Tensor perturbations of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>T</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>branes

Zhong, Yuan; Liu, Yu-Xiao; Yang, Ke

doi:10.1103/physrevd.93.044002

Cited by 49 publications

(49 citation statements)

References 71 publications

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“…[39] contains a basic error, because of the use of the conformal dimension for the two-partonic states. This gives misleading results for the twist-scaling for small values of the holographic coordinate of the tetraquark wave function and results in a underestimate of the tetraquark mass spectrum.…”

Section: Introductionmentioning

confidence: 99%

Tetraquarks in holographic QCD

Gutsche¹,

Lyubovitskij²,

Schmidt³

2017

Phys. Rev. D

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Using a soft-wall AdS/QCD approach we derive the Schrödinger-type equation of motion for the tetraquark wave function, which is dual to the dimension-4 AdS bulk profile. The latter coincides with the number of constituents in the leading Fock state of the tetraquark. The obtained equation of motion is solved analytically, providing predictions for both the tetraquark wave function and its mass. A low mass limit for possible tetraquark states is given by M ≥ 2κ = 1 GeV, where κ = 0.5 GeV is the typical value of the scale parameter in soft-wall AdS/QCD. We confirm results of the COMPASS Collaboration recently reported on the discovery of the a1(1414) state, interpreted as a tetraquark state composed of light quarks and having J P C = 1 ++ . Our prediction for the mass of this state, Ma 1 = √ 2 GeV ≃ 1.414 GeV, is in good agreement with the COMPASS result Ma 1 = 1.414−0.013 GeV. Next we included finite quark mass effects, which are essential for the tetraquark states involving heavy quarks.

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Section: Introductionmentioning

confidence: 99%

Tetraquarks in holographic QCD

Gutsche¹,

Lyubovitskij²,

Schmidt³

2017

Phys. Rev. D

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“…As shown by Beiglböck [41], there exists a unique timelike world line x μ (τ ) which is called the center of mass of the particle. Then the motion of the particle can be described by the well-known Mathisson-Papapetrou-Dixon (MPD) equation [15,19]…”

Section: Motions Of Spinning Particlesmentioning

confidence: 99%

“…The a e-mail: jiejiang@mail.bnu.edu.cn b e-mail: sijie@bnu.edu.cn orbit of a spinning particle deviates from a geodesic and can be described by the Mathisson-Papapetrou-Dixon (MPD) equation [15][16][17][18]. The BSW mechanism for spinning particles in Kerr, Kerr-Newman and Kerr-Sen spacetimes has been investigated [19][20][21].…”

Section: Introductionmentioning

confidence: 99%

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Universality of BSW mechanism for spinning particles

Jiang

Gao

2019

Eur. Phys. J. C

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Bañados et al. (BSW) found that Kerr black holes can act as particle accelerators with collisions at arbitrarily high center-of-mass energies. Recently, collisions of particles with spin around some rotating black holes have been discussed. In this paper, we study the BSW mechanism for spinning particles by using a metric ansatz which describes a general rotating black hole. We notice that there are two inequivalent definitions of center-of-mass (CM) energy for spinning particles. We mainly discuss the CM energy defined in terms of the worldline of the particle. We show that there exists an energy-angular momentum relation e = h j that causes collisions with arbitrarily high energy near extremal black holes. We also provide a simple but rigorous proof that the BSW mechanism breaks down for nonextremal black holes. For the alternative definition of the CM energy, some authors find a new critical spin relation that also causes the divergence of the CM mass. However, by checking the timelike constraint, we show that particles with this critical spin cannot reach the horizon of the black hole. Further numerical calculation suggests that such particles cannot exist anywhere outside the horizon. Our results are universal, independent of the underlying theories of gravity.

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“…Harada [18] has given an excellent review work on particle collision. Several authors have discussed particle collision in [19][20][21]. Now, the lower dimensional setting becomes more sharper than 3+1 dimensional case to get conceptual focus.…”

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confidence: 99%

Collision of particles near charged MSW black hole in 2 + 1 dimensions

Saha

Debnath

2019

Mod. Phys. Lett. A

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Here, we explore the dynamics of particle near the horizon of charged Mandal-Sengupta-Wadia (MSW) black hole in 2+1 dimensions. It results analysis of angular momentum and potential energy for null and time-like geodesics. We also appraise the high center-of-mass energy of coming particles from rest at infinity near the horizon of the charged MSW black hole in 2+1 dimension for the extremal case. Finally, we study the ISCO and MBCO radii for this type of black hole. Introduction:Recently, "Two particle collision at the neighborhood of horizons of the black hole" becomes fascinated window in Astrophysics. This method, known as BSW effect, has been firstly achieved by Banados, Silk and West [1] in 2009 for the Kerr black hole to get large center-of-mass (CM) energy if one of particles has critical angular momentum. To get this process, the black hole should be extremal. The CM energy for non-extremal black hole has been demonstrated by Jacobson and Sotiriou [2] where they have pointed out the drawback of this process. So, there must exist astrophysical limitations for extremal Kerr black hole. Lake [3] has found divergent CM energy at inner horizon for rotating Kerr black hole. Liu et al. [4] have studied BSW effect of the Kerr-Taub-NUT space-time for extremal case. Grib and Pavlov [5] have established disbursement of acceleration of the particles to produce high amount of CM energy for a rotating black hole in the case of extremal and non extremal both. Kerr-de Sitter black hole for non extremal case [6] acts as a particle accelerator with unbounded CM energy for two particle collisions. Wei et al. [7] have studied the same thing for the Sen black hole. For non rotating black hole, Zaslavskill [8] has studied particle acceleration. Extension of the BSW effect on particle acceleration on various type of black holes such as charged, non charged, rotating and non rotating black holes have been investigated in [9][10][11][12].Some attractions have been occurred on a new type of black hole, named as Regular black hole with non-singular curvature. Bardeen [13] has introduced First Regular black hole. Then slowly many authors have worked on this type of various black holes in [14][15][16]. Next Amir and Ghosh [17] have studied the rotating Hayward black hole as particle accelerator. Harada [18] has given an excellent review work on particle collision. Several authors have discussed particle collision in [19][20][21]. Now, the lower dimensional setting becomes more sharper than 3+1 dimensional case to get conceptual focus. To solve Einstein gravity equations, 2+1 dimensional black hole is exact solution than 3+1 dimensional black hole. Both 2+ 1 black hole and 3+ 1 black hole contribute same physical *

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Tensor perturbations off(T)branes

Cited by 49 publications

References 71 publications

Tetraquarks in holographic QCD

Tetraquarks in holographic QCD

Universality of BSW mechanism for spinning particles

Collision of particles near charged MSW black hole in 2 + 1 dimensions

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