Magneto-transport in a quantum network: evidence of a mesoscopic switch

Saha, Srilekha; Maiti, Santanu K.; Karmakar, S. N.

doi:10.1140/epjb/e2012-30163-6

Cited by 14 publications

(13 citation statements)

References 32 publications

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“…This shows that Bianchi type II spacetime (2) does not allow the pressures of the DE fluid to be different along x and y directions as long as the shear stress of the overall EMT is null (i.e., as long as T 2 3 = 0, which gives G 2 3 = 0 (10)). This is a result similar to the one discussed in a recent paper [60] by Saha. Hence, although the metric we consider is totally anisotropic, the anisotropy of the DE is constrained to be axially symmetric, as long as the overall EMT possesses zero shear stress.…”

Section: The Metric Field Equations Solution and Some Immediate Ressupporting

confidence: 91%

Bianchi type-II models in the presence of perfect fluid and anisotropic dark energy

Kumar

Akarsu

2012

Eur. Phys. J. Plus

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Spatially homogeneous but totally anisotropic and non-flat Bianchi type II cosmological model has been studied in general relativity in the presence of two minimally interacting fluids; a perfect fluid as the matter fluid and a hypothetical anisotropic fluid as the dark energy fluid. The Einstein's field equations have been solved by applying two kinematical ansätze: we have assumed the variation law for the mean Hubble parameter that yields a constant value of deceleration parameter, and one of the components of the shear tensor has been considered proportional to the mean Hubble parameter. We have particularly dwelled on the accelerating models with non-divergent expansion anisotropy as the Universe evolves. Yielding anisotropic pressure, the fluid we consider in the context of dark energy, can produce results that can be produced in the presence of isotropic fluid in accordance with the ΛCDM cosmology. However, the derived model gives additional opportunities by being able to allow kinematics that cannot be produced in the presence of fluids that yield only isotropic pressure. We have obtained well behaving cases where the anisotropy of the expansion and the anisotropy of the fluid converge to finite values (include zero) in the late Universe. We have also showed that although the metric we consider is totally anisotropic, the anisotropy of the dark energy is constrained to be axially symmetric, as long as the overall energy momentum tensor possesses zero shear stress.

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Section: The Metric Field Equations Solution and Some Immediate Ressupporting

confidence: 91%

Bianchi type-II models in the presence of perfect fluid and anisotropic dark energy

Kumar

Akarsu

2012

Eur. Phys. J. Plus

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“…Especially after the detection and further experimental reconfirmation of current cosmic acceleration [23,24] the spinor field was considered as an alternative model for dark energy in a number of papers [9-11, 13, 22]. Moreover, it was established that beside describing the different stages of the evolution of the Universe, spinor field can simulate perfect fluid and dark energy [25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

Nonlinear spinor fields in Bianchi type-VI spacetime

Saha

2016

Eur. Phys. J. Plus

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Within the scope of Bianchi type-V I 0 spacetime we study the role of spinor field on the evolution of the Universe. It is found that the presence of nontrivial non-diagonal components of energy-momentum tensor of the spinor field plays vital role on the evolution of the Universe. As a result of their mutual influence there occur two different scenarios. In one case the invariants constructed from the bilinear forms of the spinor field become trivial, thus giving rise to a massless and linear spinor field Lagrangian. According to the second scenario massive and nonlinear terms do not vanish and depending on the sign of coupling constants we have either an expanding mode of expansion or the one that after obtaining some maximum value contracts and ends in big crunch generating spacetime singularity. This result shows that the spinor field is highly sensitive to the gravitational one.

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“…The electromagnetic field E µν is taken in the form given by Lichnerowich [9]. We assume that the magnetic field is homogeneous aligned along the z-direction, B µ ∼ B 3 δ 3 µ and consequently the energy density of the magnetic field is [4,10]…”

Section: )mentioning

confidence: 99%

“…Taking into account the conservation of the energy-momentum tensor, i.e., T ν µ;ν = 0, after a little manipulation one obtains [5,10,11]:…”

Section: )mentioning

confidence: 99%