Profiled spectral lines generated by Keplerian discs orbiting in the Bardeen and AyonBeatoGarcia spacetimes
Abstract
Shape and frequencyshift map of direct and indirect images of Keplerian discs orbiting in Bardeen and AyonBeatoGarcia (ABG) black hole and nohorizon spacetimes are determined. Then profiles of spectral lines generated in the innermost parts of the Keplerian discs in the Bardeen and ABG spacetimes are constructed. The frequencyshift maps and profiled spectral lines are compared to those generated in the field of Schwarzschild black holes and possible observationally relevant signatures of the regular black hole and nohorizon spacetimes are discussed. We demonstrate that differences relative to the Schwarzschild spacetimes are for the nohorizon spacetimes much more profound in comparison to the regular black hole spacetimes and increase with increasing charge parameter of the spacetime. The differences are stronger for small and large inclination angles than for mediate ones. For the nohorizon spacetimes, the differences enable to distinguish the Bardeen and ABG spacetime, if inclination angle to the distant observer is known. We also show that contribution of the so called ghost images to the profiled lines increases with increasing charge parameter of the spacetimes.
Introduction
The black holes governed by standard general relativity contain a physical singularity with diverging Riemann tensor components and predictability breakdown, considered as a realm of quantum gravity overcoming this internal defect of general relativity. However, families of regular black hole solutions of Einstein’s gravity have been found that eliminate the physical singularity from the spacetimes having an event horizon. Of course, these are not vacuum solutions of the Einstein equations, but contain necessarily a properly chosen additional field, or modified gravity, so that the energy conditions related to the existence of physical singularities [25] are then violated.
The regular black hole solution containing a magnetic charge as a source parameter has been proposed by Bardeen [14], having the magnetic charge related to a nonlinear electrodynamics [7]. The other solution of the combined Einstein and nonlinear electrodynamic equations has been introduced by AyonBeato and Garcia [4, 5, 6]. Both these solutions are characterized by the mass parameter and the charge parameter . Their geodesic structure is governed by the dimensionless ratio giving the specific charge of the source. Details of the properties of the electromagnetic fields related to the spherically symmetric Bardeen and AyonBeatoGarcia (ABG) spacetimes were discussed by Bronnikov [16, 17]. A different approach to the regular black hole solutions was applied by Hayward [26]. Modification of the mass function in the Bardeen and Hayward solutions and inclusion of the cosmological constant can be found in the new solutions of Neves and Saa [34]. Rotating regular black hole solutions were introduced in [33, 11, 59, 8].
For properly chosen charge parameter , the Bardeen and ABG solutions allow for existence of fully regular spacetime, without an event horizon. We call such solutions ”nohorizon” spacetimes. Some of their properties were discussed in [38]. We shall consider here both the black hole and nohorizon spacetimes.
Dynamics of test particles and fields around regular black holes has been recently discussed in [38, 59, 8, 22, 60, 61, 21, 23, 31]. A detailed discussion of the geodesic structure of the regular Bardeen and ABG black hole and nohorizon spacetimes and its implication to simple optical phenomena as the silhouette shape and extension and the profiled spectral lines generated by Keplerian rings constituted from test particles following stable circular geodesics were presented in [57]. It has been demonstrated that the geodesic structure of the regular black holes outside the horizon is similar to those of the Schwarzschild or ReissnerNördström (RN) black hole spacetimes, but under the inner horizon, no circular geodesics can exist. The geodesic structure of the nohorizon spacetimes is similar to those of the naked singularity spacetimes of the RN type [50, 39] related to the Einstein gravity, or the KehagiasSfetsos (KS) type [55, 56] that is related to the solution of the modified Hořava quantum gravity [28, 27] in the infrared limit [29]. In all of these nohorizon and naked singularity spacetimes, an ”antigravity” sphere exists consisting of static particles located at stable equilibrium points at a given ”static” radius that can be surrounded by a Keplerian disc.
In the naked singularity and nohorizon spacetimes, additional optical images of Keplerian discs in comparison to those related to the images observed in the field of black holes exist [52, 55, 46]. They occur in the region that should be empty in the case of images created in the black hole spacetimes – for this reason we call them ghost images. Moreover, character of the ghost images differs in the case of the naked singularity spacetimes, and the nohorizon spacetimes, because of different character of the motion of photons having small values of the impact parameter. Such photons feel strong repulsion in the naked singularity spacetimes, but they feel very weak influence in the central region of the nohorizon spacetimes [46].
Properties of the Keplerian discs in the Bardeen and ABG nohorizon spacetimes strongly depend on the value of the charge parameter. If the charge parameter is close to value corresponding to the extreme blackhole state, two Keplerian discs exist above the static radius, and even two photon circular orbits exist in the nearextreme states, the inner one being stable representing the outer edge of the inner Keplerian disc, while the outer disc is limited by the innermost stable circular geodesic. As an exceptional phenomenon, not occuring in the naked singularity or the Bardeen nohorizon spacetimes, an internal Keplerian disc can occur under the antigravity sphere in the ABG nohorizon spacetimes with [57]. Such an internal disc can be visible, if matter is not filling whole the static radius.
It is important to look for observationally relevant phenomena of the regular Bardeen and ABG blackhole and nohorizon spacetimes. In strong gravity, three observationally important tests are widely discussed – the spectral continuum [41, 32], the profiled spectral lines [30, 12, 13, 20, 44, 45], and highfrequency quasiperiodic oscillations [51, 53]. Here we calculate the profiled spectral lines generated at the innermost parts of the Keplerian accretion discs related to stable circular geodesics [35]. The profiled spectral lines generated at the spherically symmetric regular blackhole and nohorizon spacetimes are compared to those generated under corresponding conditions around Schwarzschild black holes.
