Issue 
A&A
Volume 581, September 2015



Article Number  A35  
Number of page(s)  12  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/201525867  
Published online  28 August 2015 
Twin peak highfrequency quasiperiodic oscillations as a spectral imprint of dual oscillation modes of accretion tori
^{1} Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, 746 01 Opava, Czech Republic
email: pavel.bakala@fpf.slu.cz
^{2} Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00716 Warszawa, Poland
^{3} Institute of Physics, Polish Academy of Sciences, aleja Lotnikow 32/46, 02668 Warszawa, Poland
^{4} Physics Department, Gothenburg University, 41296 Göteborg, Sweden
Received: 11 February 2015
Accepted: 24 May 2015
Context. Highfrequency (millisecond) quasiperiodic oscillations (HF QPOs) are observed in the Xray powerdensity spectra of several microquasars and lowmass Xray binaries. Two distinct QPO peaks, socalled twin peak QPOs, are often detected simultaneously exhibiting their frequency ratio close or equal to 3:2. A widely discussed class of proposed QPOs models is based on oscillations of accretion toroidal structures orbiting in the close vicinity of black holes or neutron stars.
Aims. Following the analytic theory and previous studies of observable spectral signatures, we aim to model the twin peak QPOs as a spectral imprint of specific dual oscillation regime defined by a combination of the lowest radial and vertical oscillation mode of slender tori. We consider the model of an optically thick slender accretion torus with constant specific angular momentum. We examined power spectra and fluorescent Kα iron line profiles for two different simulation setups with the mode frequency relations corresponding to the epicyclic resonance HF QPOs model and modified relativistic precession QPOs model.
Methods. We used relativistic raytracing implemented in the parallel simulation code LSDplus. In the background of the Kerr spacetime geometry, we analyzed the influence of the distant observer inclination and the spin of the central compact object. Relativistic optical projection of the oscillating slender torus is illustrated by images in false colours related to the frequency shift.
Results. We show that performed simulations yield power spectra with the pair of dominant peaks that correspond to the frequencies of radial and vertical oscillation modes and with the peak frequency ratio equal to the proper value 3:2 on a wide range of inclinations and spin values. We also discuss exceptional cases of a very low and very high inclination, as well as unstable high spin relativistic precessionlike configurations that predict a constant frequency ratio equal to 1:2. We demonstrate a significant dependency of broadened Kα iron line profiles on the inclination of the distant observer.
Conclusions. This study presents a further step towards the proper model of oscillating accretion tori producing HF QPOs. More realistic future simulations should be based on incorporating the resonant coupling of oscillation modes, the influence of torus opacity, and the pressure effects on the mode frequencies and the torus shape.
Key words: accretion, accretion disks / black hole physics / relativistic processes
© ESO, 2015
1. Introduction
Highfrequency quasiperiodic oscillations (HF QPOs) have been observed in several microquasars and lowmass Xray binaries (LMXBs). Their frequencies are roughly comparable to frequencies of the orbital motion of test particles in the vicinity of the central compact object. The black hole HF QPOs occur at frequencies that are characteristic of a particular source and that seem to be constant in time. Strictly speaking, the current observational data only enables HF QPOs to be distinguished for fairly specific spectral states (Belloni et al. 2012). However, provided that HF QPOs with lower amplitudes and different frequencies exist in the remaining time, their detection goes beyond our present technological capabilities.
Two kinds of sharp HF QPO peaks can be distinguished, socalled lower and upper HF QPOs (see van der Klis 2004; Remillard & McClintock 2006, for a review). If both HF QPO peaks are observed simultaneously (twinpeak HF QPOs), the ratio of frequencies of upper and lower HF QPO peaks is often close to 3:2, indicating the possible presence of unspecified resonant phenomena (Abramowicz & Kluźniak 2001; Török et al. 2005)^{1}. At present, there is no consensus about the QPO nature. However, the inverse mass scaling of the QPOs frequencies (Abramowicz & Kluźniak 2001) provides a strong argument for interpreting the observed QPO peaks by the frequencies of perturbed orbital motion in the strong gravitational field or oscillation of some accretion structures. Such interpreting naturally promises an attractive possibility of measuring the mass and spin of the black hole (e.g. Abramowicz & Kluźniak 2001; Abramowicz & Fragile 2013; Ingram & Motta 2014; Motta et al. 2014; Török 2005; Török et al. 2012). Many QPO models have been proposed (Alpar & Shaham 1985; Lamb et al. 1985; Miller et al. 1998; Psaltis et al. 1999; Stella & Vietri 1999; Abramowicz & Kluźniak 2001, 2004; Kato 2001, 2007; Titarchuk & Wood 2002; Rezzolla et al. 2003; Schnittman & Bertschinger 2004; Pétri 2005; Zhang 2005; Tagger & Varnière 2006; Stuchlík et al. 2008; Mukhopadhyay 2009; Čadež et al. 2008; Kostić et al. 2009; Germanà et al. 2009; Germanà 2013; Lai et al. 2013; Pecháček et al. 2008, 2013); however, each model still faces several difficulties. Moreover, the capabilities of the present Xray observatories (e.g. Rossi Xray Timing Explorer – RTXE) are insufficient for adequately analysing the harmonic content of the power spectra of observed lightcurves, which can be crucial for distinguishing between particular QPO models (Bakala et al. 2014; Karas et al. 2014). Hopefully, the proposed future instruments represented by the Large Observatory for Xray Timing (LOFT) project (Feroci et al. 2014), for instance, which is targeted to explore strong gravity environment, will advance QPOs observational possibilities.
