Note on the decay of noncommutative solitons

Acatrinei, Ciprian Sorin; Sochichiu, Corneliu

doi:10.1103/physrevd.67.125017

Cited by 18 publications

(55 citation statements)

References 26 publications

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“…The (ij) component of the matrix represents the tachyon in the open string sector beginning on the i-th D-brane and ending on the j-th D-brane. A family of minima of the tachyon potential can be found by beginning with the configuration T = T 0 1 0 0 −1 which represents the tachyon on the first D-brane at its minimum T 0 and the tachyon on the second D-brane at its minimum −T 0 , and then making an SU (2) rotation. This gives a family of minima of the form T = T 0n .…”

Section: Static Solutions In Superstring Theorymentioning

confidence: 99%

“…Let A (1) µ and A (2) µ denote the gauge fields in the two SU(2) gauge groups. Then we can construct a codimension 4 brane solution where the fields depend on four of the spatial coordinates, and have the asymptotic behaviour:…”

Section: Static Solutions In Superstring Theorymentioning

confidence: 99%

“…23 We also define 2) and let V be the vertex operator associated with |V . Clearly V has ghost number 0.…”

Section: Boundary String Field Theorymentioning

confidence: 99%

“…Contribution to |Ψ (2) c from the terms in |B 2 involving excitations by Liouville Virasoro generators have been analyzed in [490]. Since we shall not need these results for later analysis we refer the reader to the original paper for details.…”

Section: Closed String Background Produced By |Bmentioning

confidence: 99%

See 3 more Smart Citations

Tachyon Dynamics in Open String Theory

SEN¹

2005

Progress in String Theory

103

193

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In this review we describe our current understanding of the properties of open string tachyons on an unstable D-brane or brane-antibrane system in string theory. The various string theoretic methods used for this study include techniques of two dimensional conformal field theory, open string field theory, boundary string field theory, non-commutative solitons etc. We also describe various attempts to understand these results using field theoretic methods. These field theory models include toy models like singular potential models and p-adic string theory, as well as more realistic version of the tachyon effective action based on Dirac-Born-Infeld type action. Finally we study closed string background produced by the 'decaying' unstable D-branes, both in the critical string theory and in the two dimensional string theory, and describe the open string completeness conjecture that emerges out of this study. According to this conjecture the quantum dynamics of an unstable D-brane system is described by an internally consistent quantum open string field theory without any need to couple the system to closed strings. Each such system can be regarded as a part of the 'hologram' describing the full string theory.

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Section: Static Solutions In Superstring Theorymentioning

confidence: 99%

Section: Static Solutions In Superstring Theorymentioning

confidence: 99%

“…23 We also define 2) and let V be the vertex operator associated with |V . Clearly V has ghost number 0.…”

Section: Boundary String Field Theorymentioning

confidence: 99%

Section: Closed String Background Produced By |Bmentioning

confidence: 99%

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Tachyon Dynamics in Open String Theory

SEN¹

2005

Progress in String Theory

103

193

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“…[4].) This provides a rich gamut of possibilities in the context of cosmology [2,[4][5][6][7].The stress tensor for the tachyonic scalar field can be written in a perfect fluid formwithThe remarkable feature of this stress tensor is that it could be considered as the sum of a pressure less dust component and a cosmological constant [2]. To show this explicitly, we break up the density ρ and the pressure p and write them in a more suggestive form as…”

mentioning

confidence: 99%

Cosmology with tachyon field as dark energy

2003

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We present a detailed study of cosmological effects of homogeneous tachyon matter coexisting with non-relativistic matter and radiation, concentrating on the inverse square potential and the exponential potential for the tachyonic scalar field. A distinguishing feature of these models (compared to other cosmological models) is that the matter density parameter and the density parameter for tachyons remain comparable even in the matter dominated phase. For the exponential potential, the solutions have an accelerating phase, followed by a phase with a(t) ∝ t 2/3 as t → ∞. This eliminates the future event horizon present in ΛCDM models and is an attractive feature from the string theory perspective. A comparison with supernova Ia data shows that for both the potentials there exists a range of models in which the universe undergoes an accelerated expansion at low redshifts and are also consistent with requirements of structure formation. They do require fine tuning of parameters but not any more than in the case of ΛCDM or quintessence models. I. MOTIVATIONObservations suggest that our universe has entered a phase of accelerated expansion in the recent past. Friedmann equations can be consistent with such an accelerated expansion only if the universe is populated by a medium with negative pressure. One of the possible sources which could provide such a negative pressure will be a scalar field with either of the following two types of Lagrangians:Both these Lagrangians involve one arbitrary function V (φ). The first one L quin , which is a natural generalization of the Lagrangian for a nonrelativistic particle, L = (1/2)q 2 − V (q), is usually called quintessence (for a sample of models, see Ref.[1]). When it acts as a source in Friedmann universe, it is characterized by a time dependent w(t) ≡ (P/ρ) withJust as L quin generalizes the Lagrangian for the nonrelativistic particle, L tach generalizes the Lagrangian for the relativistic particle [2]. A relativistic particle with a (one dimensional) position q(t) and mass m is described by the Lagrangian L = −m 1 −q 2 . It has the energy E = m/ 1 −q 2 and momentum p = mq/ 1 −q 2 which are related by E 2 = p 2 +m 2 . As is well known, this allows the possibility of having massless particles with finite energy for which E 2 = p 2 . This is achieved by taking the limit of m → 0 andq → 1, while keeping the ratio in E = m/ 1 −q 2 finite. The momentum acquires a life of its own, unconnected with the velocityq, and the energy is expressed in terms of the momentum (rather than in terms ofq) in the Hamiltonian formulation. We can now construct a field theory by upgrading q(t) to a field φ. Relativistic invariance now requires φ to depend on both space and time [φ = φ(t, x)] andq 2 to be replaced by ∂ i φ∂ i φ. It is also possible now to treat the mass parameter m as a function of φ, say, V (φ) thereby obtaining a field theoretic Lagrangian L = −V (φ) 1 − ∂ i φ∂ i φ. The Hamiltonian structure of this theory is algebraically very similar to the special relativistic example we starte...

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Discrete nonlocal waves

Acatrinei

2013

J. High Energ. Phys.

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We study generic waves without rotational symmetry in (2+1)dimensional noncommutative scalar field theory. In the representation chosen, the radial coordinate is naturally rendered discrete. Nonlocality along this coordinate, induced by noncommutativity, accounts for the angular dependence of the fields. The exact form of standing and propagating waves on such a discrete space is found in terms of finite series. A precise correspondence is established between the degree of nonlocality and the angular momentum of a field configuration. At small distance no classical singularities appear, even at the location of the sources. At large radius one recovers the usual commutative behaviour.

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Note on the decay of noncommutative solitons

Cited by 18 publications

References 26 publications

Tachyon Dynamics in Open String Theory

Tachyon Dynamics in Open String Theory

Cosmology with tachyon field as dark energy

Discrete nonlocal waves

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