First, we compare for the Bardeen and ABG black hole and nohorizon spacetimes the direct and indirect images, including the ghost images, of the innermost parts of the Keplerian discs radiating in a fixed frequency, giving the shape of the images and map of the frequency shift of the radiation. Then we calculate profiled spectral lines generated by the innermost parts of the Keplerian discs taking into account the condition of the negative gradient of angular velocity in the Keplerian discs [57] that is necessary condition for the accretion governed by the magnetorotational instability (MRI) [9, 10], as discussed in [55, 62]. We also demonstrate the role of the ghost images in the shaping of profiled spectral lines.
The electromagnetic field related to the spherically symmetric regular Bardeen and ABG black hole (or nohorizon) spacetimes is discussed in [4, 5, 6]. Due to the electrodynamics nonlinearity, the motion of photons could deviate from the null geodesics of the spacetimes. However, here we do not consider these deviations keeping the assumption of the photon motion governed by the null geodesics of the spacetime, as in related previous studies. Then the electromagnetic field is irrelevant for our study and we consider the geometry properties only, both for the Keplerian (circular) geodesic motion assumed for accretion discs, and the null geodesics of the spacetime related to the photon motion. We assume that at the centre of coordinates, , the selfgravitating source of the electromagnetic field of the background is located, where trajectories of test particles and photons terminate, similarly to the case of the central singular points in the spherically symmetric naked singularity spacetimes [46].
1 Regular Bardeen and AyonBeatoGarcia spacetimes
The spherically symmetric geometry of the regular Bardeen and ABG blackhole or nohorizon spacetimes is characterized in the standard spherical coordinates and the geometric units (c=G=1) by the line element
(1) 
where the ”lapse” function depends only on the radial coordinate, the gravitational mass parameter . and the charge parameter . Both Bardeen and ABG spacetimes are constructed to be regular everywhere, i.e., the components of the Riemann tensor, and the Ricci scalar are finite at all [6].
The lapse function reads

Bardeen spacetime
(2) 
ABG spacetime
(3)
The event horizons of the Bardeen and ABG spacetimes are given by the condition
(4) 
The loci of the black hole horizons are determined by the relations

Bardeen
(5) 
ABG
(6)
The solutions for the location of the event horizons are presented in Figure 1. If real and positive solutions of the equation (4) do not exist, the spacetime is fully regular, having no event horizon. We call it ”nohorizon” spacetime. The critical values of the dimensionless parameter separating the blackhole and the ”nohorizon” Bardeen and ABG spacetimes read

Bardeen
(7) 
ABG
(8)
In the ”no horizon” Bardeen and ABG spacetimes the metric is regular at all radii . We assume to be the site of the selfgravitating charged source of the spacetime; test particle or photon trajectories terminate at . For more details on the properties of the Bardeen and ABG spacetimes see [57, 46].
2 Keplerian discs and classification of the Bardeen and ABG spacetimes
The Keplerian accretion discs are governed by circular geodesics of the background spacetime. In the spherically symmetric spacetimes the geodesics are tied to central planes. For the Keplerian discs we choose the central plane to be the equatorial plane . The spacetime symmetries imply existence of two constant of motion, the energy related to the timelike Killing vector, and the axial angular momentum related to the axial Killing vector that coincides with the total angular momentum for the motion in the equatorial plane. The rest massenergy is the other constant of motion. Then it is convenient to consider the specific energy and specific angular momentum . For simplicity we can put .
2.1 Effective potential and circular geodesics
The circular motion of test particles is determined by an effective potential related to the specific angular momentum related to the particle rest mass that takes in the equatorial plane of spherically symmetric spacetimes a simple form
(9) 
The radial equatorial motion of a particle with specific energy is then governed by the equation for the radial component of the 4velocity
(10) 
For the photon motion, , the effective potential is related to the impact parameter and reads
(11) 
The properties of the effective potential outside the event horizon are similar to those in the Schwarzschild spacetimes, while in the nohorizon spacetimes they are similar to the case of RN naked singularity spacetimes, and are discussed in [57].
The specific angular momentum , the specific covariant energy , and the angular frequency relative to distant observer of the circular geodesic orbits at a given radius in the Bardeen and ABG spacetimes take the form [57]

Bardeen
(12) (13) (14) 
ABG
(15) (16) (17)
We now briefly summarize properties of the circular geodesics that were in detail presented in [57]. First we give two significant radii occuring in all the Bardeen and ABG nohorizon spacetimes.
2.2 Antigravity sphere
In all the Bardeen and ABG nohorizon spacetimes a static radius exists where an ”antigravity” effect of the geometry is demonstrated by vanishing of the specific angular momentum, , similarly to the case of the KS naked singularity spacetimes of the modified Hořava gravity [55, 62], or to the case of the RN naked sigularity spacetimes [50, 39]. The static radius is given by

Bardeen
(18) 
ABG
(19)
Location of the static radius in dependence on the charge parameter of the Bardeen and ABG nohorizon spacetimes is demonstrated in Figure 1. The static radius corresponds to an ”antigravity” sphere where the particles can remain is stable static equilibrium. The antigravity sphere, being surrounded by a Keplerian disc, can be considered as a final state of the accretion process, and in some sense can represent the effective surface of the objects described by the Bardeen of ABG nohorizon spacetimes. No circular orbits are possible under the stable static radius, except the case of the ABG nohorizon spacetimes with the charge parameter when ”internal” circular orbits can exist under the stable static radius [57]. The inner part of the ABG internal circular geodesics starting at is stable, and is separated by an outermost stable circular geodesic from the region of unstable circular geodesics terminating at an outer edge of the circular geodesics given by a secondary static radius corresponding to static particles in an unstable static equilibrium position [57] – see Figure 1.
2.3 Radius of local maximum of the angular frequency of circular geodesics
The standard Keplerian accretion requires increasing gradient of the angular frequency of the orbiting matter, , if the MRI accretion mechanism should be at work [9]. However, this condition is not fulfilled for all stable circular geodesics in the nohorizon Bardeen and ABG spacetimes, similarly to the spherically symmetric naked singularity spacetimes of the KS type [55].