A specific class of QPO models assumes oscillations excited in accretion tori. The first QPO model involving numerically modelled thick accretion tori was developed by Rezzolla et al. (2003), and related lightcurves and power spectra were analysed by Schnittman & Rezzolla (2006). Lightcurves and power spectra of radially and vertically oscillating slender torus with a circular crosssection were investigated in the background of the Schwarzschild geometry by Bursa et al. (2004). Numerical simulations of epicyclic modes of tori oscillations were compared to the analytical results by Šrámková (2005). Later on, several studies devoted to more realistic analytic treatment of oscillating slender tori appeared (e.g. Abramowicz et al. 2006; Blaes et al. 2006). These studies were extended to the case of nonslender tori by Šrámková et al. (2007) and Straub & Šrámková (2009).
In this paper, we examine the timing properties of the numerically simulated flux emitted from a slender, polytropic, perfect fluid, nonselfgravitating accretion torus with constant specific angular momentum, which oscillates simultaneously in radial and vertical directions^{2}. The article is a followup of the studies of Mazur et al. (2013) and Vincent et al. (2014), who investigated the observable signatures of simple timeperiodic slender torus deformations, as well as the slender torus motion described by the set of oscillation modes derived by Blaes et al. (2006). Using their results, we took the next step towards a fully realistic model of HF QPO based on oscillations of accretion tori. To model detected twinpeak HF QPOs pairs, we defined a new dual oscillation mode as a linear combination of the two lowest slender torus oscillation modes: radial and vertical ones. We assumed that the observed twin peaks HF QPOs can be identified with the pairs of the most prominent peaks in the modelled power spectra. We examined two different setups of the dual oscillation regime corresponding to the twin peaks HF QPOs frequency relation of epicyclic resonance HF QPOs model (Abramowicz & Kluźniak 2001) and slightly modified analogous relations of relativistic precession QPOs model (Stella & Vietri 1999; Török et al. 2012). Those two competing QPOs models are probably the most discussed ones at present (Feroci et al. 2014).
Our simulations were performed in the background of the Kerr geometry that corresponds to the case of microquasars with the black hole binary component. It was shown that the spacetime around slowly rotating highmass neutron stars can be approximated fairly well by the Kerr metric (Török et al. 2010, 2012; Urbanec et al. 2013). Therefore, such a finding sets conditions and constraints for the applicability of our results for the case of LMXBs with neutron star.
The commonly accepted model of Xray energy spectrum of microquasars and LMXBs assumes that the illumination of the cold accretion disk or torus by the primary component of Xray spectrum, interpreted as the inverse Compton scattering of thermal photons in a hot corona, produces spectral lines by fluorescence. The strongest observed line is the Kα iron line located at 6.4 keV in the rest frame. Observed broad profiles of the spectral lines are substantially influenced by the spacetime metric, the geometry of the emitting region and the distant observer inclination (Fabian et al. 1989; Čadež & Calvani 2005; Bambi 2013). To develop an additional tool for distinguishing various configurations of radiating slender torus, we computed related Kα iron line profiles.
The article consits of the following parts. Section 2 is devoted to the theory that describes the slender torus model and its dual oscillation regime. Section 3 provides more details of the investigated particular setup of the model of slender torus. Section 4 describes our numerical implementation of relativistic raytracing and the following construction of lightcurves, power spectra, and iron Kα line profiles. Section 5 is devoted to the methodology of simulations performance and results analysis. Section 6 shows the obtained results, and Sect. 7 gives conclusions and future research perspectives.
2. Slender torus
2.1. Equilibrium torus configuration
We consider an axisymmetric, non selfgravitating, perfect fluid, constant specific angular momentum, circularly orbiting accretion torus in the background of the Kerr geometry. Using the (−+++) signature and geometrical units (c = G = M = 1), the line element of the Kerr spacetime in BoyerLindquist coordinates parameterized by specific angular momentum (spin) a reads (1)where Σ ≡ r^{2} + a^{2}cos^{2}θ and Δ ≡ r^{2}−2r + a^{2}. Moreover, we assume that the radial extent of the torus crosssection is smaller than its central radius. The perfect fluid that forms the torus is described by the polytropic equation of state (with a polytropic constant K and polytropic index n). In this case, the energy density e is a function of pressure p and mass density ρ. The pressure is a function of mass density alone. The torus surface is given by the zero pressure, while the pressure gradient is equal to zero in the torus centre. Using the conservation law, one can get (see Abramowicz et al. 2006; Blaes et al. 2006) (2)where the surface function f is constant at isobaric and isodensity surfaces. Naturally, the surface function vanishes at the torus surface. Here and below, values of the quantities denoted with a subscript _{0} are taken in the centre of the torus in the equilibrium state.
