Superspinning compact objects and models of highfrequency quasiperiodic oscillations observed in Galactic microquasars
II. Forced resonances
^{1} Institute of Physics and Research Centre for Computational Physics and Data Processing, Faculty of Philosophy & Science, Silesian University in Opava, Bezručovo nám. 13, 746 01 Opava, Czech Republic
email: Andrea.Kotrlova@fpf.slu.cz
^{2} Institute of Physics and Research Centre for Theoretical Physics and Astrophysics, Faculty of Philosophy & Science, Silesian University in Opava, Bezručovo nám. 13, 746 01 Opava, Czech Republic
^{3} Nicolaus Copernicus Astronomical Centre, Bartycka 18, 00716 Warsaw, Poland
Received: 9 February 2017
Accepted: 11 July 2017
In our previous work (Paper I) we applied several models of highfrequency quasiperiodic oscillations (HF QPOs) to estimate the spin of the central compact object in three Galactic microquasars assuming the possibility that the central compact body is a superspinning object (or a naked singularity) with external spacetime described by Kerr geometry with a dimensionless spin parameter a ≡ cJ/GM^{2} > 1. Here we extend our consideration, and in a consistent way investigate implications of a set of ten resonance models so far discussed only in the context of a < 1. The same physical arguments as in Paper I are applied to these models, i.e. only a small deviation of the spin estimate from a = 1, a ≳ 1, is assumed for a favoured model. For five of these models that involve Keplerian and radial epicyclic oscillations we find the existence of a unique specific QPO excitation radius. Consequently, there is a simple behaviour of dimensionless frequency M × ν_{U}(a) represented by a single continuous function having solely one maximum close to a ≳ 1. Only one of these models is compatible with the expectation of a ≳ 1. The other five models that involve the radial and vertical epicyclic oscillations imply the existence of multiple resonant radii. This signifies a more complicated behaviour of M × ν_{U}(a) that cannot be represented by single functions. Each of these five models is compatible with the expectation of a ≳ 1.
Key words: Xrays: binaries / black hole physics / accretion, accretion disks
© ESO, 2017
1. Introduction
Accreting black holes (BHs) or neutron stars (NSs) are believed to constitute the compact component in several tens of Xray binaries. The accretion disc contributes significantly to the high Xray luminosity of these objects. Most of the Xray radiation comes from the inner parts of the disc. Both the BH and NS sources exhibit a variability over a wide range of frequencies. In addition to broad noise, their power density spectra (PDS) also contain relatively coherent features known as quasiperiodic oscillations (QPOs). A brief introduction to the subject of QPOs can be found in van der Klis (2006) and McClintock & Remillard (2006).
The Xray PDS of several stellar mass BH systems display lowfrequency (LF) QPOs in the range of 0.1–30 Hz. Their strength expressed in terms of the fractional rootmeansquared (rms) amplitude ℛ is sometimes as high as ℛ ~ 20%. Much attention among theoreticians is, however, attracted to highfrequency (HF or kHz) QPOs that display their frequencies within the range of 40–450 Hz. Highfrequency QPOs usually display much smaller amplitudes than LF QPOs, ℛ ~ 1−4%, but their frequencies correspond to orbital timescales in the vicinity of a BH. It is believed that this coincidence is a strong indication that the corresponding signal originates in the innermost parts of the accretion disc. This belief has also been supported by means of the Fourierresolved spectroscopy (e.g. Gilfanov et al. 2000).
The kHz QPO peaks are detected at rather constant frequencies characteristic for a given source. Moreover, it has been noticed (Abramowicz & Kluźniak 2001; McClintock & Remillard 2006) that they usually appear in ratios of small natural numbers, typically in the 3:2 ratio. Discussion of these measurements and their relation to other sources can be found in McClintock & Remillard (2006), Török et al. (2005), Török (2005a), and van der Klis (2006). It has been noticed that the 3:2 frequencies observed in the Galactic microquasars are well matched by the relation (e.g. McClintock & Remillard 2006) (1)where ν_{L} is the lower of the two frequencies forming the 3:2 ratio,(2)This scaling of QPO frequencies further supports the hypothesis of their orbital origin (e.g. Török et al. 2005).
There is a common conviction in the astrophysical community that studying Xray spectra and variability can be used to put constraints on the properties of compact objects such as BH mass M and spin a ≡ cJ/GM^{2}. A standard way to measure the BH spin is based on different spectral fitting methods, namely by fitting the Xray spectral continuum or the relativistically broadened Fe K alpha lines. Using these spectral fitting methods, many authors have carried out estimations of BH spin (see e.g. McClintock & Remillard 2006; Middleton et al. 2006; Done et al. 2007; McClintock et al. 2007; Miller 2007; Shafee et al. 2008; McClintock et al. 2010, 2011, 2014).