The local maximum of the function is located along the curve determined by the condition that for the particular spacetime imply the formulae

Bardeen
(20) 
ABG where is determined in an implicit form by the relation
(21)
The functions are given for both the Bardeen and ABG spacetimes in Figure 1. The radius can be considered as the inner edge of the standard Keplerian discs. Possible scenarios of the subsequent accretion, under the radius , are discussed in [55] and will not be repeated here.
2.4 Classification of the Bardeen and ABG spacetimes according to circular geodesics
Now, we summarize the classification of the Bardeen and ABG spacetimes introduced in [57]. In the nohorizon spacetimes, the classification is related to the character of the circular geodesics above the antigravity sphere. The classification is related to the existence of the photon circular geodesics (stable at and unstable at ) and the marginally stable geodesics (giving the outer edge at and the inner edge at ) that are determined in [57]. Dependence of these radii on the dimensionless charge parameter is given in Figure 1. The critical values of the charge parameter governing the spacetimes allowing for existence of photon (marginally stable) orbits () are given in Table 1.
Charge parameter  

Bardeen  
ABG 
The classification of the Bardeen and ABG spacetimes according to the properties of the circular geodesics (at in the nohorizon spacetimes) was given in [57] and is summarized in Table 2; the classification holds equally for the Bardeen and ABG spacetimes.
Range of  Regions of circular geodesics  

Class I  
Class II  
Class III  
Class IV 
In the Class II spacetimes, two regions of circular geodesics exist above the stable static radius. The outer one ranges, as in the blackhole spacetimes, from infinity down to the unstable photon circular geodesic. The stable circular orbits exist down to the ISCO, under which unstable circular orbits exist being limited from below by the unstable photon circular orbit. The inner region consists of stable circular geodesics that range from the stable photon circular geodesic down to the static radius with stable equilibrium positions of test particles. It should be stressed that the inner region of stable circular geodesics is very extraordinary one, being very narrow, with the specific energy and specific angular momentum of the freely orbiting matter decreasing extremely steeply from arbitrarily high values down to the minimum at the stable static radius [57].
In the Class III spacetimes, the circular geodesics extend from infinity down to the stable static radius. Two regions of stable circular geodesics are separated by a region of unstable circular geodesics. The outer region of stable orbits extends from infinity down to the ISCO, the inner region of the stable orbits extends from the OSCO down to the stable static radius.
3 Photon motion and direct and indirect images of Keplerian discs
In [46] we have constructed the direct and indirect Keplerian disc images in the Bardeen spacetimes, with focus on the special case of the direct ghost images. Here, we systematically compare appearance of the innermost parts of the Keplerian discs orbiting the regular Bardeen and ABG black hole, and nohorizon spacetimes of all three classes, and give their distinction to the images created by the Schwarzschild black hole.
We present the optical appearance of both direct and indirect images of the Keplerian discs, reflecting their shape distortions due to gravitational lensing, and the frequency shift of the emitted radiation due to the gravitational and Doppler effects. We include also the ghost images related to the direct and indirect images, not going into details of their construction that have been exhaustively discussed in the case of the regular Bardeen nohorizon spacetimes and the ReissnerNordstrom naked singularity spacetimes in [46]. We demonstrate the combined gravitational and Doppler shifts by a simple map assuming the Keplerian discs radiating locally at a fixed frequency corresponding, e.g., to a Fe Xray line. In the following section, we construct profile of the spectral lines (usually assumed to be the fluorescent spectral Fe lines) generated in the innermost regions of the Keplerian discs, extending thus the results of the previous paper [57] where profiled spectral lines were constructed in the simple case of radiating Keplerian rings near the ISCO.
The disc appearance can be relevant for sources close enough when the current observational technique enables a detailed study of the innermost parts of the accretion structures located at vicinity of the black hole horizon or at the innermost parts of the nohorizon spacetimes. Such extremely precise observations are expected during few next years for the Sgr A* source [19, 24, 36, 42, 37, 18]. On the other hand, the profiled spectral lines can be measurable also for very distant sources.
3.1 Photon motion
For a general motion not confined to the equatorial plane where the Keplerian disc location is assumed, the trajectories of photons are independent of energy and can be related to impact parameters
(22) 
where is the axial angular momentum and represents the total angular momentum [57]. For the nonequatorial photon motion, it is convenient to use the coordinates
(23) 
(24) 
The equations of the radial and the latitudinal motion then take the form [55]
(25) 
where
(26) 
and
(27) 
that can be properly integrated when photons radiated by Keplerian discs are considered [40, 43, 44, 52].
3.2 Frequency shift
We assume the Keplerian discs to be composed from isotropically radiating particles following the circular geodesics. The frequency shift of radiation emitted by a point source moving along a circular orbit in the equatorial plane is given in the standard manner – the frequency shift between the emitter (e) and observer (o) is defined by the formula
(28) 
For circular orbits, the emitter fourvelocity has only the time and axial components
(29) 
For the static observers at infinity, the frequency shift formula then reads
(30) 
where is the impact parameter of the photon, and is the angular velocity of the emitter, here assumed to be the Keplerian angular velocity.
3.3 Apppearance of Keplerian discs
Appearance of the Keplerian discs gives a basic physical information on the strong gravity influencing astrophysical processes around compact objects [43, 52, 1, 53, 3, 2]. We shall construct the direct and indirect images of the Keplerian discs for small, mediate, and large inclination angle of the discs relative to the distant observers. In the case of regular Bardeen and ABG black holes, the Keplerian accretion discs have their edge at the ISCO. In the case of the nohorizon spacetimes allowing stable circular geodesics only, the Keplerian discs related to the MRI viscosity mechanism are considered to be physically relevant and will be studied here – a detailed discussion can be found in the case of the KehagiasSfetsos naked singularity spacetimes in [55]. Therefore, in the nohorizon spacetimes with , we restrict our attention to the outer Keplerian discs located at , while in the spacetimes with , we consider the part of the Keplerian discs at . We also demonstrate the possible role of the Keplerian disc located at for the Bardeen spacetime.