Following Abramowicz et al. (2006), we use the new radial and vertical coordinates (3)with zero in the torus centre. Parameter β determines the torus thickness and is given by formula (4)where denotes the fourvelocity of the fluid and square of the sound speed can be expressed in the form (5)Keplerian angular velocity Ω_{K0} in the Kerr spacetime reads as(6)In the case of slender torus, the parameter β must fulfil the condition (7)In such a coordinate frame, the surface function f(r,θ) can be rewritten as (8)where are radial and vertical epicyclic frequencies of free test particles in the centre of the torus scaled to Ω_{K0} (see e.g. Aliev & Galtsov 1981; Abramowicz & Kluźniak 2005; Aliev 2008). We can easily see that the slender torus crosssection (given by ) has elliptical shape in the  plane.
2.2. Oscillating slender torus
We assume small pressure perturbation in the form (11)where m is azimuthal wave number (m ∈ N), and Ω is oscillation angular frequency. It is useful to introduce a new variable – eigenfunction W_{i}, which is the function of perturbation in pressure in the form (12)where related eigenfrequency σ_{i} reads (13)The perturbative surface equation and torus fourvelocity can be expressed in the form (Vincent et al. 2014) A discrete set of eigefunctions W_{i} and related eigenfrequencies σ_{i} describing different oscillation modes was found by Blaes et al. (2006) solving PapaloizouPringle equation for slender torus case corresponding to the condition β → 0 (Abramowicz et al. 2006; Papaloizou & Pringle 1984). Here we use only the two simplest solutions: radial oscillation mode and vertical oscillation mode. In the case of radial oscillation mode, the eigenfunction and related eigenfrequency are given as (16)where a_{r} is a free parameter related to the amplitude of oscillations. Then the surface Eq. (14) takes the form (17)where amplitude A_{r} is given by the formula (18)and the mode oscillation angular frequency reads as(19)To rewrite the surface Eq. (17) to the form (20)the term (21)must be added. Then the displacement can be expressed by the formula (22)In this approximation, the added term should be small enough, which corresponds to the condition for radial amplitudes (23)The radial component of the surface fourvelocity is simply given by a derivative of the displacement with respect to proper time τ as (24)and it takes the covariant form (25)Analogously, in the case of the vertical oscillation mode, the eigenfunction and related eigenfrequency are given as (26)Using the condition for vertical amplitudes , the surface equation, displacement and surface fourvelocity component for the vertical mode can be expressed as
where amplitude A_{θ} given by formula (30)and mode oscillation angular frequency reads (31)
2.3. Dual oscillation mode
In such an approximation, radial and vertical oscillations are independent, and we can easily combine them into a new surface equation (32)The equation above defines the dual oscillation mode with four parameters: amplitudes A_{r}, A_{θ} and azimuthal wave numbers m_{r}, m_{θ}.
3. Investigated model of oscillating slender torus
3.1. Location, thickness, and frequencies identification
Radial and vertical angular frequencies Ω_{r},Ω_{θ} of the dual oscillation mode are given as a linear combination of eigenfrequencies σ_{r},σ_{θ}, and Keplerian angular velocity Ω_{K0}. Therefore the location of the torus centre in equilibrium r_{0}, value of the spin of the central Kerr black hole and wave number pair m_{r}, m_{θ} fully determine the ratio of oscillation angular frequencies Ω_{θ}/ Ω_{r}. Considering the properties of epicyclic and orbital frequencies in the Kerr spacetime (Török & Stuchlík 2005), our model identifies the lower and upper kHz QPOs frequencies with ν_{l} = Ω_{r}/ 2π and ν_{u} = Ω_{θ}/ 2π, respectively. As the aim of the article is to model twin peak HF QPOs with peaks frequency ratio close to 3:2, we choose r_{0} in such a way that the ratio Ω_{θ}/ Ω_{r} is just equal to 3:2 for a given wave number pair^{3}. In each of these positions of the torus centre, we set the radial extent of the torus crosssection to r_{0}/10. Corresponding values of the parameter β are in accordance with a slender torus condition (7). Arbitrary amplitudes of oscillations are fixed by setting .