Abramowicz et al. (2004) have suggested that detections of 3:2 QPOs could provide a basis for another method for the determination of masses of BH sources such as the active galactic nuclei and ultraluminous Xray sources. This suggestion is further supported by Török (2005a,b) who has discussed the possibility of orbital resonance origin of QPOs in the Galactic centre BH Sagittarius A^{∗} measured by Aschenbach et al. (2004). It has been argued that the confirmation of 3:2 QPOs in this source could be of fundamental importance to the BH accretion theory. At present, a full decade after these results were published and even though Sgr A^{∗} QPO detections remain questionable, there is a growing evidence of the existence of a largescale validity of the 1 /M scaling of the BH QPO frequencies (1) (see e.g. Zhou et al. 2015).
For a BH candidate which displays HF QPOs and whose mass has been measured by independent measurements, the BH spin estimate can in principle be obtained by simply comparing the observed QPO frequencies to QPO frequencies predicted by a particular QPO model. Through this approach, using miscellaneous QPO models, a number of authors have attempted to estimate the spin of the central Kerr BH in three Galactic microquasars – GRS 1915+105, XTE J1550−564, and GRO J1655−40 – that display the 3:2 twin peak QPOs and have known masses (e.g. Abramowicz & Kluźniak 2001; Wagoner et al. 2001; Kato 2004; Török 2005b; Wagoner 2012; Horák & Lai 2013; OrtegaRodríguez et al. 2014; Motta et al. 2014; Stuchlík & Kološ 2016a,b).
This approach can also be applied in the context of testing hypotheses alternative to consideration of Kerr BHs (Török & Stuchlík 2005; Kotrlová et al. 2008; Psaltis et al. 2008; Bambi & Freese 2009; Gimon & Hořava 2009; Stuchlík & Kotrlová 2009; Stuchlík & Schee 2010, 2012a,b, 2013; Bambi 2011; Johannsen & Psaltis 2011; Li & Bambi 2013a,b; Bambi 2012, 2014; Kološ & Stuchlík 2013; Yagi & Stein 2016; Johannsen 2016). Here we focus on the QPO based spin estimates of compact object properties, in particular on those assuming orbital resonances in Kerr spacetimes.
Fig. 1 Panel a: behaviour of orbital frequencies and location of several resonant radii determined by the Ep and Kep models for a = 0.9. Panel b: behaviour of orbital frequencies and location of several resonant radii determined by the Ep and Kep models for a = 1.001. For Kerr black holes there is only one specific resonant radius for each displayed resonance, while even three resonant radii may appear for a single Ep model in the case of a superspinning compact object or naked singularity. 

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Frequency relations corresponding to individual epicyclic and Keplerian forced resonance models.
2. Estimates of spin in Galactic microquasars and forced resonances
Orbital resonances have been proposed as a generic QPO mechanism in the works of Abramowicz & Kluźniak (2001) and Kluźniak & Abramowicz (2001), and previously discussed in the general framework of orbital motion by Aliev & Galtsov (1981). Several consequent studies have elaborated this proposal (e.g. Abramowicz et al. 2002; Kluźniak & Abramowicz 2002, 2005; Abramowicz et al. 2003a,b; Rebusco 2004; Horák 2004, 2005; Šrámková 2005; Horák & Karas 2006; Vio et al. 2006; Šrámková et al. 2007; Horák 2008; Rebusco 2008; Stuchlík et al. 2008; Horák et al. 2009; Stuchlík et al. 2013, 2014)^{1}. In the works of Kluźniak & Abramowicz (2001) and Török et al. (2005), spin estimates have been carried out for the three microquasars based on a group of QPO models that deal with a nonlinear resonance between some modes of accretion disc oscillations. In particular, Török et al. (2005) have discussed resonances that occur between axisymmetric radial and vertical disc oscillations and that may also involve Keplerian motion.
Assuming fluiddiscoscillation frequencies, it is expected that resonances occur at preferred resonant orbits (QPO excitation radii), r_{p : q} or , where the vertical and radial epicyclic frequency, ν_{r} and ν_{θ}, or the Keplerian (ν_{K}) and radial epicyclic frequency are in ratios of small rational numbers, The 3:2 ratio of the observed frequencies then arises either from the generic 3:2 ratio of the resonant eigenfrequencies or due to resonant combinational frequencies. The wellknown explicit formulae for epicyclic frequencies in Kerr spacetimes have been discussed in several works (e.g. Aliev & Galtsov 1981; Nowak & Lehr 1999; Török & Stuchlík 2005). The behaviour of orbital frequencies and the positions of several specific resonant orbits are illustrated in Fig. 1 assuming two different values of a corresponding to BH and nonBH Kerr spacetimes. For a fixed a, these frequencies scale with the compact object mass M as ν ∝ 1 /M.
Consideration of Kerr BHs and superspinars (or naked singularities) and resonance QPO models. Several variations of resonance models have been assumed by Török et al. (2005). These consist of both parametric and forced nonlinear resonances, in particular the 3:2 parametric resonance, and the 3:1, 2:1, 5:1, 5:2, 5:3 forced resonances. The two most popular alternatives are under consideration: the epicyclic resonance (Ep) model dealing with radial and vertical epicyclic oscillations and the Keplerian resonance (Kep) model assuming a resonance between the orbital Keplerian motion and the radial epicyclic oscillations.
