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^{μ ν}rather than the metric tensor g

_{μ ν}. The corresponding Lagrangian function, denoted as L

_{R}, is realized by a polynomial expression of the Ricci 4-scalar R ≡g

_{μ ν}R

^{μ ν}and of the quadratic curvature 4-scalar ρ ≡R

^{μ ν}R

_{μ ν}. The Lagrangian variational principle applies both to vacuum and non-vacuum cases and for its validity it demands a non-vanishing, and actually also positive, cosmological constant Λ >0 . Then, by implementing the deDonder-Weyl formalism, the physical conditions for the existence of a manifestly-covariant Hamiltonian structure associated with such a Lagrangian formulation are investigated. As a consequence, it is proved that the Ricci tensor can obey a Hamiltonian dynamics which is consistent with the solutions predicted by the Einstein field equations.

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_{q}, namely (i) ω

_{q}=-1 /3 , (ii) ω

_{q}=-1 , and (iii) ω

_{q}=-2 /3 , and for different values of the normalization factor α and electric charge Q of the black hole. It is found that the presence of the quintessence field shifts outward the innermost stable circular orbits (ISCOs) around the Kiselev black hole, having the same charge parameter Q , as compared to the ISCOs around a Riessner-Nordstrom black hole, while the effect of the quintessence field on the outermost stable circular orbits (OSCOs) is just opposite to that on the ISCOs. Further, the radii of the photon circular orbits are also calculated for different ranges of the parameters α and Q . It is observed that the photon orbits are also shifted outward as the value of α increases. The radial and latitudinal epicyclic motion of test particles, which can be related to the quasiperiodic oscillations of test particles slightly above the MSCOs in the vicinity of the charged Kiselev black hole, is analyzed for the three different values of ω

_{q}. It is seen that the azimuthal and latitudinal frequencies coincide, and the radial epicyclic frequency is different in dependence on the spacetime parameters. In the case of ω

_{q}=-1 /3 , the azimuthal and latitudinal frequencies depend on the radial position r of the particle, the charge Q , and the mass M of the black hole, and do not depend on the factor α . However, for ω

_{q}=-2 /3 and ω

_{q}=-1 , these two frequencies, along with the black hole parameters—i.e., M and Q and the radial position r —also depend on the factor α . The radial epicyclic frequency for all the values of ω

_{q}depends on M , Q , r , and also on the normalization factor α . We also compare the epicyclic frequencies with that for an uncharged black hole. With the increase of electric charge, the ISCO becomes closer to the central object, and one can observe epicyclic frequencies closer to the central object, which makes the epicyclic frequencies larger. The ISCO gets larger as α increases, and thus the epicyclic frequencies can be observed away from the central object and would be smaller as compared to the case of a pure Riessner-Nordstrom black hole without quintessence. As the effect of the parameters Q and α on the OSCOs is just opposite to that on the ISCOs, the epicyclic frequencies near the OSCOs behave the other way around.

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_{e}(Q

_{m}), and scalar charge C (or n parameter) of the gravitational compact object. It is also shown that dual solution for the vector potential A

_{ϕ}=Q

_{m}cos θ is satisfied by the EMS field equations and the electric charge can be safely replaced by magnetic charge Q

_{m}. Finally, we have studied curvature invariants and test particle motion around the gravitational source described the obtained new spacetime metric. We have also provided analysis of degeneracy values of spin parameter of the rotating Kerr black hole and charge parameter of compact object described by the new spacetime metric through comparison of radii of ISCO, photonsphere and energy efficiency. It is shown that new black hole solution in Einstein-Maxwell-scalar field theory can mimic spin parameter of the Kerr black hole up to a

_{∗}≲ 0 . 6 while the astrophysical black hole' observations that it reaches up to a

_{∗}≲ 0 . 99 . Consequently, one may conclude that the obtained new black hole solution can be considered as realistic candidate for the astrophysical black holes with a

_{∗}≲ 0 . 6 .

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