3.2. Optical properties of the torus
The torus described above is assumed to be optically thick. Moreover, we use two other very simple assumptions. The torus surface emits radiation isotropically in its comoving local frame and the local flux integrated over the surface area of a thin vertical slice of the torus is conserved. Such a surface area is proportional to r_{c}(t_{em},φ) × C(t_{em},φ), where C(t_{em},φ) is the torus crosssection circumference, t_{em} the time of emission, and r_{c}(t_{em},φ) the radial coordinate of the centre of the torus crosssection. In the case of the approximation we used, the investigated dual oscillation mode describes pure radial and vertical displacements, and the torus crosssection circumference remains constant. Therefore, using normalization to 1 for the equilibrium state, the local emitted intensity simply reads as (33)
3.3. Epicyclic resonance axisymmetric setup
The first investigated torus setup combines pure epicyclic axisymmetric vertical and radial oscillation, where radial and vertical oscillation frequencies are identical with radial and vertical epicyclic frequencies, respectively. This setup corresponds to the often quoted epicyclic resonance (ER) HF QPOs model (Abramowicz & Kluźniak 2001) based on the presence of nonlinear resonant phenomena between epicyclic disc oscillation modes (Kluźniak & Abramowicz 2001; Abramowicz et al. 2003a,b; Horák 2008). The dual oscillation mode with such behaviour is related to wave number pair m_{r} = 0, m_{θ} = 0. Therefore the frequency relation determining the radial coordinate of the torus centre r_{0} reads as(34)
3.4. Relativistic precessionlike nonaxisymmetric setup
The dual oscillation mode related to wave number pair m_{r} = −1, m_{θ} = −2 yields the frequency relation in the form (35)where ν_{K} = Ω_{K0}/ 2π is the Keplerian orbital frequency at r_{0}. As the denominator matches the periastron precession frequency, in the Schwarzschild case the relation corresponds exactly to the relation of the relativistic precession (RP) QPOs model (36)The RP model was proposed in a series of papers by Stella & Vietri (1998, 1999, 2002), Morsink & Stella (1999) and explains the QPOs as a direct manifestation of relativistic epicyclic motion of radiating blobs (Stella & Vietri 1999). In the case of slow rotation, the frequency relation (35) still almost coincides with the ratio of twin peaks HP QPOs frequencies predicted by the relation (36) (Török et al. 2012). Such an approach can be understood as a redefinition of the modulation mechanism of RP model, but it preserves the predictive power of the model.
4. Numerical modelling of radiation emission, propagation, and detection
4.1. Raytracing in the Kerr spacetime
Fig. 1 Schematic raytracing geometry for the cases of a general observer and distant observer (r_{obs} → ∞). 

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Relativistic raytracing is a key ingredient of proper models of relativistic imaging, lightcurves of accretion structures, related power spectra, as well as relativistic spectral line profiles. Different raytracing techniques were developed using direct numerical integration, transfer functions, and elliptic integrals (see e.g. Cunningham & Bardeen 1972; Karas et al. 1992; Viergutz 1993; Schnittman 2006; Rauch & Blandford 1994; Beckwith & Done 2005; Broderick & Loeb 2005; Bakala et al. 2007; Dexter & Agol 2009; Vincent et al. 2011; Schee & Stuchlík 2013; Chan et al. 2013; Yang & Wang 2014). Our parallel code LSDplus uses reverse raytracing implemented by a direct numerical integration of the null geodesics.
Components of the fourmomentum of a photon in the Kerr spacetime are given by (37)where the dotted quantities denote differentiation with respect to some affine parameter, and the sign pair s_{r},s_{θ} describes orientation of radial and latitudinal evolution, respectively (see e.g. Carter 1968; Misner et al. 1973; Chandrasekhar 1983). Radial and latitudial effective potentials read as (38)Here, λ and q are constants of motion related to the photons covariant angular and linear momenta. The LSDplus code performs a timereverse integration of the package of null geodesics falling on a virtual detector of a distant observer with the screen resolution 1000 × 1000 pixels located at (θ_{obs}, r = 1000 M, ϕ = 0) and traces the intersection of the geodesics with the disk surface corresponding to the emission events.
The code LSDplus enables modelling relativistic optical effects in the sky of the observer located anywhere above the event horizon of a Kerr black hole. In the local reference frame related to such an observer, the components of the fourmomentum of photons with energy normalized to one, falling on the pixel with coordinates x, y, can be written as follows (see the right side of Fig. 1): (39)Then one can obtain the coordinate covariant components of the fourmomentum by transforming the local components (39), using appropriate frame tetrads of oneform by relation (40)The frame tetrad of oneform related to static observer in the Kerr spacetime is given as (41)The constants of motion λ(x,y) and q(x,y) can be easily obtained by straightforward calculation from the components of the fourmomentum (40), using the relations (see e.g. Chandrasekhar 1983) (42)However, in the investigated case of a distant static observer (r_{obs} → ∞), when the rays reaching the observer position are almost parallel (see Fig. 1), the relations between coordinates on the detector screen and constants of motion can be simply written as (e.g. Cunningham & Bardeen 1973) (43)In the event of detection, the constants λ(x,y) and q(x,y), together with the initial conditions (coordinates of observer and sign pair s_{r}, s_{θ}), fully determine the reverse temporal evolution of the zero geodesics of photons falling on a pixel of the detector screen with the coordinates x, y. The Runge Kutta method of the eighth order (DormanPrince method) (Press et al. 2002) used here, integrates the null geodesics and reaches the relative accuracy of 10^{15}, which, in the case of a central black hole with stellar mass M = 5 M_{⊙}, corresponds to an order of accuracy of 10^{11} m on a radial coordinate. To determine the proper orientation of the radial and latitudinal component of the fourmomentum (37), the code also analyses the positions of the radial and vertical turning point and sets the corresponding signs s_{r} and s_{θ}. The integration of Eq. (37) by the Runge Kutta method of the eighth order proceeds naturally with an adaptive step. However, the resulting null geodesic is then finally interpolated by the polynomials of the third order for the chosen equidistant time step ΔT, in the case of central black hole mass M = 5 M_{⊙}, corresponding to 10^{5} s.