Further complex analysis of spin estimations has been done by Török et al. (2011) for a set of various QPO models. It has been performed namely for hotspotlike models, models assuming a certain form of resonance between some accretion disc oscillatory modes, and for discoseismic models. Individual models considered in Török et al. (2005, 2011) point to very different values of a covering the whole BH range a ∈ [0,1]. The ironline profile, Xray continuum, and the QPO based spin estimates reveal good agreement only in certain particular applications (e.g. Steiner et al. 2011). There are still discrepancies, and no agreement between the three approaches has been achieved so far (see e.g. Török et al. 2011; Kotrlová et al. 2014).
In Kotrlová et al. (2014, hereafter Paper I) we extended the consideration of QPO based spin estimates to the nonBH case and investigated the behaviour of M × ν_{U}(a) relations implied by individual QPO models for a > 1. We discussed various types of models including several resonance models and concluded that the Ep and Kep models are favoured in the context of the a> 1 hypothesis. In Paper I, our consideration did not include forced resonances investigated by Török et al. (2005) for Kerr BHs. Here we explore the predictions of ten of the forced resonance models mentioned above. The list of these models together with associated relations giving observable QPO frequencies is given in Table 1.
Fig. 2 Panel a: resonant radii of Kep models calculated in Kerr spacetimes. Panel b: resonant frequencies of Kep models calculated in Kerr spacetimes. The shaded region corresponds to observational values of ν_{U} × M determined for Galactic microquasars (see Fig. 4 for details and Sect. 5 for a discussion). 

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3. Keplerian models
In this section we examine the predictions of the forced resonance models assuming Keplerian and radial epicyclic oscillations. Paper I illustrates that the 3:2 parametric Kep model implies a much simpler behaviour of the M × ν_{U}(a) relation than the 3:2 parametric Ep model. This is also true for the forced resonance models. As noted by Török & Stuchlík (2005), the ratio between Keplerian frequency and radial (or vertical) epicyclic frequency is a monotonic function of orbital radius r for any value of a ∈ [ 0, ∞). For this reason, there is always a unique QPO excitation radius for any Kep model.
In the particular case of the 3:1 forced Keplerian resonance model (Kep1 model), the resonance occurs at the orbit where(5)and we can express the observed 3:2 QPO frequencies in the same manner as Kluźniak & Abramowicz (2001), (6)Solving Eq. (5) yields the relation between spin and dimensionless resonant radius , (7)where the “−” sign holds for . The associated function is shown in Fig. 2a. Figure 2b then shows the related M × ν_{U}(a) function exhibiting its maximum for .
The other four Kep models (Kep2–Kep5) exhibit qualitatively similar behaviour of resonant radii to that of the Kep1 model. In full analogy, M × ν_{U}(a) relations are then also represented by single continuous functions having a maximum close to . In Table 2 we specify relations between the spin and resonant radii calculated for each of the Kep1–Kep5 models. Illustrations of relevant M × ν_{U}(a) relations are included in Fig. 2.
Spin functions determined for the Keplerian forced resonance QPO models.
4. Epicyclic models
In analogy to Eq. (5), for the 3:1 forced epicyclic resonance model (Ep1 model), the resonance occurs at the r_{3:1} orbit where we have (8)and we can express the observed 3:2 QPO frequencies as Kluźniak & Abramowicz (2001), (9)Solving Eq. (8) yields the relation between the spin and dimensionless resonant radius x_{3:1}, (10)where the “−” sign holds for a ≤ a_{3:1} = 1.08471.
Spin functions a(x_{p:q}) determined for the epicyclic forced resonance QPO models.
Fig. 3 Panel a: resonant radii of Ep models calculated in Kerr spacetimes. The enlarged area emphasizes a region close to a = 1 where each a(r_{p:q}) function exhibits both a local minimum and a local maximum. Global minima of r_{p:q}(a) functions are denoted by circles. Panel b: detailed view of the behaviour of the r_{3:1}(a) relation for a ≈ 1. The global minimum of r_{3:1} is not shown since it occurs only for a higher value of spin, a_{3:1} = 1.08471. 

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Fig. 4 Resonant frequencies of the Ep models calculated in Kerr spacetimes. The enlarged area emphasizes the existence of maxima of the ν_{U} × M curves in the case of the Ep1, Ep3, and Ep4 models in BH spacetimes. The shaded region corresponds to the observational values of ν_{U} × M determined for Galactic microquasars (see Sect. 5 for discussion). Panel a: behaviour of resonant frequencies of the whole group of models on a large scale of a. Panel b: detailed view of behaviour of the resonant frequencies for the Ep1 and Ep2 models for a ≈ 1. The individual horizontal greyscaled areas denote the observational values of ν_{U} × M determined for each of the Galactic microquasars. Panel c: detailed view of the behaviour of resonant frequencies for the Ep3 model for a ≈ 1. Panel d: detailed view of the behaviour of resonant frequencies for the Ep4 and Ep5 models for a ≈ 1. 