We are comparing the role of the specific charge of the spacetime in the appearance of the Keplerian discs. Since the regions of the specific charges related to the Bardeen and ABG nohorizon spacetimes of the same class are not overlapping in the case of the Classes II and III, admitting the unstable circular geodesics and the photon circular geodesics, we choose the values of the specific charge in the following way:
(31) 
In the case of the black hole spacetimes, and the nohorizon spacetimes with , the value of the specific charge is chosen the same for the Bardeen and ABG spacetimes.
We construct the direct and indirect images for characteristic values of the spacetime charge parameter (that will be for short denoted as , assuming m=1) covering all four spacetime classes. The images are given for typical inclination angles of the Keplerian disc to the distant static observer , , . For each of the inclination angles, we first compare the Bardeen and ABG black hole images to the image created by the Schwarzchild black hole and then compare the Bardeen and ABG nohorizon Class II  IV spacetime images.
The direct images are presented in Figures 27, while indirect images are presented in Figures 813. The role of the region of the Keplerian disc where , and the MRI condition is not satisfied, is demonstrated in Figs 14 and 15. In all the cases the outer edge of the Keplerian disc is located at . The images are expressed in terms of the standard coordinates and introduced in the basic paper of Bardeen [15]. The frequency shift is represented by a colour code, and by few lines of . The frequency range reflecting the edges of the color code is explicitly given for each of the individual images.
We see that the images created in the Bardeen and ABG black hole spacetimes are of the same character as those created by the Schwarzschild black hole. Small differences are reflected by the range of the frequency shift  they have the same character for both direct and indirect images and considered inclination angles. For small () and intermediate () inclination the frequency range shifts to smaller values at both ends of the range, as compared to the Schwarzschild range; the shift is larger for the ABG black holes than for the Bardeen black holes. For large inclination angles (), the frequency shift decreases at the red end of the range and increases at the blue end, being larger for the ABG black holes. Generally, the extension of the frequency range is larger for direct images as compared to the indirect images.
We further observe that the direct images have the same character for the Bardeen and ABG spacetimes of Class IIIII in both the image shape and the frequency shift distribution. Clear differences arise in the case of the Class IV spacetimes, with inner edge of the Keplerian disc at . For a given spacetime parameter , the ghost images are more visible in the ABG spacetime, while the range of the frequency shift across the direct image is narrower in comparison to those in the Bardeen spacetime, as demonstrated especially for the large inclination angle (Figure 7) – we can see even the ghost image in the ABG spacetime, while it does not occur in the Bardeen spacetime. Note that the highest blueshift occurs for the direct images created in the black hole spacetimes for the small and mediate inclination angles, while for the large inclination the largest blueshift occurs for the direct images generated in the Bardeen Class III spacetime.
For the indirect images only minor shift of their properties occurs again in the Bardeen and ABG spacetimes of Class IIIII. For the Class IV ABG spacetime with , the indirect images do not exist for small and mediate inclination angles (Figures 9 and 11) as their gravitational field is too weak to cause deflection of light strong enough to create the indirect images under small and mediate inclination angles. The ghost secondary images do not exist in both the Bardeen and ABG Class IV spacetimes for the large inclination angle (Figure 13).
For values of , properties of the images in the Bardeen spacetimes can be similar to those demonstrated in the ABG spacetime, as shown in [46] where also the higherorder images in the Bardeen Class II spacetimes have been studied. We shall not repeat here discussion of the higherorder images that is qualitatively the same for the Bardeen and ABG spacetimes. For the highest blueshift in the indirect images we observe the same qualitative properties as those that are demonstrated in the direct images. Generally, the highest blueshift is lower in the indirect images than in the direct images.
The possible influence of the innermost parts of Keplerian discs in the Bardeen spacetimes located at is reflected for direct (Figure 14) and indirect (Figure 15) images that demonstrate no effect on frequency shift range, but for large inclination angle () the occurrence of the direct ghost image is demonstrated in Figure 14.
4 Profiles of spectral lines
In constructing the profiled spectral lines we assume the radiation that originates in the innermost regions of Keplerian disc governed by the strong gravity of the regular black hole and nohorizon spacetimes. The disc is composed of point sources orbiting on circular geodetical orbits and radiating locally isotropicaly and monochromatically, i.e., at the frequency given by a considered spectral line, usually the Fe spectral line giving Xray radiation. The spectral line is then profiled by the gravitational lensing and by the gravitational frequency shift combined with the Doppler frequency shift due to the orbital motion that are related to a fixed distant observer.
The profiles of spectral lines are constructed for the radiation coming from the disc region between the inner edge at and some appropriatelly chosen outer edge at . Each emitted photon suffers from gravitational and Doppler frequency shift which takes the general form
(32) 
where the photon impact parameter and is the Keplerian angular frequency.
The specific flux at the detector is constructed by binning the photons (pixels) contributing to specific flux at observed frequency . Let ith pixel on the detector subtends the solid angle . Then the corresponding flux reads
(33) 
where the specific intensity of naturally (thermally) broadened line with the power law emissivity model is given by
(34) 
In our simulations the dimensionless parameter and the emissivity law index .
The solid angle is given by the coordinates and on the observer plane due to the relation , where denotes the distance to the source. The coordinates and can be then expressed in terms of the radius of the source orbit and the related redshift factor . The Jacobian of the transformation implies [44, 45]
(35) 
The parameter represents the total photon impact parameter related to the plane of motion of the photon, while represents the axial impact parameter related to the plane of the Keplerian disc. To obtain the specific flux at a particular frequency , all contributions given by are summed
(36) 
5 Constructed profiled lines
We construct the profiled lines assuming in the standard way the extension of the radiating Keplerian discs to be restricted between the innermost stable circular orbit at and for the black hole spacetimes. In the case of the nohorizon spacetimes with (), i.e., with doubled region of the stable circular orbits, we do not consider the inner region of the stable orbits and we put . In the case of the nohorizon spacetimes with (), we do not consider the region of and we put . However, in a special case we demonstrate the role of the contribution from the radiating region to the profiled spectral line. On the other hand, we include the contribution of the ghost images [46] to the profiled spectral lines. In all the nohorizon spacetimes, we keep the outer edge of the radiating disc at . We compare our results to the profiled line generated by the Keplerian disc with and orbiting a Schwarzschild black hole.
