Charged Massive Scalar Field Research Articles

CASIMIR ENERGY AND FORCE INDUCED BY AN IMPENETRABLE FLUX TUBE OF FINITE RADIUS

A perfectly reflecting (Dirichlet) boundary condition at the edge of an impenetrable magnetic-flux-carrying tube of nonzero transverse size is imposed on the charged massive scalar matter field which is quantized outside the tube. We show that the vacuum polarization effects outside the tube give rise to a macroscopic force acting at the increase of the tube radius (if the magnetic flux is held steady). The Casimir energy and force are periodic in the value of the magnetic flux, being independent of the coupling to the space–time curvature scalar. We conclude that a topological defect of the vortex type can polarize the vacuum of only those quantum fields that have masses which are much less than a scale of the spontaneous symmetry breaking.

Phase transition to a hairy black hole in asymptotically flat spacetime

We discuss a phase transition of a Reissner-Nordström black hole to a hairy black hole in asymptotically flat spacetime. The hair is due to a massive charged scalar field. The no-hair theorem is evaded thanks to a derivative coupling of the scalar field to the Einstein tensor. The resulting hairy configuration is spherically symmetric. We solve the equations analytically near the transition temperature and show that the hair is concentrated near the horizon decaying exponentially away from it.

Massive charged scalar field in the Kerr-Newman background: Quasinormal modes, late-time tails and stability

So far analysis of the quasinormal spectrum of a massive charged scalar field in the black hole background has been limited by the regime of small \mu M and qQ, where \mu, q (M, Q) are mass and charge of the field (black hole). Here we shall present a comprehensive picture of quasinormal modes, late-time tails and stability of a massive charged scalar field around Kerr-Newman black holes for any physically meaningful values of the parameters. We shall show that despite presence of the two mechanisms of superradiance (owing to black hole's rotation and charge) and the massive term creating growing bound states, there is no indication of instability under quasinormal modes' boundary conditions. We have shown that for some moderate values of qQ dominant quasinormal modes may have arbitrarily small real oscillation frequencies Re(\omega). An analytic formula for the quasinormal modes has been derived in the regime of large qQ. The larger the field's charge, the sooner asymptotic tails dominate in a signal, making it difficult to extract quasinormal frequencies from a time-domain profile. Analytic expressions for intermediate and asymptotically late-time tails have been found for the Reissner-Nordstr\"om black hole. For the near extremal Kerr-Newman black holes we have obtained a more general picture of the mode branching found recently for massless fields [arXiv:1212.3271] in the Kerr background.

Charged Quasinormal Modes and Dynamical Property of Black Hole with Global Monopole in de Sitter Spacetime

According to the basic rules of finite difference method,we calculate massive charged scalar field quasinormal modes of Reissner-Nordstrom-de Sitter Black Hole with a global monopole, which shows that when electronic quantity of scalar field e is comparatively small, all the factors including angular quantum number, the mass of scalar field, the size of horizon and the breaking scale will influence the frequency spectrum of quasinormal modes. When e is more than some definite critical value, second-order transition will appear and after that the curve of frequency spectrum rises, the black hole is no longer steady, which means when e is greater than some definite critical value, the structure of black hole can be changed. While the size of angular quantum number and breaking scale will influence the happening time of second-order transition. When breaking scale is less than some definite critical value, the second-order transition can be vanished.

Superradiant instability of charged massive scalar field in Kerr–Newman–anti-de Sitter black hole

We study the superradiance instability of charged massive scalar field in the background of Kerr–Newman–anti-de Sitter black hole. By employing the asymptotic matching technique to solve Klein–Gordon equation analytically, the complex parts of quasinormal frequencies are shown to be positive in the regime of superradiance. Because the calculation is performed in the approximation of small black hole, the result indicates that small Kerr–Newman–anti-de Sitter black hole is unstable against the massive scalar field perturbation with small charge.

VACUUM ENERGY INDUCED BY AN IMPENETRABLE FLUX TUBE OF FINITE RADIUS

We consider the effect of the magnetic field background in the form of a tube of the finite transverse size on the vacuum of the quantized charged massive scalar field which is subject to the Dirichlet boundary condition at the edge of the tube. The vacuum energy is induced, being periodic in the value of the magnetic flux enclosed in the tube. The dependence of the vacuum energy density on the distance from the tube and on the coupling to the space-time curvature scalar is comprehensively analyzed.