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The behaviour of relation (10) is shown in Fig. 3a together with relations obtained for the other four Ep models. On a large scale of a, the displayed curves are similar to those drawn for the Kep models in Fig. 2a. However, there is a qualitative difference which is emphasized within the enlarged area in Fig. 3a. For a ≳ 1, each of Ep models exhibits “Slike” behaviour of resonant radii. In contrast to Kep models, the resonance radius is not a single function of spin because of the nonmonotonic behaviour of the ratio between epicyclic frequencies noted and discussed by Török & Stuchlík (2005) and Stuchlík et al. (2013). We find that for Ep models and three distinct branches of x_{p:q}(a) appear. This is illustrated in detail for the Ep1 model in Fig. 3b. We specify the relations between the spin and resonant radii calculated for each of the Ep1–Ep5 models in Table 3.
The behaviour of resonant frequencies ν_{U}(a) implied by Ep models displayed in Fig. 3 is more complex than that implied by Kep models. In analogy to the comparison between the behaviours of resonant radii, on a large scale of a, there is a similarity between the behaviours of frequencies predicted by both Kep and Ep models (see Figs. 2b and 4a). It can also be found that there is a clear qualitative difference for a ~ 1. Even for a ≲ 1, only the Ep2 and Ep5 models imply qualitatively the same monotonic increase in ν_{U} with increasing a as in the Kep models. The other three Ep models (Ep1, Ep3, and Ep4) display sharp maxima of ν_{U}(a) for rapidly rotating Kerr BHs (see the enlarged area in Fig. 4a). The existence of these maxima is a consequence of the existence of the maximum of the vertical epicyclic frequency ν_{θ}(r) discussed by Török & Stuchlík (2005). For , the M × ν_{U}(a) curves then have the same topology for the Ep1, Ep3, and Ep4 models, and two additional and different topologies for the Ep2 and Ep5 models. These topologies are illustrated in Figs. 4b–d.
Spin intervals inferred for the three microquasars (GRS 1915+105, XTE J1550−564, and GRO J1655−40) from the individual Ep and Kep models.
5. Discussion and conclusions
As discussed in detail in Paper I, numerous attempts to estimate the spin a of black hole candidates have been undertaken using the ironline profile, the Xray continuum, or the QPO frequency fittingmethods. In Paper I we attempted to extend the application of the Xray timing approach to superspinning compact objects with exteriors described by the spacetime of a Kerr naked singularity and interior given by the solutions of string theory. We discussed there various types of QPO models including several resonance models and concluded that the Ep and Kep models are favoured in the context of the a> 1 hypothesis. Here we extended our consideration and investigated in a consistent way the implications of a set of ten forced resonance models including five Kep and five Ep models so far discussed only in the context of a< 1. We applied the same physical arguments to these models as used in Paper I. In particular, we assumed that only a small deviation of spin estimate from a = 1, a ≳ 1 could occur for a favoured model, as is often considered in the case of superspinning relativistic compact objects (Calvani & Nobili 1979; Stuchlík 1980, 1981; Stuchlík et al. 2011; see discussion in Paper I).
Predictions of these ten newly considered models are illustrated in Figs. 2–4. The observationally determined ranges of M × ν_{U}(a) for each of the Galactic microquasars are denoted in Figs. 2b and 4 by the individual horizontal greyscaled areas. For a particular QPO model and source with an independently estimated mass range we calculated the relevant spin interval of the central compact object as predicted by the concrete model. The results are summarized in Table 4 and show that there could be two (for the Kep models) or up to four (for the Ep models) different spin intervals for each QPO model. The number of the relevant spin intervals and their ranges depend on the topology of the M × ν_{U}(a) relation and on the observed range of mass for a given source. Confronting the QPO models predictions with the data of Galactic microquasars^{2}, we find that each of these models is compatible with the assumption of a> 1, but only some of them with the assumption of a ≳ 1.
Comparing our new results with the results obtained in Paper I, we conclude that five Keplerian forced resonance models (Kep1–Kep5) show qualitatively similar behaviour with the 3:2 parametric Keplerian model (Kep) considered in Paper I. More specifically, for all the Kep models we find the existence of a unique QPO excitation radius and consequent simple behaviour of M × ν_{U}(a) relations represented by a single function having solely one maximum close to a ≳ 1. Inspecting the resonant frequencies drawn in Fig. 2b and the results given in Table 4 we can find that only one of the Keplerian forced resonance models (Kep5) is compatible with the expectation of a ≳ 1 and gives quantitatively similar results to the 3:2 parametric Keplerian model (Kep) considered in Paper I. For the other four Kep models (Kep1–Kep4), the inferred values of spin are either lower or several times higher than the extreme Kerr black hole value a = 1. Therefore, for the case of the three Galactic microquasars considered here, these four Kep models can be ruled out from further consideration.