4.2. Radiating surfaces and lightcurves
The surfaces of the tori are modelled by the grid with a resolution of 15 nodes in the radial direction and 75 nodes in the azimuthal one. The grid contains the timedependent information about coordinates, local intensity, and the fourvelocity in the nodes. The time resolution of the surface of the tori necessarily corresponds to the time resolution of the interpolation steps of the geodesics package ΔT. The code LSDplus traces the intersections of the geodesics and linearly interpolated surface of a torus between triads of the nodes of the grid. Assuming the normalized energy in the local observer’s frame, the frequency ratio of the emitted and observed radiation from the torus can be expressed using projection of the fourmomentum of a photon p^{μ} to the fourvelocity of the surface of the torus in the event of the emission as follows: (44)Radial and vertical components of the surface fourvelocity are given by equations (25) and (29). The remaining components , can easily be obtained using the normalisation condition u^{μ}u_{μ} = −1, together with the assumption of constant specific angular momentum (Vincent et al. 2014). Then the instantaneous bolometric intensity detected by each pixel of the screen of a small virtual detector is calculated as (45)where t_{delay} corresponds to the time delay (the change of a time coordinate) along the appropriate photon trajectory connecting the event of detection of a photon on a pixel with the event of emission on the surface of the torus. Here, I_{em} is local intensity on the surface in the comoving frame given by the Eq. (33). The total instantaneous detected bolometric flux F(t_{obs}) is a sum of intensities (45) detected by individual pixels multiplied by the solid angle ΔΠ subtended by the pixel in the observer sky (46)where i is the index of a pixel column and where j is the index of a pixel row^{4}. Since we are using relative units, we can simply set ΔΠ = 1. The resulting lightcurves are generated in the time resolution ΔT that corresponds to 20 time samples per characteristic vertical oscillation period of the analysed dual oscillation mode.
4.3. Power spectra
To calculate power spectral densities (PSD), the resulting lightcurves are processed by fast Fourier transform (FFT). The PSD at frequency f_{k} = k/ (NΔt) is given as the square of the modulus of the FFT of the signal as (47)where F(t_{j}) is the observed flux (46) at observation time t_{j} = jΔt, and N is the total number of time samples in the lightcurve.
4.4. Iron Kα line profiles
The fluorescent iron Kα line consists of two components with FWHM ≈ 3.5 eV and separation ≈13 eV (see Basko 1978, for details). Considering the energy resolution ΔE = 10 eV of the simulation code, we approximated the rest iron Kα line profile by Lorentzian peak with the scale factor γ = 20 eV located at E_{0} = 6.4 keV. The instantaneous observed flux per pixel in the energy bin with the central energy E_{c} is given as (48)where Lorentzian function f reads as(49)Then the observed instantaneous iron Kα line profile is constructed by summing energy bin fluxes per pixels (48) over all pixels of the virtual detector in the given time sample. The final integrated line profile is obtained by summing instantaneous line profiles over all time samples.
5. Methods
Applying raytracing methods described in the previous section, we performed simulations of lightcurves of the model discussed above of a slender accretion torus oscillating in the dualmode regime. To obtain closed trajectories of the torus surface and corresponding closed lightcurves, we simulated the behaviour of emitted radiation during three periods of vertical oscillation considering the fixed ratio of oscillation frequencies ν_{u}/ν_{l} = 3:2. Then we calculated power spectra of obtained lightcurves by relation (47). We studied the impact of the central black hole spin using its three representative values a ∈ (0, 0.5, 0.96). The upper limit of the investigated spin value is almost the highest one, for which the location of equilibrium torus centre r_{0} can be found by the RPlike frequency relation (35). The impact of the observer inclination (polar angle) i is analysed using the following set of inclination values: We analyse the magnitude relations of five prominent PSD peaks corresponding to two main dualmode oscillation frequencies, their higher harmonics, and their sum or difference, particularly summarised in the Table 1.
Most prominent peaks observed in power density spectra of simulated lightcurves.
