Fermi surface renormalization in two dimensions

Freire, Hermann; Correa, Eberth; Ferraz, A.

doi:10.1016/j.physc.2004.02.143

Cited by 4 publications

(6 citation statements)

References 4 publications

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“…[3](a) the self-energy corrections are stronger in the less curved regions of the FS around the diagonal parts of the BZ. This correction coincides with that found in [30] for the renormalization of a flat FS by a two-loop field theory RG approach, where interactions induce a small curvature to the bare flat FS. When we change the filling, the FS shape varies, and close to half-filling the FS has the form shown in Fig.…”

supporting

confidence: 88%

Deformation of anisotropic Fermi surfaces due to electron-electron interactions

Roldán¹,

Sancho²,

Guinea³

et al. 2006

Europhys. Lett.

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Strongly correlated electron systems. PACS. 71.18.+y -Fermi surfaces.Abstract. -We analyze the deformations of the Fermi surface induced by electron-electron interactions in anisotropic two dimensional systems. We use perturbation theory to treat, on the same footing, the regular and singular regions of the Fermi surface. It is shown that, even for weak local coupling, the self-energy presents a nontrivial behavior showing momentum dependence and interplay with the Fermi surface shape. Our scheme gives simple analytical expressions based on local features of the Fermi surface.

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supporting

confidence: 88%

Deformation of anisotropic Fermi surfaces due to electron-electron interactions

Roldán¹,

Sancho²,

Guinea³

et al. 2006

Europhys. Lett.

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“…For a few µG magnetic fields, freshly injected electrons (and positrons) create a small synchrotron nebula around the pulsar which should be visible in X-rays, in contrast to an often much larger TeV nebula, generated by IC processes (for a recent review see [34]). Typically only young pulsars with large spin-down power ( Ė>10 33 erg s −1 ) produce prominent PWNe [18]. This is illustrated in Fig.…”

Section: Pulsars and Pulsar Wind Nebulae At Very High Energymentioning

confidence: 87%

“…Moreover, unpulsed γ-rays from 11 globular clusters have been detected; this is interpreted as due to the ensembles of MSPs in these clusters. Some support for such interpretation comes from the case of J1823-3021A in globular cluster NGC6624, the first MSP in a GC detected so far as a source of pulsed γ-rays [33].…”

Section: Age [Yrs]mentioning

confidence: 99%

Prospects for observations of pulsars and pulsar wind nebulae with CTA

Oña-Wilhelmi

Rudak

Barrio

et al. 2013

Astroparticle Physics

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The last few years have seen a revolution in very-high gamma-ray astronomy (VHE; E > 100 GeV) driven largely by a new generation of Cherenkov telescopes (namely the H.E.S.S. telescope array, the MAGIC and MAGIC-II large telescopes and the VERITAS telescope array). The Cherenkov Telescope Array (CTA) project foresees a factor of 5 to 10 improvement in sensitivity above 0.1 TeV, extending the accessible energy range to higher energies up to 100 TeV, in the Galactic cut-off regime, and down to a few tens GeV, covering the VHE photon spectrum with good energy and angular resolution. As a result of the fast development of the VHE field, the number of pulsar wind nebulae (PWNe) detected has increased from one PWN in the early '90s to more than two dozen firm candidates today. Also, the low energy threshold achieved and good sensitivity at TeV energies has resulted in the detection of pulsed emission from the Crab Pulsar (or its close environment) opening new and exiting expectations about the pulsed spectra of the high energy pulsars powering PWNe. Here we discuss the physics goals we aim to achieve with CTA on pulsar and PWNe physics evaluating the response of the instrument for different configurations. (C) 2012 Elsevier B.V. All rights reserved

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“…( 1) we need to keep track of the momentum-and frequency dependence of the fourpoint vertex. To do this we use here the functional RG method 12,13,14,18,19,20,21,22,23 . We have derived Eq.…”

Section: Exact Rg Equation For the Fermi Surfacementioning

confidence: 99%

“…We have derived Eq. ( 1) using both the field theoretical 13,14,21 and the Wilsonian formulation 12,22 of the functional RG. In order to make contact with previous work 5,9 , let us outline here the derivation within the Wilsonian approach.…”

Section: Exact Rg Equation For the Fermi Surfacementioning

confidence: 99%