On the other hand, from our results given in Fig. 4 and Table 4, we can see that each of the five epicyclic forced resonance models (Ep1–Ep5) is compatible with the expectation of a ≳ 1, and thus none of them can be ruled out. The Ep models imply the existence of multiple resonant radii and therefore more complicated M × ν_{U}(a) relations than those implied by the Kep models. The Ep1–Ep5 models are similar to the 3:2 parametric epicyclic model (Ep) considered in Paper I. However, as elaborated in Sect. 4, the Ep models in general allow a very wide variety of topologies of the M × ν_{U}(a) relation. The relation explored in Paper I for the Ep model corresponds to only one specific topology from this variety. For the Ep models considered here, three different topologies are possible and for only one of them (Ep5) the M × ν_{U}(a) relation has the same topology as that explored in Paper I.
For all the Ep models, there is the possibility of recognizing a direct observational signature of presence of a superspinning compact object. It is clear from Figs. 4b–d that more pairs of different 3:2 commensurable frequencies can be expected within a single source. In a full analogy to the specific case of Ep model discussed in Paper I, we conclude that this issue can be resolved using the large amount of highquality data available from the next generation of Xray observatories including technologies such as the proposed concept of Large Area Detector (Feroci et al. 2012, 2014; Zhang et al. 2016).
Spin intervals implied by 3:2 or 2:3 QPOs. The results presented in Table 4 assume that the predicted pair of QPO frequencies forms the 3:2 ratio, whereas the frequency denoted in Table 1 as ν_{U} is higher than that denoted as ν_{L}. However, some of the considered models imply that there can be an inverse inequality, ν_{L}/ν_{U} = 3/2. We have investigated this possibility and found that four models are compatible with observation. Specifically, for the Kep4 model the implied spin intervals are then the same as those given in Table 4 for the Kep5 model and vice versa. A fully analogous conclusion also holds for the Ep4 and Ep5 models.
These works often assume the formation of an inner accretion torus, which is frequently considered in the context of the generic QPO mechanism; see also Rezzolla et al. (2003), Zanotti et al. (2005), Schnittman & Rezzolla (2006), Montero et al. (2007), Ingram et al. (2009), Ingram & Done (2010, 2011), Ingram et al. (2016), Török et al. (2016) and references therein.
The assumed values of the measured mass and QPO frequencies of each microquasar are summarized in Table 1 of Paper I, and follow from the studies of Greene et al. (2001), Greiner et al. (2001), Strohmayer (2001), Orosz et al. (2002), Remillard et al. (2002), McClintock & Remillard (2006).
Acknowledgments
We would like to acknowledge the Czech grant GAČR 1716287S, “Oscillations and coherent features in blackhole accretion disks and their observational signatures”. We thank to the INTEREXCELLENCE project No. LTI17018 which supports international activities of the Silesian University in Opava (SU) and Astronomical Institute in Prague (ASU). We also acknowledge two internal SU grants, SGS/14,15/2016 and IGS/2/2016. Z.S. acknowledges the Albert Einstein Center for Gravitation and Astrophysics supported by the Czech Science Foundation grant No. 1437086G. We are grateful to Marek Abramowicz (Nicolaus Copernicus Astronomical Center in Warsaw – CAMK & SU), Wlodek Kluźniak (CAMK), Maciek Wielgus (CAMK), Jiří Horák (ASU), and Pavel Bakala (SU) for many useful discussions. Furthermore we would like to acknowledge the hospitality of CAMK. We express our sincere thanks to the concierges of the Mlýnská hotel in Uherské Hradiště, Czech Republic for their kind help and participation in organizing frequent workshops of SU and ASU. Last but not least, the authors wish to thank the anonymous referee for the useful and constructive comments that substantially helped to improve the manuscript.
