scholarly journals Slowly damped quasinormal modes of the massive Dirac field in d -dimensional Tangherlini spacetime

2018 ◽  
Vol 97 (4) ◽  
Author(s):  
Jose Luis Blázquez-Salcedo ◽  
Christian Knoll
Keyword(s):  
Quasinormal Modes ◽  
Dirac Field ◽  
Massive Dirac Field

scholarly journals QUASINORMAL MODES AND STABILITY OF A FIVE-DIMENSIONAL DILATONIC BLACK HOLE

2009 ◽  
Vol 18 (09) ◽  
pp. 1441-1459 ◽  
Author(s):  
A. LÓPEZ-ORTEGA
Keyword(s):  
Black Hole ◽  
Linear Stability ◽  
Quasinormal Modes ◽  
Dirac Field ◽  
Dimensional Black Hole ◽  
Klein Gordon ◽  
Dilatonic Black Hole ◽  
Massive Dirac Field

We exactly calculate the quasinormal frequencies of the electromagnetic and Klein–Gordon perturbations propagating in a five-dimensional dilatonic black hole. Furthermore, we exactly find the quasinormal frequencies of the massive Dirac field. Using these results we study the linear stability of this black hole. We compare our results for the quasinormal frequencies and for the linear stability of the five-dimensional black hole with those already published.

scholarly journals QUASINORMAL MODES OF RN BLACK HOLE SPACETIME WITH COSMIC STRING IN A DIRAC FIELD

2009 ◽  
Vol 24 (25) ◽  
pp. 2025-2037 ◽  
Author(s):  
R. SINI ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
Cosmic String ◽  
Quasinormal Modes ◽  
Potential Method ◽  
Dirac Field ◽  
Black Hole Spacetimes ◽  
Black Hole Spacetime ◽  
Field Decay ◽  
Positively Charged ◽  
Small Charge

We evaluate quasinormal mode frequencies for RN black hole spacetimes with cosmic string perturbed by a massless Dirac field, using Pöschl–Teller potential method. We find that only in the case of RN black hole having small charge, the effect due to cosmic string will dominate when perturbed by a negatively charged Dirac field, but if we are perturbing with positively charged Dirac field decay will be less in the case of black hole having cosmic string compared to the RN black hole without string.

Massive Dirac field in 3D and induced equations for higher spin fields

2017 ◽  
pp. 293-298 ◽  
Author(s):  
L. Bonora ◽  
M. Cvitan ◽  
P. Dominis Prester ◽  
S. Giaccari ◽  
B. Lima de Souza ◽  
...  
Keyword(s):  
Dirac Field ◽  
Higher Spin ◽  
Spin Fields ◽  
Massive Dirac Field ◽  
Higher Spin Fields

scholarly journals DECAY OF SPIN-1/2 FIELD AROUND REISSNER–NORDSTROM BLACK HOLE

2004 ◽  
Vol 13 (06) ◽  
pp. 1105-1118 ◽  
Author(s):  
WEI ZHOU ◽  
JIAN-YANG ZHU
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Quantum Number ◽  
Turning Point ◽  
Quasinormal Modes ◽  
Astronomical Observation ◽  
Dirac Field ◽  
Neutrino Field ◽  
Extremal Limit ◽  
Field Decay

To find what influence the charge of the black hole Q will bring to the evolution of the quasinormal modes, we calculate the quasinormal frequencies of the neutrino field (charge e=0) perturbations and those of the massless Dirac field (e≠0) perturbations in the RN metric. The influences of Q, e, the momentum quantum number l, and the mode number n are discussed. Among the conclusions, the most important one is that, at the stage of quasinormal ringing, when the black hole and the field have the same kind of charge (eQ>0), the quasinormal modes of the massless charged Dirac field decay faster than those of the neutral ones, and when eQ<0, the massless charged Dirac field decays slower, which may be helpful in the astronomical observation. In addition, we compare the influence from the charge of the black hole to the spin 1/2 field and scalar field perturbations including the extremal limit (M=Q) and find a turning point of Q exists in both cases. The explanation of this fact is unclear with some suggestions that may be helpful are given.

EFFECT OF COSMIC STRING IN SPHERICALLY SYMMETRIC BLACK HOLE ON THE DIRAC PERTURBATION

2010 ◽  
Vol 25 (02) ◽  
pp. 111-124 ◽  
Author(s):  
R. SINI ◽  
NIJO VARGHESE ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
Cosmic String ◽  
Oscillation Frequency ◽  
Quasinormal Modes ◽  
Dirac Field ◽  
Spherically Symmetric ◽  
Black Hole Spacetimes ◽  
Quasi Normal Mode ◽  
Symmetric Black Hole ◽  
Sds Black Hole

The effect of cosmic string on the quasinormal modes (QNMs) of massless Dirac field perturbations were studied in different black hole spacetimes. Quasi-normal mode frequencies of massless Dirac field in Schwarzschild, RN extremal, SdS and near extremal SdS black hole spacetimes with cosmic string are obtained using WKB approximation. Our study shows a clear deviation in QNMs due to presence of cosmic string from those in the absence of string. The influence of cosmic string coded in the form of an increase in the oscillation frequency and damping time of QNMs.

scholarly journals On the nature of the neutrino

2016 ◽  
Vol 31 (19) ◽  
pp. 1650113
Author(s):  
R. Romero
Keyword(s):  
Field Operator ◽  
Dirac Field ◽  
Majorana Particle ◽  
Massive Dirac Field

Assuming that one neutrino type with definite mass is described by a massive Dirac field operator, it is shown that the physical one-particle states for particles and antiparticles can be rotated to each other, irrespective of their helicity. This result is used to prove that the neutrino must necessarily be a Majorana particle.

scholarly journals CASIMIR ENERGY FOR A MASSIVE DIRAC FIELD IN ONE SPATIAL DIMENSION: A DIRECT APPROACH

2012 ◽  
Vol 27 (07) ◽  
pp. 1250038 ◽  
Author(s):  
R. SAGHIAN ◽  
M. A. VALUYAN ◽  
A. SEYEDZAHEDI ◽  
S. S. GOUSHEH
Keyword(s):  
Boundary Condition ◽  
Analytic Continuation ◽  
Spatial Dimension ◽  
Casimir Energy ◽  
Dirac Field ◽  
Rigorous Derivation ◽  
Fermionic Field ◽  
Bag Model ◽  
Mit Bag Model ◽  
Massive Dirac Field

In this paper, we calculate the Casimir energy for a massive fermionic field confined between two points in one spatial dimension, with the MIT bag model boundary condition. We compute the Casimir energy directly by summing over the allowed modes. The method that we use is based on the Boyer's method, and there will be no need to resort to any analytic continuation techniques. We explicitly show the graph of the Casimir energy as a function of the distance between the points and the mass of the fermionic field. We also present a rigorous derivation of the MIT bag model boundary condition.

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