5.1 Black hole spacetimes
The modelled profiles of spectral lines generated by the Keplerian discs in vicinity of the Bardeen and ABG black holes are constructed for the spacetimes with the same charge parameter and the results are presented in Figure 16 for the typical inclination angles of the Keplerian discs to the distant observer , , . The same angles will be used for construction of the profiled lines in all the considered nohorizon spacetimes.
We can see that for both the Bardeen and ABG spacetimes the profiled lines follow very closely the line corresponding to the Schwarzschild black hole case. It is quite interesting that the coincidence is strongest for the mediate inclination angle (). Small differences arise for the small () and large () inclination angles. For both small and large inclination angles the tendency in both the Bardeen and ABG spacetimes is to make the profile flatter in comparison to the Schwarzschild profile; for increasing charge parameter the peak height is slightly suppressed, while the frequency range slightly increases. The modifications in the ABG black hole spacetime are slightly stronger than those in the Bardeen spacetime. However, these modifications are very small and their detectability is probably out of abilities of recent observational technique.
5.2 Nohorizon spacetimes
We have constructed the profiled lines for the three Classes (IIIV) of the nohorizon regular Bardeen and ABG spacetimes. As in the black hole case, we compare the profiled lines for a specific value of the charge parameter of the Bardeen and ABG spacetimes. For the nohorizon spacetimes of the Class III and IV we then demonstrate the role of increasing charge parameter .
Spacetimes with trapped null geodesics
In the case of the Bardeen (ABG) nohorizon spacetimes with (), the profiles of spectral lines take the form demonstrated in Figure 17.
For the small () and large () inclination angles the modifications of the Bardeen and ABG lines relative to the Schwarzschild line have the same character as in the black hole case, being more profound. The profile height is always reduced, the frequency range is increased at the redend and slightly decreased at the blueend for the small inclination, while it is increased at both ends of the frequency range for large inclination. For mediate inclination (), the height of the profiled line increased for the Bardeen spacetime, but decreased for the ABG spacetime, as related to the height of the profiled line in the Schwarzschild spacetime. The frequency range increases at the redend for both the spacetime, while at the blueend it decreases (increases) for the Bardeen (ABG) spacetime. Very precise measurements only could enable distinction of the profiled lines in the Bardeen and ABG spacetimes.
Spacetimes with unstable circular geodesics
In the case of the Bardeen and ABG nohorizon spacetimes with (), the profiled spectral lines are compared in Figure 18. Recall that now the inner edge of the Keplerian discs corresponds to the outer marginally stable orbit again. The influence of increasing spacetime charge parameter is demonstrated in Figure 19.
Now we can conclude that the relative behavior of the Bardeen and ABG profiled lines, and their relation to the Schwarzschild line, are qualitatively the same as in the case of the Class II nohorizon spacetimes, but the differences are slightly magnified in relation to those occurring in the Class II spacetimes and could be observed easily.
We also can see that for the ABG spacetimes increasing of the specific charge parameter makes the profiled lines flatter for all the inclination angles, the height is reduced, while the frequency range expands at both end of the range. In the Bardeen spacetimes, the same statement holds for the small and large inclination angles, while for the mediate inclination () the height increases, while the frequency range decreases at the blueend with increasing. In the case of the nohorizon spacetimes of the Class III the signatures of the spacetimes in the profiled lines could be in principle measurable, but they are of quatitative character only.
Spacetimes allowing only stable circular orbits
In the case of the Bardeen and ABG Class IV spacetimes, with (), the inner edge of the standard (MRI governed) Keplerian disc has to be located at . First, we shall not include the remaining part of the disc, extending down to the static radius. The Bardeen and ABG profiles of lines are compared in Figure 20, while influence of increasing spacetime charge parameter is demonstrated in Figure 21.
For comparison of the profiled lines we use in Figure 20 the common charge parameter , and we observe a significant relative shift of the profiled lines in the Bardeen and ABG spacetimes and their strong modification in comparison to the Schwarzschild profiled lines.
For small inclination, the Bardeen and ABG profiled lines are flatter in comparison to the Schwarzschild line, their height is substantially lowered relative to the Schwarzschild case, their frequency range is similar and nearly equal to the Schwarzschild range at the blueend, but the range is substantially increased at the redend, being much larger for the Bardeen case in comparison to the ABG case. The ABG profiled line has the redend peak only slightly lower than the blueend peak. In the Bardeen spacetime, the difference of the heights of the two peaks is larger than in the ABG spacetime.
For the mediate inclination, the line height is lowered (slightly more in the Bardeen case) relative to the Schwarzschild case. The frequency range of the Bardeen and ABG lines is shifted relative to the Schwarzschild range to lower values at both ends. At the blueend the shift is insignificant, being larger for the ABG line, while its is substantial at redend, being significantly larger for the Bardeen line.
For large inclination, the height of the Bardeen line is significantly reduced in comparison to the height of the Schwarzschild line, while the height of the ABG profiled line is slightly higher and substantially wider than for the Schwarzschild line. The frequency range of the Bardeen and ABG lines is shifted relative to the range of the Schwarzschild line to lower values at the redend (the shift being substantially larger in the Bardeen case), and to the lower (higher) values at the blueend for the ABG (Bardeen) line.