References
 Abramowicz, M. A., & Kluźniak, W. 2001, A&A, 374, L19 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Abramowicz, M. A., Almergren, G. J. E., Kluźniak, W., Thampan, A. V., & Wallinder, F. 2002, CQG, 19, L57 [NASA ADS] [CrossRef] [Google Scholar]
 Abramowicz, M. A., Bulik, T., Bursa, M., & Kluźniak, W. 2003a, A&A, 404, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Abramowicz, M. A., Karas, V., Kluźniak, W., Lee, W. H., & Rebusco, P. 2003b, PASJ, 55, 467 [NASA ADS] [CrossRef] [Google Scholar]
 Abramowicz, M. A., Kluźniak, W., McClintock, J. E., & Remillard, R. A. 2004, ApJ, 609, L63 [NASA ADS] [CrossRef] [Google Scholar]
 Aliev, A. N., & Galtsov, D. V. 1981, GRG, 13, 899 [Google Scholar]
 Aschenbach, B., Grosso, N., Porquet, D., & Predehl, P. 2004, A&A, 417, 71 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Bambi, C. 2011, Europhys. Lett., 94, 50002 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Bambi, C. 2012, J. Cosmol. Astropart. Phys., 9, 14 [NASA ADS] [CrossRef] [Google Scholar]
 Bambi, C. 2014, Phys. Lett. B, 730, 59 [NASA ADS] [CrossRef] [Google Scholar]
 Bambi, C., & Freese, K. 2009, PRD, 79, 043002 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Calvani, M., & Nobili, L. 1979, Nuovo Cimento B Serie, 51, 247 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Done, C., Gierliński, M., & Kubota, A. 2007, A&ARv, 15, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Feroci, M., Stella, L., van der Klis, M., et al. 2012, Exp. Astron., 34, 415 [NASA ADS] [CrossRef] [Google Scholar]
 Feroci, M., den Herder, J. W., Bozzo, E., et al. 2014, in Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, Proc. SPIE, 9144, 91442T [CrossRef] [Google Scholar]
 Gilfanov, M., Churazov, E., & Revnivtsev, M. 2000, MNRAS, 316, 923 [NASA ADS] [CrossRef] [Google Scholar]
 Gimon, E. G., & Hořava, P. 2009, Phys. Lett. B, 672, 299 [NASA ADS] [CrossRef] [Google Scholar]
 Greene, J., Bailyn, C. D., & Orosz, J. A. 2001, ApJ, 554, 1290 [NASA ADS] [CrossRef] [Google Scholar]
 Greiner, J., Cuby, J. G., & McCaughrean, M. J. 2001, Nature, 414, 522 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Horák, J. 2004, in RAGtime 4/5: Workshops on Black Holes and Neutron Stars, eds. S. Hledík, & Z. Stuchlík, 91 [Google Scholar]
 Horák, J. 2005, Astron. Nachr., 326, 824 [NASA ADS] [CrossRef] [Google Scholar]
 Horák, J. 2008, A&A, 486, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Horák, J., & Karas, V. 2006, A&A, 451, 377 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Horák, J., & Lai, D. 2013, MNRAS, 434, 2761 [NASA ADS] [CrossRef] [Google Scholar]
 Horák, J., Abramowicz, M. A., Kluźniak, W., Rebusco, P., & Török, G. 2009, A&A, 499, 535 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ingram, A., & Done, C. 2010, MNRAS, 405, 2447 [NASA ADS] [Google Scholar]
 Ingram, A., & Done, C. 2011, MNRAS, 415, 2323 [NASA ADS] [CrossRef] [Google Scholar]
 Ingram, A., Done, C., & Fragile, P. C. 2009, MNRAS, 397, L101 [NASA ADS] [CrossRef] [Google Scholar]
 Ingram, A., van der Klis, M., Middleton, M., et al. 2016, MNRAS, 461, 1967 [NASA ADS] [CrossRef] [Google Scholar]
 Johannsen, T. 2016, CQG, 33, 124001 [NASA ADS] [CrossRef] [Google Scholar]
 Johannsen, T., & Psaltis, D. 2011, ApJ, 726, 11 [NASA ADS] [CrossRef] [Google Scholar]
 Kato, S. 2004, PASJ, 56, L25 [NASA ADS] [CrossRef] [Google Scholar]
 Kluźniak, W., & Abramowicz, M. A. 2001, ArXiv eprints [arXiv:astroph/0105057] [Google Scholar]
 Kluźniak, W., & Abramowicz, M. A. 2002, ArXiv eprints [arXiv:astroph/0203314] [Google Scholar]
 Kluźniak, W., & Abramowicz, M. A. 2005, Ap&SS, 300, 143 [NASA ADS] [CrossRef] [Google Scholar]
 Kološ, M., & Stuchlík, Z. 2013, PRD, 88, 065004 [NASA ADS] [CrossRef] [Google Scholar]
 Kotrlová, A., Stuchlík, Z., & Török, G. 2008, CQG, 25, 225016 [NASA ADS] [CrossRef] [Google Scholar]
 Kotrlová, A., Török, G., Šrámková, E., & Stuchlík, Z. 2014, A&A, 572, A79 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Li, Z., & Bambi, C. 2013a, PRD, 87, 124022 [NASA ADS] [CrossRef] [Google Scholar]
 Li, Z., & Bambi, C. 2013b, J. Cosmol. Astropart. Phys., 3, 31 [NASA ADS] [CrossRef] [Google Scholar]