Power spectra are calculated for all combinations of investigated values for the spin and the inclination. We plot the magnitudes of these peaks as linearly interpolated functions of the inclination for all the investigated values of the spin and for both investigated torus setups separately (see left panels of Figs. 3 and 4).
Moreover, the integrated iron Kα line profiles emitted from the torus surface are modelled for inclination values . The geometry of the torus’s optical projection is illustrated in Fig. 2 by the frequency shift maps on the virtual detector screen drawn in false colours related to the frequency shift values^{5}. The maps clearly show that the simulation parameters are sufficient for distinguishing the first three relativistic images. The iron Kα line profiles that were also computed display significant secondary blueshifted horns related to secondary (first indirect) relativistic images (see right panels of Figs. 3 and 4).
Fig. 2 Examples of the frequency shift maps for different distant views of the oscillating slender torus. The colour boxes on the right display the false colours scale of frequency shift values. The left column corresponds to the case of the ER axisymmetric dual mode. The right column corresponds to the case of the RPlike nonaxisymmetric dual mode. The rows of the figure correspond to spin values a = 0, a = 0.5 and a = 0.96, respectively. 

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Fig. 3 Simulations outputs in the case of the ER axisymmetric dual mode. Left panels: the amplitudes of prominent PSD peaks (see Table 1) as a function of distant observer inclination i. Right panels: iron Kα line profiles constructed for . The rows of the picture correspond to the cases of spin values a = 0, a = 0.5, and a = 0.96, respectively (see Table 2). 

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Fig. 4 Simulations outputs in the case of the RPlike nonaxisymmetric dual mode. Left panels: the amplitudes of prominent PSD peaks (see Table 1) as a function of distant observer inclination i. Right panels: iron Kα line profiles constructed for . The rows of the picture correspond to the cases of spin values a = 0, a = 0.5, and a = 0.96, respectively (see Table 3). 

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6. Results
6.1. Results for the ER axisymmetric setup
Table 2 summarises the parameters of the slender torus that oscillates in the pure epicyclic axisymmetric dual mode (m_{r} = 0, m_{θ} = 0) for three investigated values of the spin. The radial coordinate of equilibrium torus centre r_{0} given by relation (34) remains above both the black hole photosphere^{6} and the ergosphere for all such configurations.
Values of parameters describing the investigated slender torus model for ER axisymmetric setup.
The lightcurve waveforms are influenced by a complex interplay of the general relativistic frequency shift, the time variation of the emitting torus surface area, and the time variation of the apparent torus area on the virtual detector screen (Bakala et al. 2015). All these effects strongly depend on the radial coordinate of the emission event, the inclination of the distant observer i, and the central black hole spin a. Nevertheless, the magnitude relations depicted in the lefthand panels of Fig. 3 exhibit certain identical qualitative features for all investigated spin values. The pair of peaks corresponding to radial ν_{l} and vertical ν_{u} torus oscillation frequency is dominant on a wide range of i. For this inclination range, the examined ER axisymmetric setup predicts twin peaks HF QPOs frequency ratio equal to 3:2 in accordance with expectations. The ν_{l} peak remains most prominent for low and medium values of distant observer inclination i. The magnitude of the ν_{u} peak grows with i becoming the most prominent for relatively high inclinations, but it rapidly falls for exact or almost exact equatorial observers. At the same time, the magnitude of the peak corresponding to 3ν_{l}, 2ν_{u} rapidly grows. Therefore, in the case of such observers, the examined torus configuration predicts a frequency ratio equal to 1/3 for the pair of the most distinguishable HF QPO peaks. In the case of zero or moderate spins (a = 0, a = 0.5) and small inclinations (), the magnitude of the 2ν_{l} peak slightly exceeds the ν_{l} peak magnitude, and the predicted twin peaks HF QPOs frequency ratio value is equal to 1:2. As illustrated in the plots of magnitude relations (see left panels of Fig. 3), the spectral content of less distinct PSD peaks varies depending on values of i and a.
Like the power spectra behaviour, the iron Kα line profiles keep some identical qualitative features for all investigated spin values. Naturally, the energy span of line profiles is expanded and shifted down with decreasing r_{0}. The dependence of the height of the primary blueshifted horns on i is the only qualitative difference observable for different spin values (see right panels of Fig. 3).
6.2. Results for the RPlike nonaxisymmetric setup
Table 3 summarizes parameters of the slender torus oscillating in the RPlike nonaxisymmetric dual mode (m_{r} = −1, m_{θ} = −2) for three investigated values of the spin. In the case of zero or moderate spin (a = 0, a = 0.5), the radial coordinate of equilibrium torus centre r_{0} given by relation (35) remains located above the black hole photosphere, as well as the ergosphere, while in the case of high spin (a = 0.96), the torus is located inside the ergopshere and therefore also deeply inside the photosphere. Moreover, in the case of high spin, the radial extent of the torus obtained as r_{0}/ 10 exceeds the location of the cusp of equipotential surfaces (Blaes et al. 2006; Straub & Šrámková 2009). Such a torus configuration becomes unstable. Unfortunately, a surface area of the high spin stable configuration with maximum possible β = 7.0 × 10^{5} is almost negligible, and emitted flux is comparable to the numerical error of the simulation. Therefore, we keep the torus radial extent equal to r_{0}/ 10 and choose the unstable high spin configuration with β = 0.002.
