

(12) |

in which is the tortoise coordinate, defined through , and

(13) |

is the scalar field effective potential. The scalar field potential is localized, going to zero at both asymptotic limits of (infinity and horizon) Macedo and Crispino (2014).

Plane waves coming from infinity can be described in terms of the so-called modes. These modes are purely incoming from the past null infinity, obeying the following boundary conditions:

(14) |

with

(15) | |||||

(16) |

where and are the reflection and transmission coefficients, respectively. Flux conservation implies that . Note that the summations in Eqs. (15) and (16) are required to keep track of the convergence of the solutions. The numerical infinity and horizon are chosen such that at the boundaries.

The scalar differential scattering cross section for Bardeen BHs can be written in terms of partial waves as Futterman et al. (1988)

(17) |

where

(18) |

is the scattering amplitude, with the phase shifts () given by

(19) |

## Iv Results

In order to obtain the phase shifts to compute the scattering cross section via the partial-wave method, we have applied a fourth-fifth Runge-Kutta method to solve the radial equation (12). We have typically started with the near-horizon condition at , and the outer boundary (numerical infinity) chosen depends on the value of . Results were obtained with boundary conditions (14), as well as with alternative conditions in terms of spherical Hankel functions (see, e.g., Eq. (18) of Ref. Crispino et al. (2009b)). Both conditions lead basically to the same results. Since the sum in Eq. (18) does not converge very quickly, because of the Coulomb characteristic of the problem, we have applied the convergence method first introduced by Yennie et al. Yennie et al. (1954), and first applied to the BH scattering problem by Dolan et al. in Ref. Dolan et al. (2006).

In Fig. 4 we show the scattering cross section for Bardeen BHs with different charges (), as well as for the Schwarzschild BH, and . We see that the fringe widths increase with the increase of the BH charge. This, as anticipated by the semiclassical analysis of Sec. II.2, is in accordance with the fact that decreases monotonically with the increase of , as previously seen in Fig. 3. The amount of scattered flux (on average) remains basically the same. These general behaviors are similar to the ones presented by the RN BHs Crispino et al. (2009b).

Figure 5 presents comparisons of the numerical scalar scattering cross sections for Bardeen BHs with the approximated geodesic and glory results. We see that the glory results fit remarkably well the numerical results for large angles (), while the geodesic results fit well the small-angle region. This very good agreement can also be considered as a consistency check of our results.

The glory approximation can be used to capture most of the features of the back-scattered wave. Some caution, however, should be taken when one considers the glory intensity in the backward direction (normalized by the wave frequency). To illustrate this, in Fig. 6 we plot the amplitudes of the back-scattered wave, for and , computed through the partial-wave method and through the glory approximation, as a function of the Bardeen BH charge. We see that the results obtained via the partial-wave method oscillate around the one obtained using the glory approximation. This agrees with the analysis presented in Ref. Crispino et al. (2009b) for RN BHs.

In Fig. 7 we compare the differential scattering cross sections of Bardeen and RN BHs. While RN and Bardeen BHs with the correspondent charge produce different scattering patterns — illustrated by the top-left panel of Fig. 7 — we can have configurations with different charges that produce almost the same scattering pattern. A similarity of the patterns also happens in the case of absorption cross sections, when the critical impact parameter () of the RN and Bardeen cases are the same Macedo and Crispino (2014). Here, however, the similarity of the scattering cross sections intensifies when for the RN and Bardeen cases match. The similarities are illustrated in the top-right and bottom panels of Fig. 7, where we show the scattering cross section for a RN BH with and for a Bardeen BH with , for different values of the frequency. The scattering flux intensities are different for intermediate-to-high scattering angles, while the interference widths are essentially the same for all scattering angles.

## V Final remarks

We have computed the scalar scattering cross section of regular Bardeen BHs. Numerical results were compared with both geodesic and glory approximations, and we have found excellent agreement within the validity limits of each approximation.

From the glory approximation, it is known that the interference fringe widths depend inversely on the impact parameter of backscattered waves, . The classical analysis from geodesics shows that decreases monotonically with the increase of . Therefore, we expect that the interference fringes get wider as increases. This was confirmed from our numerical results obtained via partial-wave method.

Comparison of Bardeen BHs with RN BHs reveals that the
scattering of these two kinds of BHs can be similar but not
identical. By similar we mean that in both cases the scattering
cross section presents (i) intense oscillations in the near-backward
scattering, (ii) rapidly growing flux amount and smoother oscillations for
smaller angles, and (iii) similar results for very small scattering
angles. (i) is a consequence of the strong interference between
rays passing by the opposite sides of the BH, as it is well
described by the glory approximation in both
cases.
(ii) is a consequence of the fact that for small scattering angles both and
increase as diminishes, and the
difference between paths followed by neighboring rays becomes smaller,
weakening interference effects. We can conclude that the main
contribution to the scattering cross section for very small angles
comes from rays with high impact parameters ^{3}^{3}3There are also
contribution from rays with that pass multiple times
around the BH, but since is very small in these
cases, their contribution to the scattering cross section can be neglected.. We may treat such cases in the weak-field regime, where
the main contribution to the gravitational interaction comes from
the BH mass, i.e., ,
where in the case of RN BHs, and
in the case of Bardeen BHs. This explains (iii), i.e., why, for BHs with the same mass, in the regime of small angles, all results tend to be the same, regardless of the nature and value of their charge.

The results presented in this paper reinforce in a way the results presented in Ref. Macedo and Crispino (2014), implying the conclusion that some properties of Bardeen BHs can be very similar to those of RN BHs (with different charge). In this sense, we conclude that it may be difficult to discriminate regular BHs from the standard ones, as far as absorption and scattering of scalar plane waves are concerned. It should be interesting to extend the analyses presented here and in Ref. Macedo and Crispino (2014) to the scattering and absorption of waves with higher spins and compare with recently obtained results for RN BHs Crispino and Oliveira (2008); Crispino et al. (2009c, 2010); Oliveira et al. (2011); Crispino et al. (2014).

###### Acknowledgements.

C.M. thanks A. Flachi for discussions and for pointing out useful references. The authors would like to thank Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES), Fundação Amazônia de Amparo a Estudos e Pesquisas do Pará (FAPESPA) (FAPESPA), and Marie Curie action NRHEP-295189-FP7-PEOPLE-2011-IRSES for partial financial support.## References

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