 McClintock, J. E., & Remillard, R. A. 2006, in Compact Stellar Xray Sources, eds. W. Lewin, & M. van der Klis (Cambridge, UK: Cambridge University Press), Cambridge Astrophys. Ser., 39, 157 [Google Scholar]
 McClintock, J. E., Narayan, R., & Shafee, R. 2007, ArXiv eprints [arXiv:0707.4492] [Google Scholar]
 McClintock, J. E., Narayan, R., Gou, L., et al. 2010, Xray Astronomy 2009, Present Status, MultiWavelength Approach and Future Perspectives, 1248, 101 [NASA ADS] [CrossRef] [Google Scholar]
 McClintock, J. E., Narayan, R., Davis, S. W., et al. 2011, CQG, 28, 114009 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 McClintock, J. E., Narayan, R., & Steiner, J. F. 2014, Space Sci. Rev., 183, 295 [NASA ADS] [CrossRef] [Google Scholar]
 Middleton, H., Del Pozzo, W., Farr, W. M., Sesana, A., & Vecchio, A. 2006, MNRAS, 455, L72 [NASA ADS] [CrossRef] [Google Scholar]
 Miller, J. M. 2007, ARA&A, 45, 441 [NASA ADS] [CrossRef] [Google Scholar]
 Montero, P. J., Zanotti, O., Font, J. A., & Rezzolla, L. 2007, MNRAS, 378, 1101 [NASA ADS] [CrossRef] [Google Scholar]
 Motta, S. E., MuñozDarias, T., Sanna, A., et al. 2014, MNRAS, 439, L65 [NASA ADS] [CrossRef] [Google Scholar]
 Nowak, M., & Lehr, D. 1999, in Theory of Black Hole Accretion Disks, eds. M. A. Abramowicz, G. Björnsson, & J. E. Pringle (Cambridge: Cambridge University Press), 21 [Google Scholar]
 Orosz, J. A., Groot, P. J., van der Klis, M., et al. 2002, ApJ, 568, 845 [NASA ADS] [CrossRef] [Google Scholar]
 OrtegaRodríguez, M., SolísSánchez, H., LópezBarquero, V., MatamorosAlvarado, B., & VenegasLi, A. 2014, MNRAS, 440, 3011 [NASA ADS] [CrossRef] [Google Scholar]
 Psaltis, D., Perrodin, D., Dienes, K. R., & Mocioiu, I. 2008, PRL, 100, 091101 [NASA ADS] [CrossRef] [MathSciNet] [PubMed] [Google Scholar]
 Rebusco, P. 2004, PASJ, 56, 553 [NASA ADS] [Google Scholar]
 Rebusco, P. 2008, New Astron. Rev., 51, 855 [NASA ADS] [CrossRef] [Google Scholar]
 Remillard, R. A., Muno, M. P., McClintock, J. E., & Orosz, J. A. 2002, ApJ, 580, 1030 [NASA ADS] [CrossRef] [Google Scholar]
 Rezzolla, L., Yoshida, S., & Zanotti, O. 2003, MNRAS, 344, 978 [NASA ADS] [CrossRef] [Google Scholar]
 Schnittman, J. D., & Rezzolla, L. 2006, ApJ, 637, L113 [NASA ADS] [CrossRef] [Google Scholar]
 Shafee, R., McKinney, J. C., Narayan, R., et al. 2008, ApJ, 687, L25 [NASA ADS] [CrossRef] [Google Scholar]
 Šrámková, E. 2005, Astron. Nachr., 326, 835 [NASA ADS] [CrossRef] [Google Scholar]
 Šrámková, E., Torkelsson, U., & Abramowicz, M. A. 2007, A&A, 467, 641 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Steiner, J. F., Reis, R. C., McClintock, J. E., et al. 2011, MNRAS, 416, 941 [NASA ADS] [CrossRef] [Google Scholar]
 Strohmayer, T. E. 2001, ApJ, 552, L49 [NASA ADS] [CrossRef] [Google Scholar]
 Stuchlík, Z. 1980, Bull. Astron. Inst. Czechoslovakia, 31, 129 [NASA ADS] [Google Scholar]
 Stuchlík, Z. 1981, Bull. Astron. Inst. Czechoslovakia, 32, 68 [NASA ADS] [Google Scholar]
 Stuchlík, Z., & Kološ, M. 2016a, APJ, 825, 13 [NASA ADS] [CrossRef] [Google Scholar]
 Stuchlík, Z., & Kološ, M. 2016b, A&A, 586, A130 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Stuchlík, Z., & Kotrlová, A. 2009, GRG, 41, 1305 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Stuchlík, Z., & Schee, J. 2010, Class. Quant. Grav., 27, 215017 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Stuchlík, Z., & Schee, J. 2012a, Class. Quant. Grav., 29, 025008 [NASA ADS] [CrossRef] [Google Scholar]
 Stuchlík, Z., & Schee, J. 2012b, Class. Quant. Grav., 29, 065002 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Stuchlík, Z., & Schee, J. 2013, Class. Quant. Grav., 30, 075012 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Stuchlík, Z., Kotrlová, A., & G. Török. 2008, Acta Astron., 58, 441 [NASA ADS] [Google Scholar]
 Stuchlík, Z., Hledík, S., & Truparová, K. 2011, Class. Quant. Grav., 28, 155017 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Stuchlík, Z., Kotrlová, A., & Török, G. 2013, A&A, 552, A10 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Stuchlík, Z., Kotrlová, A., Török, G., & Goluchová, K. 2014, Acta Astron., 64, 45 [NASA ADS] [Google Scholar]