Values of parameters describing the investigated slender torus model for RPlike nonaxisymmetric setup.
In the case of zero or moderate spin (a = 0, a = 0.5), the qualitative picture of power spectra and iron Kα line profiles behaviour is very similar to the case of the ER axisymmetric setup discussed in the previous section (see Fig. 4). The prediction for low inclination represents the main difference. In the Schwarzschild case, the pair of peaks corresponding to radial ν_{l} and vertical ν_{u} oscillation frequency also remains dominant for , predicting the twin peaks HF QPOs frequency ratio equal to 3:2, as depicted in the top left panel of Fig. 4. In the case of a = 0.5 and a very small inclination, the magnitude of the ν_{u}−ν_{l} peak (instead of the 2ν_{l} peak acting the same way in the case of the ER axisymmetric setup) slightly exceeds the ν_{l} peak magnitude, and the predicted twin peaks HF QPOs frequency ratio is equal to 1:2 (see the middle left panel of Fig. 4).
The unstable highspin configuration exhibits an entirely different picture, as shown in the bottom panels of Fig. 4. In the whole range of inclination, the pair of dominant PSD peaks corresponds to the radial ν_{l} frequency and its second harmonic 2ν_{l}. Therefore, in the unstable high spin case, the examined RPlike nonaxisymmetric setup surprisingly predicts the twin peaks HF QPOs frequency ratio value that is only equal to 1:2. The dramatic change of the optical projection properties is documented by iron Kα line profiles in the bottom righthand panel of Fig. 4. The energy span is significantly shifted down, and both primary and secondary blueshifted horns have comparable heights. The computed profiles also display numerical instabilities caused by a small emitting surface area of the unstable high spin torus configuration. The line profile related to exhibits exceptional behaviour, because its extremely wide energy span reaches 11 keV and its primary blueshifted horn is absolutely dominant. The corresponding frequency shift map in the bottom righthand panel of Fig. 2 also illustrates the equatorial optical projection of the torus located in the close vicinity of the Kerr black hole event horizon. It is clearly visible that the angular size of both secondary and tertiary relativistic images exceeds the angular size of the primary image. Moreover, despite the significant gravitational redshift, the high Keplerian orbital velocity causes a high Doppler blueshift for the left side of the torus projection corresponding to the extreme height of the primary blueshifted horn in the iron Kα line profile.
7. Conclusions and perspectives
The aim of this article has been to model twin peaks HF QPOs as a spectral impact of isotropically radiating slender tori oscillating in a dual mode regime in the close vicinity of Kerr black holes. Vincent et al. (2014) show that a significant fraction of the observed flux is regulated by the torus motion described by the lowest oscillation modes. We therefore examined two configurations of the dual oscillation regime based on the lowest radial and vertical oscillation modes with different azimuthal wave numbers. Appropriate frequency relations correspond to the two competing QPOs models, the epicyclic resonance (ER) HF QPOs model (Abramowicz & Kluźniak 2001) and a slightly modified relativistic precession (RP) QPOs model (Stella & Vietri 1999). We model twin peaks HF QPOs by the pair of the most prominent peaks in the obtained power spectra. Our results show that independently of the spin, the ER axisymmetric setup yields power spectra with the pair of dominant PSD peaks corresponding to the frequencies of radial and vertical oscillation modes with a proper ratio equal to 3:2, except some special cases of very high or very low distant observer inclinations, where higher harmonics becomes prominent. The predictions of the RPlike nonaxisymmetric setup are almost identical to the ER case for zero or moderate spin configurations. An unstable highspin RPlike configuration with the torus located in the ergosphere exhibits dominant PSD peaks pair corresponding to the frequency of radial oscillation modes and its second harmonics in the whole range of inclinations, so it predicts a constant frequency ratio equal to 1:2. The entire change of the optical projection is also documented by the different iron Kα line profiles with respect to the previous cases.
The analysis presented in the article primarily focused on the relative ratios of the amplitudes of the most prominent frequency peaks in the modelled power spectra. However, the absolute fractional rms of the amplitudes of HF QPOs peaks in the detected signal depends not only on the amplitudes of perturbation A_{r,θ}, but also on the relations of individual components of the whole total source flux. In Bakala et al. (2014) we defined an empirical model of total source flux, which mimics the socalled high steep powerlaw (HSPL) state in GRS 1905+105, including steep spectrum and powerlawdominated variability with an additional broad Lorentzian component at low frequencies (McClintock & Remillard 2006). Then we used this background to analyse the resolution of HF QPO peaks for a similar but simpler model of oscillating slender torus in the Schwarzschild geometry (Bursa et al. 2004), slowly passing the resonant orbit r_{0}. Considering the capabilities of the RXTE and LOFT instruments simulated by their response matrices, we showed that the presently available observational technology enables a good detection of the pair of the most prominent peaks in such a modelled signal. Nevertheless, the behaviour of spectral content of less distinct PSD peaks probably remains the key task for the data analysis of future sensitive space observatory missions for Xray timing, such as the proposed LOFT mission (see Bakala et al. 2014; Feroci et al. 2014; Karas et al. 2014, for details).