From Figure 21 we can conclude that for both the Bardeen and ABG Class IV nohorizon spacetimes, and for all inclination angles of the Keplerian disc, increasing charge parameter causes substantial modifications of the profiled lines and substantial restriction of their frequency range. In all cases, the changes have even qualitative character for the substantial increasing of the charge parameter to the value of . Then the frequency range of the Bardeen and ABG spacetimes is for all inclinations located inside of the frequency range of the Schwarzschild line. The changes are clearly most profound for large inclination angle when even multipeak profiled lines could be created due to the occurrence of the ghost images. For small inclination, the modifications due to increasing of the charge parameter tend to creation of one peak line in the Bardeen spacetimes, while a narrow line profile with clearly distinguished two peaks is generated in the ABG spacetimes, where this tendency survives for the profiled lines created under mediate inclination of the Keplerian disc.
In Figure 22 we represent for the Bardeen nohorizon spacetime with the input of radiation occuring from the Keplerian disc located under the radius to the profiled spectral lines. We demonstrate that such an input is relevant and observable especially for large inclination angles. The photons coming from significantly amplify the red wing and central region of the profiled line, as they origin in the slowly rotating part of the disc where Doppler shift is suppressed. In the ABG spacetimes the same effects are relevant.
The profiled lines created by Keplerian discs orbiting in the Bardeen and ABG Class IV spacetimes give clearly measurable signatures. For sufficiently large charge parameters () the differences between the Bardeen and ABG profiled lines can be even of qualitative character for all considered inclination angles. Note that such kind of behavior does not occur in the naked singularity KehagiasSfetsos spacetimes of modified Hořava quantum gravity [55].
5.3 Contribution of the ghost images
Finally, we shortly illustrate the role of the radiation incoming from the ghost images to the profile of the spectral lines. Recall that in the nohorizon spacetimes the ghost images are created by a small part of the Keplerian disk near its inner edge, momentarily located just behind the centre of the geometry while being on the line connecting the centre and the observer. The ghost images are created by photons with small impact parameters following almost radial geodesics crossing the nearly flat central region of the nohorizon spacetime – this is the reason why the inclination angle of the observer has to be very large [46]. In the naked singularity spacetimes (of RN or KS type) the photons are repulsed by the central region of the spacetime and the ghost images have different character as demonstrated in [46].
We construct in the relevant cases of the Bardeen spacetimes (with charge parameter large enough to enable creation of the ghost images) and for large inclination angle () necessary for creation of sufficiently large ghost images [46] the profiled lines for the total incoming radiation, and those without the contribution of the ghost images.
We demonstrate in Figure 23 that the role of the ghost images cannot be abandoned, and in some cases could be quite relevant. We can see that the role of the ghost images increases with increasing charge parameter, and its signature is clearly reflected in the innermost peak created in the multipeaked profiled line. The quantitative reflection of the increasing role of the ghost image with the dimensionless charge parameter increasing is reflected by the ratio of the bolometric luminosities represented in Table 3.
6 Conclusions
In the present paper we complete the results of our previous extended study of the optical phenomena in the regular nohorizon spacetimes and nakedsingularity ReissnerNördström spacetimes where attention was concentrated on the so called ghost images [46].
We have constructed the profiled spectral lines in the field of regular black holes of the Bardeen and ABG type, and their ”nohorizon” counterparts, in dependence on the dimensionless charge parameter of the spacetime reflecting fully properties of the spacetime. The influence of the electromagnetic field related to the Bardeen and ABG spacetimes has not be considered.
The nohorizon spacetimes have their astrophysical properties very similar to those found for the first time in the case of the spherically symmetric ReissnerNordstronde Sitter naked singularity spacetimes [50], and recently discussed for the naked singularity spacetimes of the ReissnerNordstrom type related to the Einstein gravity [39], or to the spherically symmetric braneworld black holes [51], and to the KehagiasSfetsos naked singularity spacetimes of the Hořava quantum gravity [56, 62, 55]. For the nohorizon Bardeen and ABG spacetimes, three different regimes of circular geodesics occur in dependence on the parameter [57]. For all three regimes, a ”static sphere” representing the innermost limit on the existence of circular geodesics exists due to some antigravity effects arising near the coordinate origin  therefore, we call it also ”antigravity sphere”. For large values of , stable circular geodesics exist at all radii above the static sphere. For intermediate values of , two regions of stable circular geodesics exist, being separated by a region of unstable circular geodesics. For lowest values of compatible with the nohorizon Bardeen and ABG solutions, an inner region of stable circular geodesics, beginning at the static radius, is limited from above by a stable photon circular geodesics, and an outer region, beginning at ISCO, extends up to infinity. In all cases we have considered as the radiating Keplerian disc the region of the stable circular geodesics where angular frequency of the orbital motion increases with decreasing radius, and the MRI instability governing the Keplerian accretion can work as discussed in [55].
It has been demonstrated that in the case of the regular black hole spacetimes the profiled spectral lines are of the same character as in the Schwarzschild spacetime and the quantitative difference related to the frequency range of the profiled spectral line is generally larger for the ABG black holes than for the Bardeen ones.
Bardeen and ABG nohorizon spacetimes of all these three types of the character of the circular geodesic motion can be distinguished by the behavior of the profiled spectral lines, if the inclination angle to the disc is known. Large differences in the shape and the frequency range of the profiled spectral lines has been demonstrated in the case of the Bardeen and ABG nohorizon spacetimes with large values of the spacetime charge parameter . These differences enable also a clear distinguishing of the Bardeen and ABG nohorizon spacetimes. Moreover, there exist also a clear distinction of the Bardeen and ABG profiled lines, and the profiled lines generated in the KehagiasSfetsos naked singularity spacetimes of the modified Hořava quantum gravity. We expect that recent observational techniques could enable to distinct the regular nohorizon and the naked singularity spacetimes.
Acknowledgements
The authors acknowledge institutional support of the Faculty of Philosophy and Science of the Silesian University at Opava, and the Albert Einstein Centre for Gravitation and Astrophysics supported by the Czech Science Foundation Grant No. 1437086G.
Footnotes
 Notice that ; corresponds to the outer edge of the inner region of the stable orbits, while denotes the inner edge of the outer region of the stable orbits.
