Super-spinning compact objects and models of high-frequency quasi-periodic oscillations observed in Galactic microquasars. II. Forced resonances
In our previous work (Paper I) we applied several models of high-frequency quasi-periodic oscillations (HF QPOs) to estimate the spin of the central compact object in three Galactic microquasars assuming the possibility that the central compact body is a super-spinning object (or a naked singularity...
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| creator | Kotrlová, Andrea Šrámková, Eva Török, Gabriel Stuchlík, Zdeněk Goluchová, Kateřina |
| description | In our previous work (Paper I) we applied several models of high-frequency quasi-periodic oscillations (HF QPOs) to estimate the spin of the central compact object in three Galactic microquasars assuming the possibility that the central compact body is a super-spinning object (or a naked singularity) with external spacetime described by Kerr geometry with a dimensionless spin parameter \(a\equiv cJ/GM^2>1\). Here we extend our consideration, and in a consistent way investigate implications of a set of ten resonance models so far discussed only in the context of \(a |
| doi_str_mv | 10.48550/arxiv.1708.04300 |
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II. Forced resonances</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Kotrlová, Andrea ; Šrámková, Eva ; Török, Gabriel ; Stuchlík, Zdeněk ; Goluchová, Kateřina</creator><creatorcontrib>Kotrlová, Andrea ; Šrámková, Eva ; Török, Gabriel ; Stuchlík, Zdeněk ; Goluchová, Kateřina</creatorcontrib><description>In our previous work (Paper I) we applied several models of high-frequency quasi-periodic oscillations (HF QPOs) to estimate the spin of the central compact object in three Galactic microquasars assuming the possibility that the central compact body is a super-spinning object (or a naked singularity) with external spacetime described by Kerr geometry with a dimensionless spin parameter \(a\equiv cJ/GM^2>1\). Here we extend our consideration, and in a consistent way investigate implications of a set of ten resonance models so far discussed only in the context of \(a<1\). The same physical arguments as in Paper I are applied to these models, i.e. only a small deviation of the spin estimate from \(a=1\), \(a\gtrsim 1\), is assumed for a favoured model. For five of these models that involve Keplerian and radial epicyclic oscillations we find the existence of a unique specific QPO excitation radius. Consequently, there is a simple behaviour of dimensionless frequency \(M\times\nu_{U}(a)\) represented by a single continuous function having solely one maximum close to \(a\gtrsim1\). Only one of these models is compatible with the expectation of \(a\gtrsim 1\). The other five models that involve the radial and vertical epicyclic oscillations imply the existence of multiple resonant radii. This signifies a more complicated behaviour of \(M\times\nu_{U}(a)\) that cannot be represented by single functions. 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II. Forced resonances</title><title>arXiv.org</title><description>In our previous work (Paper I) we applied several models of high-frequency quasi-periodic oscillations (HF QPOs) to estimate the spin of the central compact object in three Galactic microquasars assuming the possibility that the central compact body is a super-spinning object (or a naked singularity) with external spacetime described by Kerr geometry with a dimensionless spin parameter \(a\equiv cJ/GM^2>1\). Here we extend our consideration, and in a consistent way investigate implications of a set of ten resonance models so far discussed only in the context of \(a<1\). The same physical arguments as in Paper I are applied to these models, i.e. only a small deviation of the spin estimate from \(a=1\), \(a\gtrsim 1\), is assumed for a favoured model. For five of these models that involve Keplerian and radial epicyclic oscillations we find the existence of a unique specific QPO excitation radius. Consequently, there is a simple behaviour of dimensionless frequency \(M\times\nu_{U}(a)\) represented by a single continuous function having solely one maximum close to \(a\gtrsim1\). Only one of these models is compatible with the expectation of \(a\gtrsim 1\). The other five models that involve the radial and vertical epicyclic oscillations imply the existence of multiple resonant radii. This signifies a more complicated behaviour of \(M\times\nu_{U}(a)\) that cannot be represented by single functions. 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For five of these models that involve Keplerian and radial epicyclic oscillations we find the existence of a unique specific QPO excitation radius. Consequently, there is a simple behaviour of dimensionless frequency \(M\times\nu_{U}(a)\) represented by a single continuous function having solely one maximum close to \(a\gtrsim1\). Only one of these models is compatible with the expectation of \(a\gtrsim 1\). The other five models that involve the radial and vertical epicyclic oscillations imply the existence of multiple resonant radii. This signifies a more complicated behaviour of \(M\times\nu_{U}(a)\) that cannot be represented by single functions. Each of these five models is compatible with the expectation of \(a\gtrsim 1\).</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1708.04300</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Astronomical models Continuity (mathematics) Microquasars Physics - High Energy Astrophysical Phenomena Quasi-Periodic Oscillations Vertical oscillations |
| title | Super-spinning compact objects and models of high-frequency quasi-periodic oscillations observed in Galactic microquasars. II. Forced resonances |
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