Our simulation yields iron Kα line profiles that are very different from the line profile integrated over the entire accretion disk. Therefore, the next related topic for future space Xray missions can be sensitive frequencyresolved spectroscopy, which will be able to isolate the spectral component oscillating on the QPO frequency (see e.g. Axelsson et al. 2014; Revnivtsev et al. 1999). Phaseresolved spectroscopy that traces the iron line profile changes throughout an oscillation cycle could be another potentially interesting diagnostic tool. This idea has already been suggested for the case of lowfrequency QPOs (e.g. Ingram & Done 2012b; Tsang & Butsky 2013), but its application for the studied model of HF QPO driven by slender torus oscillations will require a more detailed future study.
We assume an optically thick slender torus, and thus the influence of the torus opacity can also be the subject for our future research. It is possible to generalise the examined slender torus model by considering the pressure effects on the mode frequencies and the torus shape (Straub & Šrámková 2009). In our study, the location of the torus centre is empirically chosen using the observed twin peaks HF QPOs ratio. The resonant coupling of oscillation modes can prefer particular values of radial coordinate for amplification or excitation of QPOs (Horák 2008). Therefore, further important improvements in the simulations can incorporate moderesonant coupling. Future implementation of improved models of nonslender tori into the used LSDplus code can be the next step towards more realistic results. A future detailed comparative study of spectral harmonic content can also be devoted to the possibility of distinguishing between QPOs models based on either accretion tori oscillations or the orbital motion of radiating blobs.
In the case of LMXBs, there are indications that the ratio of twin peak HF QPOs frequencies is not only clustered around 3:2, but 4:3 and 5:4 ratios are also observed (see e.g. Török et al. 2007, 2008a,b,c).
The slender torus geometry considered here accords well with the truncated disk model (see e.g. Done et al. 2007). Also, the power spectral fits of Ingram & Done (2012a) predict that the hot inner flow (corona) has a small scale height in the relevant spectral state.
Investigated torus model does not consider the presence of the resonant coupling of oscillation modes, which can cause amplification or excitation of QPOs for the preferred values of the radial coordinate (Horák 2008).
The frequency shift maps displayed in Fig. 2 are not zoomed and not positioned identically with respect to the projection of the whole observer sky.
Kerr black hole photosphere – a region of spherical unstable photon orbits reaches maximum extent in the equatorial plane between corotating and counterrotating circular photon orbits, while it becomes infinitesimally thin on the polar axis (see e.g. Teo 2003, for details)
Acknowledgments
We acknowledge the Czech research grant GAČR 209/12/P740, Polish NCN UMO2011/01/B/ST9/05439 grant and the internal grants of Silesian University in Opava IGS/11/2015 and SGS/11/2013.
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All Tables
Most prominent peaks observed in power density spectra of simulated lightcurves.
Values of parameters describing the investigated slender torus model for ER axisymmetric setup.
Values of parameters describing the investigated slender torus model for RPlike nonaxisymmetric setup.
All Figures
Fig. 1 Schematic raytracing geometry for the cases of a general observer and distant observer (r_{obs} → ∞). 

Open with DEXTER  
In the text 
Fig. 2 Examples of the frequency shift maps for different distant views of the oscillating slender torus. The colour boxes on the right display the false colours scale of frequency shift values. The left column corresponds to the case of the ER axisymmetric dual mode. The right column corresponds to the case of the RPlike nonaxisymmetric dual mode. The rows of the figure correspond to spin values a = 0, a = 0.5 and a = 0.96, respectively. 

Open with DEXTER  
In the text 
Fig. 3 Simulations outputs in the case of the ER axisymmetric dual mode. Left panels: the amplitudes of prominent PSD peaks (see Table 1) as a function of distant observer inclination i. Right panels: iron Kα line profiles constructed for . The rows of the picture correspond to the cases of spin values a = 0, a = 0.5, and a = 0.96, respectively (see Table 2). 

Open with DEXTER  
In the text 
Fig. 4 Simulations outputs in the case of the RPlike nonaxisymmetric dual mode. Left panels: the amplitudes of prominent PSD peaks (see Table 1) as a function of distant observer inclination i. Right panels: iron Kα line profiles constructed for . The rows of the picture correspond to the cases of spin values a = 0, a = 0.5, and a = 0.96, respectively (see Table 3). 

Open with DEXTER  
In the text 
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