 Török, G. 2005a, A&A, 440, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Török, G. 2005b, Astron. Nachr., 326, 856 [NASA ADS] [CrossRef] [Google Scholar]
 Török, G., & Stuchlík, Z. 2005, A&A, 437, 775 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Török, G., Abramowicz, M. A., Kluźniak, W., & Stuchlík, Z. 2005, A&A, 436, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Török, G., Kotrlová, A., Šrámková, E., & Stuchlík, Z. 2011, A&A, 531, A59 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Török, G., Goluchová, K., Horák, J., et al. 2016, MNRAS, 457, L19 [NASA ADS] [CrossRef] [Google Scholar]
 van der Klis, M. 2006, in Compact Stellar Xray Sources, eds. W. Lewin, & M. van der Klis (Cambridge, UK: Cambridge University Press), Cambridge Astrophys. Ser., 39 [Google Scholar]
 Vio, R., Rebusco, P., Andreani, P., Madsen, H., & Overgaard, R. V. 2006, A&A, 452, 383 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wagoner, R. V. 2012, ApJ, 752, L18 [NASA ADS] [CrossRef] [Google Scholar]
 Wagoner, R. V., Silbergleit, A. S., & OrtegaRodríguez, M. 2001, ApJ, 559, L25 [NASA ADS] [CrossRef] [Google Scholar]
 Yagi, K., & Stein, L. C. 2016, Class. Quant. Grav., 33, 054001 [NASA ADS] [CrossRef] [Google Scholar]
 Zanotti, O., Font, J. A., Rezzolla, L., & Montero, P. J. 2005, MNRAS, 356, 1371 [NASA ADS] [CrossRef] [Google Scholar]
 Zhang, S. N., Feroci, M., Santangelo, A., et al. 2016, in Society of PhotoOptical Instrumentation Engineers (SPIE) Conf. Ser., Proc. SPIE, 9905, 99051Q [CrossRef] [Google Scholar]
 Zhou, X.L., Yuan, W., Pan, H.W., & Liu, Z. 2015, ApJ, 798, L5 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
Frequency relations corresponding to individual epicyclic and Keplerian forced resonance models.
Spin functions a(x_{p:q}) determined for the epicyclic forced resonance QPO models.
Spin intervals inferred for the three microquasars (GRS 1915+105, XTE J1550−564, and GRO J1655−40) from the individual Ep and Kep models.
All Figures
Fig. 1 Panel a: behaviour of orbital frequencies and location of several resonant radii determined by the Ep and Kep models for a = 0.9. Panel b: behaviour of orbital frequencies and location of several resonant radii determined by the Ep and Kep models for a = 1.001. For Kerr black holes there is only one specific resonant radius for each displayed resonance, while even three resonant radii may appear for a single Ep model in the case of a superspinning compact object or naked singularity. 

Open with DEXTER  
In the text 
Fig. 2 Panel a: resonant radii of Kep models calculated in Kerr spacetimes. Panel b: resonant frequencies of Kep models calculated in Kerr spacetimes. The shaded region corresponds to observational values of ν_{U} × M determined for Galactic microquasars (see Fig. 4 for details and Sect. 5 for a discussion). 

Open with DEXTER  
In the text 
Fig. 3 Panel a: resonant radii of Ep models calculated in Kerr spacetimes. The enlarged area emphasizes a region close to a = 1 where each a(r_{p:q}) function exhibits both a local minimum and a local maximum. Global minima of r_{p:q}(a) functions are denoted by circles. Panel b: detailed view of the behaviour of the r_{3:1}(a) relation for a ≈ 1. The global minimum of r_{3:1} is not shown since it occurs only for a higher value of spin, a_{3:1} = 1.08471. 

Open with DEXTER  
In the text 
Fig. 4 Resonant frequencies of the Ep models calculated in Kerr spacetimes. The enlarged area emphasizes the existence of maxima of the ν_{U} × M curves in the case of the Ep1, Ep3, and Ep4 models in BH spacetimes. The shaded region corresponds to the observational values of ν_{U} × M determined for Galactic microquasars (see Sect. 5 for discussion). Panel a: behaviour of resonant frequencies of the whole group of models on a large scale of a. Panel b: detailed view of behaviour of the resonant frequencies for the Ep1 and Ep2 models for a ≈ 1. The individual horizontal greyscaled areas denote the observational values of ν_{U} × M determined for each of the Galactic microquasars. Panel c: detailed view of the behaviour of resonant frequencies for the Ep3 model for a ≈ 1. Panel d: detailed view of the behaviour of resonant frequencies for the Ep4 and Ep5 models for a ≈ 1. 

Open with DEXTER  
In the text 