Quasinormal modes, scattering, and Hawking radiation of Kerr-Newman black holes in a magnetic field

We perform a comprehensive analysis of the spectrum of proper oscillations (quasinormal modes), transmission/reflection coefficients and Hawking radiation for a massive charged scalar field in the background of the Kerr-Newman black hole immersed in an asymptotically homogeneous magnetic field. There are two main effects: the Zeeman shift of the particle energy in the magnetic field and the difference of values of an electromagnetic potential between the horizon and infinity, i.e. the Faraday induction. We have shown that "turning on" the magnetic field induces a stronger energy-emission rate and leads to "recharging" of the black hole. Thus, a black hole immersed in a magnetic field evaporates much quicker, achieving thereby an extremal state in a shorter period of time. Quasinormal modes are moderately affected by the presence of a magnetic field which is assumed to be relatively small compared to the gravitational field of the black hole.

CASIMIR-AHARONOV-BOHM EFFECT IN THE COSMIC STRING BACKGROUND

A charged massive scalar field is quantized in the background of a static gauge cosmic string. We find the energy-momentum tensor which is induced in the vacuum. The dependence of the tensor components on the gauge flux, string tension and the coupling to the space-time curvature is comprehensively analyzed.

VACUUM ENERGY INDUCED BY AN IMPENETRABLE FLUX TUBE OF FINITE RADIUS

We consider the effect of the magnetic field background in the form of a tube of the finite transverse size on the vacuum of the quantized charged massive scalar field which is subject to the Dirichlet boundary condition at the edge of the tube. The vacuum energy is induced, being periodic in the value of the magnetic flux enclosed in the tube. The dependence of the vacuum energy density on the distance from the tube and on the coupling to the space-time curvature scalar is comprehensively analyzed.

Phase transitions and regions of stability in Reissner-Nordström holographic superconductors

The phase transition of Reissner-Nordstrom AdS_4 interacting with a massive charged scalar field has been further revisited. We found exactly one stable and one unstable quasinormal mode regions for the scalar field. The two of them are separated by the first marginally stable solution.

Polarization of the vacuum of a quantized scalar field by an impenetrable magnetic vortex of finite thickness

We consider the effect of the magnetic field background in the form of a tube of the finite transverse size on the vacuum of the quantized charged massive scalar field which is subject to the Dirichlet boundary condition at the tube. It is shown that if the Compton wavelength associated with the scalar field considerably exceeds the transverse size of the tube, then the vacuum energy which is finite and periodic in the value of the magnetic flux enclosed in the tube is induced on a plane transverse to the tube. Some consequences for generic features of the vacuum polarization in the cosmic-string background are discussed.

Exact solutions to a massive charged scalar field equation in the magnetically charged stringy black-hole geometry and Hawking radiation

Exact solutions of a massive complex scalar field equation in the geometry of a Garfinkle–Horowitz–Strominger (stringy) black hole with magnetic charge is explored. The separated radial and angular parts of the wave equation are solved exactly in the nonextreme case. The angular part is shown to be an ordinary spin-weighted spheroidal harmonics with a spin-weight depending on the magnetic charge. The radial part is achieved to reduce a confluent Heun equation with a multiplier. Finally, based on the solutions, it is shown that the Hawking temperature of the magnetically charged stringy black hole has the same value as that of the Schwarzschild black hole.

Massive Charged Quasinormal Modes of a Reissner-Nordström Black Hole

Using the WKB method and HYBRD program, we evaluate the low-lying massive charged scalar and Dirac field quasinormal modes (QNMs) of a Reissner-Nordstrom black hole. We discuss the real and imaginary parts of QNMs vary with the charge of black hole, the masses and charges of scalar and Dirac fields.

Semiclassical gravitational effects near a singular magnetic flux

We consider the backreaction of the vacuum polarization effect for a massive charged scalar field in the presence of a singular magnetic massless string on the background metric. Using semiclassical approach, we find the first-order (in ℏ units) metric modifications and the corresponding gravitational potential and deficit angle. It is shown that, in certain region of values of coupling constant and magnetic flux, the gravitational potential and deficit angle can be positive as well as negative over all distances from the string and can even change its sign. Unlike the case of massless scalar field, the gravitational corrections were found to have short-range behavior.