 We do not consider the inner Keplerian discs in the case of spacetimes as existence of such discs is improbable from the astrophysical point of view [55].
 We shall not consider here for simplicity the effect of light emitted within the ISCO that can influence spectra and image of accreation discs as shown recently in magnetohydrodynamics calculations. [?, ?, ?]
References
 Abdujabbarov, A., Ahmedov, B., and Hakimov, A., Particle motion around black hole in HořavaLifshitz gravity, Phys. Rev. D, 83, 044053, 2011
 Abdujabbarov, A. and Atamurotov, F. and Kucukakca, Y. and Ahmedov, B. and Camci, U., Shadow of KerrTaubNUT black hole, Astrophys. and Sp. Sci., 344, p.429435, 2013
 Atamurotov, F. and Abdujabbarov, A. and Ahmedov, B., Shadow of rotating HořavaLifshitz black hole, Astrophys. and Sp. Sci., 348, p.179188, 2013
 AyónBeato, E. and García, A., Regular Black Hole in General Relativity Coupled to Nonlinear Electrodynamics, Phys. Rev. Lett., 80, p.50565059, 1998
 AyonBeato, E., New regular black hole solution from nonlinear electrodynamics, Phys. Lett. B, 464, p.25–29, 1999
 AyenBeato, E. and Garcia, A., NonSingular Charged Black Hole Solution for NonLinear Source, Gen. Rel. and Grav., 31, 629, 1999
 AyónBeato, E. and García, A., The Bardeen model as a nonlinear magnetic monopole, Phys. Lett. B, 493, p.149–152, 2000
 AzregAïnou, M., Generating rotating regular black hole solutions without complexification, Phys. Rev. D, 90, 064041, 2014
 Balbus, S. A. and Hawley, J. F., A powerful local shear instability in weakly magnetized disks. I  Linear analysis. II  Nonlinear evolution, Astrophys. J., 376, p.214–233, 1991
 Balbus, S. A. and Hawley, J. F., Instability, turbulence, and enhanced transport in accretion disks, Rev. of Mod. Phys., 70, p.1–53, 1998
 Bambi, C. and Modesto, L., Rotating regular black holes, Phys. Lett. B, 721, p.329334, 2013
 Bao, G. and Stuchlík, Z., Accretion disk selfeclipse  Xray light curve and emission line, Astrophys. J., 400, p.163169, 1992
 Bao, G., Hadrava, P., and Ostgaard, E., Line Profiles from Relativistic Eccentric Rings, Astrophys. J., 464, 684, 1996
 Bardeen, J., presented at GR5, Tbilisi, U.S.S.R., and published in the conference proceedings in the U.S.S.R., 1968.
 Bardeen, J. M., Timelike and null geodesics in the Kerr metric., Black Holes (Les Astres Occlus), editors: Dewitt, C. and Dewitt, B. S. , p.215239, 1973
 Bronnikov, K. A., Comment on “Regular Black Hole in General Relativity Coupled to Nonlinear Electrodynamics”, Phys. Rev. Lett., 85, 4641, 2000
 Bronnikov, K. A., Regular magnetic black holes and monopoles from nonlinear electrodynamics, Phys. Rev. D, 63, 044005, 2001
 Christian, P. and Loeb, A., Probing the spacetime around supermassive black holes with ejected plasma blobs, Phys. Rev. D, 91, 101301, 2015
 Doeleman, S. S., Fish, V. L., Broderick, A. E., Loeb, A., and Rogers, A. E. E., Detecting Flaring Structures in Sagittarius A* with HighFrequency VLBI, Astrophys. Jour., 695, p.5974, 2009
 Fanton, C., Calvani, M., de Felice, F., and Cadez, A., Detecting Accretion Disks in Active Galactic Nuclei, Pub. of the Astro. Soc. of Jap., 49, p.159169, 1997
 García, A., Hackmann, E., Kunz, J., Lämmerzahl, C., and Macías, A., Motion of test particles in a regular black hole spacetime, Jour. of Math. Phys., 56, 032501, 2015
 Ghosh, S. G. and Sheoran, P. and Amir, M., Rotating AyónBeatoGarcía black hole as a particle accelerator, Phys. Rev. D, 90, 103006, 2014
 Ghosh, S. G. and Maharaj, S. D., Radiating Kerrlike regular black hole, Europ. Phys. Jour. C, 75, 7, 2015
 Gwinn, C. R., Kovalev, Y. Y., Johnson, M. D., and Soglasnov, V. A., Discovery of Substructure in the Scatterbroadened Image of Sgr A*, Astrophys. J. Lett., 794, L14, 2014
 Hawking, S. W. and Ellis, G. F. R., The largescale structure of spacetime, Cambridge University Press, 1973
 Hayward, S. A., Formation and Evaporation of Nonsingular Black Holes, Phys. Rev. Lett., 96, 031103, 2006
 Hořava, P., Spectral Dimension of the Universe in Quantum Gravity at a Lifshitz Point, Phys. Rev. Lett., 102, 16, 2009
 Hořava, P., Quantum gravity at a Lifshitz point, Phys. Rev. D, 79, 8, 2009
 Kehagias, A. and Sfetsos, K., The black hole and FRW geometries of nonrelativistic gravity, Phys. Lett. B, 678,p.123126, 2009
 Laor, A., The Spectrum of Massive Thin Accretion Disks: Theory and Observations, Active Galactic Nuclei, IAU Symposium vol 134, editors, Osterbrock, D. E. and Miller, J. S. , p.251, 1989
 Macedo, C. F. B., de Oliveira, E. S., and Crispino, L. C. B., Scattering by regular black holes: Planar massless scalar waves impinging upon a Bardeen black hole, Phys. Rev. D, 92, 024012, 2015
 McClintock, J. E., Narayan, R., Davis, S. W., Gou, L., Kulkarni, A., Orosz, J. A., Penna, R. F., Remillard, R. A., and Steiner, J. F., Measuring the spins of accreting black holes, Class. and Quant. Grav.,28,114009,2011
