Physics in the Global Monopole Spacetime

Mello, E. R. Bezerra de

doi:10.1590/s0103-97332001000200012

Cited by 55 publications

(65 citation statements)

References 7 publications

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“…The global monopole spacetime is characterized by a line element that possesses a parameter related to the deficit angle δΩ = 8π 2 Gη 2 0 , with η 0 being the dimensionless volumetric mass density of the pointlike global monopole and G is the gravitational Newton constant, and with the scalar curvature R = R µ µ = 2 (1−α 2 ) r 2 . By working with the units c = = 1 and the signature (−, +, +, +), the line element of the pointlike global monopole spacetime is written in the form [27]:…”

Section: Do In the Global Monopole Spacetimementioning

confidence: 99%

“…are indices corresponding to the Minkowski spacetime. We consider the following choice for the tetrad base in the pointlike global monopole spacetime (1) [27]:…”

Section: Do In the Global Monopole Spacetimementioning

confidence: 99%

“…In this case, the energy spectrum of the system is influenced by the defect [24], in a charged particle-magnetic monopole scattering [25] and on the harmonic oscillator [26]. For the relativistic case, there are studies on the hydrogen atom and pionic atom [27], on the exact solutions of scalar bosons in the presence of the Aharonov-Bohm and Coulomb potentials [28]. In addition, the exact solutions of the Klein Gordon equation in the presence of a dyon, magnetic flux and scalar potential [29] also have been analyzed in the nonrelativistic context.…”

Section: Introductionmentioning

confidence: 99%

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Relativistic quantum oscillators in the global monopole spacetime

et al. 2020

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We investigated the effects of the global monopole spacetime on the Dirac and Klein-Gordon relativistic quantum oscillators. In order to do this, we solve the Dirac and Klein-Gordon equations analytically and discuss the influence of this background which is characterized by the curvature of the spacetime on the energy profiles of these oscillators. In addition, we introduce a hard-wall potential and, for a particular case, determine the energy spectrum for relativistic quantum oscillators in this background.

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Section: Do In the Global Monopole Spacetimementioning

confidence: 99%

“…are indices corresponding to the Minkowski spacetime. We consider the following choice for the tetrad base in the pointlike global monopole spacetime (1) [27]:…”

Section: Do In the Global Monopole Spacetimementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Relativistic quantum oscillators in the global monopole spacetime

et al. 2020

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“…We will numerically calculate this corrected potential regarding typical neutron stars and the Sun, comparing them with the situation in the flat spacetime. We will also calculate the black-body potential due to the global monopole, whose major feature is the deficit in the central solid angle of the metric generated by that object, modifying its topology [4,5]. We will show that the difference from the flat spacetime black-body potential, different from the previous situation, grows with the distance to the source center.…”

Section: Introductionmentioning

confidence: 98%

Dependence of the black-body force on spacetime geometry and topology

Muniz¹,

Alencar²,

Cunha³

et al. 2017

EPL

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In this paper we compute the corrections to the black-body force (BBF) potential due to spacetime geometry and topology. This recently discovered attractive force on neutral atoms is caused by the thermal radiation emitted from black bodies and here we investigate it in relativistic gravitational systems with spherical and cylindrical symmetries. For some astrophysical objects we find that the corrected black-body potential is greater than the flat case, showing that this kind of correction can be quite relevant when curved spaces are considered. Then we consider four cases: The Schwarzschild spacetime, the global monopole, the non-relativistic infinity cylinder and the static cosmic string. For the spherically symmetric case of a massive body, we find that two corrections appear: One due to the gravitational modification of the temperature and the other due to the modification of the solid angle subtended by the atom. We apply the found results to a typical neutron star and to the Sun. For the global monopole, the modification in the black-body potential is of topological nature and it is due to the central solid angle deficit that occurs in the spacetime generated by that object. In the cylindrical case, which is locally flat, no gravitational correction to the temperature exists, as in the global monopole case. However, we find the curious fact that the BBF depends on the topology of the spacetime through the modification of the azimuthal angle and therefore of the solid angle. For the static cosmic string we find that the force is null for the zero thickness case.

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“…This metric describes a spacetime with a deficit solid angle (the section θ = π/2 coresponds to a cone with deficit angle ∆ = 8π 2 Gη 2 ). The spacetime is not flat, being characterized by the curvature scalar R = 2 α −2 − 1 r −2 [4]. The energy density, determined by the 00-th component of the stress-energymomentum tensor T µν , is given by T 00 ∼ Gη 2 /r 2 so that the total energy E(r) ∼ 4πGη 2 r is linearly divergent for large r. Despite the fact that the Ricci scalar goes to zero when r → ∞, the global monopole is not asymptotically * pitelli@ime.unicamp.br † barrosov@ifi.unicamp.br ‡ mauricio.richartz@ufabc.edu.br flat since there are non-zero components of the Riemann curvature tensor R ρσµν for arbitrarily large r. In particular, the R θφθφ = 1 − α 2 sin 2 θ component is non-zero if α = 1.…”

Section: Introductionmentioning

confidence: 99%

Scattering cross section and stability of global monopoles

2017

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We study the scattering of scalar waves propagating on the global monopole background. Since the scalar wave operator in this topological defect is not essentially self-adjoint, its solutions are not uniquely determined until a boundary condition at the origin is specified. As we show, this boundary condition manifests itself in the differential cross section and can be inferred by measuring the amplitude of the backscattered wave. We further demonstrate that whether or not the spacetime is stable under scalar perturbations also relies on the chosen boundary condition. In particular, we identify a class of such boundary conditions which significantly affects the differential cross section without introducing an instability.

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Physics in the Global Monopole Spacetime

Cited by 55 publications

References 7 publications

Relativistic quantum oscillators in the global monopole spacetime

Relativistic quantum oscillators in the global monopole spacetime

Dependence of the black-body force on spacetime geometry and topology

Scattering cross section and stability of global monopoles

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