Instability of Massive Scalar Fields in Kerr-Newman Spacetime

We investigate the instability of charged massive scalar fields in Kerr-Newman spacetime. Due to the super-radiant effect of the background geometry, the bound state of the scalar field is unstable, and its amplitude grows in time. By solving the Klein-Gordon equation of the scalar field as an eigenvalue problem, we numerically obtain the growth rate of the amplitude of the scalar field. Although the dependence of the scalar field mass and the scalar field charge on this growth rate agrees with the result of the analytic approximation, the maximum value of the growth rate is three times larger than that of the analytic approximation. We also discuss the effect of the electric charge on the instability of the scalar field.

Effective field theory and unification in AdS backgrounds

This work is an extension of our previous work, hep-th/0204160, which showed how to systematically calculate the high energy evolution of gauge couplings in compact AdS_5 backgrounds. We first directly compute the one-loop effects of massive charged scalar fields on the low energy couplings of a gauge theory propagating in the AdS background. It is found that scalar bulk mass scales (which generically are of order the Planck scale) enter only logarithmically in the corrections to the tree-level gauge couplings. As we pointed out previously, we show that the large logarithms that appear in the AdS one-loop calculation can be obtained within the confines of an effective field theory, by running the Planck brane correlator from a high UV matching scale down to the TeV scale. This result exactly reproduces our previous calculation, which was based on AdS/CFT duality. We also calculate the effects of scalar fields satisfying non-trivial boundary conditions (relevant for orbifold breaking of bulk symmetries) on the running of gauge couplings.

On ``Time-Periodic' Black-Hole Solutions to Certain Spherically Symmetric Einstein-Matter Systems

This paper explores black hole solutions of various Einstein-wave matter systems admitting a time-orientation preserving isometry of their domain of outer communications taking some point to its future. In the first two parts, it is shown that such solutions, assuming in addition that they are spherically symmetric and the matter has a certain structure, must be Schwarzschild or Reissner-Nordström. Non-trivial examples of matter for which the result applies are a wave map and a massive charged scalar field interacting with an electromagnetic field. The results thus generalize work of Bekenstein [1] and Heusler [13] from the static to the periodic case. In the third part, which is independent of the first two, it is shown that Dirac fields preserved by an isometry of a spherically symmetric domain of outer communications of the type described above must vanish. It can be applied in particular to the Einstein-Dirac-Maxwell equations or the Einstein-Dirac-Yang/Mills equations, generalizing work of Finster, Smoller and Yau [10, 8, 9 and also 7].

Massive charged scalar field in a Reissner–Nordstrom black hole background: quasinormal ringing

We compute characteristic (quasinormal) frequencies corresponding to decay of a massive charged scalar field in a Reissner–Nordstrom black hole background. It proves that, contrary to the behavior at very late times, at the stage of quasinormal ringing the neutral perturbations will damp slower than the charged ones. In the limit of the extremal black hole the damping rate of charged and neutral perturbations coincides. Possible connection of this with the critical collapse in a massive scalar electrodynamics is discussed.

Confined quantum fields under the influence of a uniform magnetic field

We investigate the influence of a uniform magnetic field on the zero-point energy of charged fields of two types, namely, a massive charged scalar field under Dirichlet boundary conditions and a massive fermion field under MIT boundary conditions. For the first, exact results are obtained, in terms of exponentially convergent functions, and for the second, the limits for small and for large masses are analytically obtained also. Coincidence with previously known, partial results serves as a check of the procedure. For the general case in the second situation—a rather involved one—a precise numerical analysis is performed.

Exact solutions to sourceless charged massive scalar field equation on Kerr–Newman background

The covariant Klein–Gordon equation in the Kerr–Newman black hole geometry is separated into a radial part and an angular part. It is discovered that in the nonextreme case, these two equations belong to a generalized spin-weighted spheroidal wave equation. Then general exact solutions in integral forms and several special solutions with physical interest are given. While in the extreme case, the radial equation can be transformed into a generalized Whittaker–Hill equation. In both cases, five-term recurrence relations between coefficients in power series expansion of general solutions are presented. Finally, the connection between the radial equations in both cases is discussed.