 Modesto, L. and Nicolini, P., Charged rotating noncommutative black holes, Phys. Rev. D, 82, 104035, 2010
 Neves, J. C. S. and Saa, A., Regular rotating black holes and the weak energy condition, Phys. Lett. B, 734, p.44–48, 2014
 Novikov, I. D. and Thorne, K. S., Astrophysics of black holes, Black Holes (Les Astres Occlus), editors: Dewitt, C. and Dewitt, B. S., p.343450, 1973
 Psaltis, D., Ozel, F., Chan, C.K., and Marrone, D. P., A General Relativistic Null Hypothesis Test with Event Horizon Telescope Observations of the blackhole shadow in Sgr A*, ArXiv eprints, astroph.HE:1411.1454, 2014
 Psaltis, D., Narayan, R., Fish, V. L., Broderick, A. E., Loeb, A., and Doeleman, S. S., Event Horizon Telescope Evidence for Alignment of the Black Hole in the Center of the Milky Way with the Inner Stellar Disk, Astrophys. J., 798, 15, 2015
 Patil, M. and Joshi, P. S., Ultrahigh energy particle collisions in a regular spacetime without black holes or naked singularities, Phys. Rev. D, 86, 044040, 2012
 Pugliese, D. and Quevedo, H. and Ruffini, R., Motion of charged test particles in ReissnerNordström spacetime, Phys. Rev. D, 83, 104052, 2011
 Rauch, K. P. and Blandford, R. D., Optical caustics in a kerr spacetime and the origin of rapid Xray variability in active galactic nuclei, Astrophys. Jour., 421, 46–68, 1994
 Remillard, R. A. and McClintock, J. E., XRay Properties of BlackHole Binaries, Annual Rev. of Astron. & Astrophys., 44,p.49–92, 2006
 Ricarte, A. and Dexter, J., The Event Horizon Telescope: exploring strong gravity and accretion physics, Month. Not. of the Roy. Astr.Soc., 446, p.19731987, 2015
 Schee, J. and Stuchlík, Z., Optical Phenomena in the Field of Braneworld Kerr Black Holes, Int. Jour. of Mod. Phys. D, 18, p.983–1024, 2009
 Schee, J. and Stuchlík, Z., Profiles of emission lines generated by rings orbiting braneworld Kerr black holes, Gen. Rel. and Grav., 41, p.17951818, 2009
 Schee, J. and Stuchlík, Z., Profiled spectral lines generated in the field of Kerr superspinars, Journ. of Cosmolog. and Astropart. Phys., 4, 005, 2013
 Schee, J. and Stuchlík, Z., Gravitational lensing and ghost images in the regular Bardeen nohorizon spacetimes, Jour. of Cosmol. and Astropart. Phys., 6, 048, 2015
 Stuchlík, Z., Equatorial circular orbits and the motion of the shell of dust in the field of a rotating naked singularity. Bull. of the Astronom. Inst. of Czechoslovakia, 31, p.129–144, 1980
 Stuchlik, Z., The motion of test particles in blackhole backgrounds with nonzero cosmological constant, Bull. of the Astron. Inst. of Czechoslovakia, 34, p.129149, 1983
 Stuchlík, Z. and Hledík, S. Equatorial photon motion in the KerrNewman spacetimes with a nonzero cosmological constant, Class. and Quant. Grav., 17, p.45414576, 2000
 Stuchlík, Z. and Hledík, S., Properties of the ReissnerNordstrom spacetimes with a nonzero cosmological constant Acta Phys. Slovac. 52, 363, 2002
 Stuchlík, Z. and Kotrlová, A., Orbital resonances in discs around braneworld Kerr black holes, Gen. Rel. and Grav., 41, p.13051343, 2009
 Stuchlík, Z. and Schee, J., Appearance of Keplerian discs orbiting Kerr superspinars, Class. and Quant. Grav., 27, 215017, 2010
 Stuchlík, Z. and Schee, J., Observational phenomena related to primordial Kerr superspinars, Class. and Quant. Grav., 29, 065002, 2012
 Stuchlík, Z. and Schee, J., Ultrahighenergy collisions in the superspinning Kerr geometry, Class. and Quant. Grav., 30, 075012, 2013
 Stuchlík, Z. and Schee, J., Optical effects related to Keplerian discs orbiting KehagiasSfetsos naked singularities, Class. and Quant. Grav., 31, 195013, 2014
 Stuchlík, Z., Schee, J. and Abdujabbarov, A., Ultrahighenergy collisions of particles in the field of nearextreme KehagiasSfetsos naked singularities and their appearance to distant observers, Phys. Rev. D, 89, 104048, 2014
 Stuchlik, Z. and Schee, J., Circular geodesic of Bardeen and AyonBeatoGarcia regular blackhole and nohorizon spacetimes Accepted in Int. Jour. of Mod. Phys. D, 2015
 Stuchlík, Z. and Slaný, P., Equatorial circular orbits in the Kerr de Sitter spacetimes, Phys. Rev. D, 69, 064001, 2004
 Toshmatov, B., Ahmedov, B., Abdujabbarov, A.,and Stuchlík, Z., Rotating regular black hole solution, Phys. Rev. D, 89, 104017, 2014
 Toshmatov, B., Abdujabbarov, A., Ahmedov, B., and Stuchlík, Z., Particle motion and Penrose processes around rotating regular black hole, Astrophys. and Sp. Sci., 357, 41, 2015
 Toshmatov, B., Abdujabbarov, A., Stuchlík, Z., and Ahmedov, B., Quasinormal modes of test fields around regular black holes, Phys. Rev. D, 91, 083008, 2015
 Vieira, R. S. S., Schee, J., Kluźniak, W., Stuchlík, Z., and Abramowicz, M., Circular geodesics of naked singularities in the KehagiasSfetsos metric of Hořava’s gravity, Phys. Rev. D, 90, 024035, 2014