Channeling of protons through radial deformed carbon nanotubes

Jovanović, V. Borka; Borka, D.; Galijaš, S.M.D.

doi:10.1016/j.physleta.2017.03.029

Cited by 10 publications

(11 citation statements)

References 39 publications

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“…time) at which, here a simulation and in reality an observation, is made. Moreover, as demonstrated in Jovanović et al (2014), the mass ratio q also has a strong influence on the amplitudes of these ripples, since the ratio between the fractions of the composite Fe Kα line flux, contributed by the accretion disks around the secondary and the primary, roughly corresponds to q. Since a highly inclined disk produces a wide line profile, as demonstrated in Fig.…”

Section: Resultsmentioning

confidence: 75%

“…Due to several effects, photons emitted from a disk at energy E em (or wavelength λ em ) will be observed by an observer at infinity at energy E obs (or wavelength λ obs ), causing the energy shift g or, equivalently, the usual redshift in wavelength z (for more details see e.g. Jovanović et al, 2016, and references therein):…”

Section: Accretion Disk Modelsmentioning

confidence: 99%

“…Popović, 2012;Bon et al, 2012;Li et al, 2016, for examples in optical band). In such a case, a strong X-ray emission in the broad Fe Kα line at 6.4 keV could arise from accretion disks around both SMBHs, and could be therefore affected by the Doppler shifts due to the orbital motion of the binary (Yu and Lu, 2001;Jovanović et al, 2014), since the radial velocities of its components could reach ≈ 1.5 × 10 4 km/s in the case when the separation between them is 10 −3 − 10 −2 pc (see Table 1 in Popović, 2012). Such, double relativistic Fe Kα lines and periodic X-ray variability are expected to be detected from very massive (M > 10 8 M ⊙ ) and cosmologically nearby (z cosm < 1) SMBHBs (Sesana et al, 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Jovanović et al, 2008;Jovanović & Popović, 2009;Jovanović, 2012;Popović, 2012), as well as the masses and spins of SMBHs (see e.g. Jovanović et al, 2011;Reynolds, 2014). X-ray reflection spectroscopy, which is based on the studies of the observed broad Fe Kα line profiles, is nowadays proven to be an especially powerful technique for the robust black hole spin measurements across the wide range of black hole masses, from the stellar-mass black holes in the X-ray binaries to the SMBHs in the Active Galactic Nuclei (AGN), as well as for the reverberation of the relativistically broadened iron line which is already detected in the observed X-ray spectra of some AGN (for more details see the review by Reynolds (2014), and references therein).…”

Section: Introductionmentioning

confidence: 99%

“…In the case of SMBHBs, the line emitting regions could have different structures, depending on the mass ratios of the components, separation between them and parameters of their accretion disks (Jovanović et al, 2014). In some cases the secondary SMBH could be even embedded in the accretion disk around the primary, causing an empty annular gap in it (McKernan et al, 2013), similarly to the empty gap in circumbinary disk of Mrk 231 (see Fig.…”

Section: Introductionmentioning

confidence: 99%

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Possible observational signatures of supermassive black hole binaries in their Fe Kα line profiles

Jovanović¹,

Jovanović²,

Borka³

2020

caosp

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Here we study the potential observational signatures of supermassive black hole binaries (SMBHBs) in the Fe Kα line profiles emitted from the accretion disks around their components. We simulated the Fe Kα line emission from the relativistic accretion disks using ray tracing method in Kerr metric. The obtained profiles from the SMBHBs are then compared with those in the case of the single supermassive black holes (SMBHs). We considered two models of the SMBHBs: a model when the secondary SMBH is embedded in the accretion disk around the primary, causing an empty gap in the disk, and a model with clearly separated components, where the accretion disks around both primary and secondary give a significant contribution to the composite Fe Kα line emission of a such SMBHB. The obtained results showed that both models of SMBHBs can leave imprints in the form of ripples in the cores of the emitted Fe Kα line profiles, which may look like an absorption component in the line profile. However, in the case of the composite line profiles emitted from two accretion disks, these ripples could have much higher amplitudes and strongly depend on orbital phase of the system, while for those emitted from a disk with an empty gap, the corresponding ripples mostly have lower amplitudes and do not vary significantly with orbital phase. The present day X-ray telescopes are not able to detect such signatures in the observed X-ray spectra of SMBHBs. However this will be possible with the next generation of X-ray observatories, which will also enable application of such effects as a tool for studying the properties of these objects.

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Section: Resultsmentioning

confidence: 75%

Section: Accretion Disk Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Possible observational signatures of supermassive black hole binaries in their Fe Kα line profiles

Jovanović¹,

Jovanović²,

Borka³

2020

caosp

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Gravitational redshift of emission lines in the AGN spectra

Bon

Marziani

et al. 2015

Astrophys Space Sci

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The detection of gravitationally redshifted optical emission lines has been reported just for a few active galaxies. In this paper we give a short overview of studies that analyzed or exploited the detection of the gravitational redshift in optical AGN spectra. In addition, we tested the consistency of gravitational redshift as the physical origin of the redward shifts observed in their spectra using a sample of ≈ 50 Hamburg-ESO intermediate to high redshift quasars that are among the most luminous quasars known (10 47 < ∼ L < ∼ 10 48 erg/s), and are expected to host very massive black holes. To this aim we modeled the line profile with accretion disk models around a black hole.

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