Searcharxiv⌕ Search

arXiv subjects

E. Elizalde

Publications and source records attributed to E. Elizalde.

At least 91 records · Page 5Linked to original sources

Some uses of $ζ-$regularization in quantum gravity and cosmology

This is a short guide to some uses of the zeta-function regularization procedure as a a basic mathematical tool for quantum field theory in curved space-time (as is the case of Nambu-Jona-Lasinio models), in quantum gravity models (in different dimensions), and also in cosmology, where it appears e.g. in the calculation of possible `contributions' to the cosmological constant coming through manifestations of the vacuum energy density. Part of this research was carried out in fruitful and enjoyable collaboration with people from Tomsk State Pedagogical University.

hep-th↗

Effective Finite Temperature Partition Function for Fields on Non-Commutative Flat Manifolds

The first quantum correction to the finite temperature partition function for a self-interacting massless scalar field on a $D-$dimensional flat manifold with $p$ non-commutative extra dimensions is evaluated by means of dimensional regularization, suplemented with zeta-function techniques. It is found that the zeta function associated with the effective one-loop operator may be nonregular at the origin. The important issue of the determination of the regularized vacuum energy, namely the first quantum correction to the energy in such case is discussed.

hep-th↗

Matching the observational value of the cosmological constant

A simple model is introduced in which the cosmological constant is interpreted as a true Casimir effect on a scalar field filling the universe (e.g. $\mathbf{R} \times \mathbf{T}^p\times \mathbf{T}^q$, $\mathbf{R} \times \mathbf{T}^p\times \mathbf{S}^q, ...$). The effect is driven by compactifying boundary conditions imposed on some of the coordinates, associated both with large and small scales. The very small -but non zero- value of the cosmological constant obtained from recent astrophysical observations can be perfectly matched with the results coming from the model, by playing just with the numbers of -actually compactified- ordinary and tiny dimensions, and being the compactification radius (for the last) in the range $(1-10^3) l_{Pl}$, where $l_{Pl}$ is the Planck length. This corresponds to solving, in a way, what has been termed by Weinberg the {\it new} cosmological constant problem. Moreover, a marginally closed universe is favored by the model, again in coincidence with independent analysis of the observational results.

hep-th↗

Spectral Zeta Functions in Non-Commutative Spacetimes

Formulas for the most general case of the zeta function associated to a quadratic+linear+constant form (in {\bf Z}) are given. As examples, the spectral zeta functions $ζ_α(s)$ corresponding to bosonic ($α=2$) and to fermionic ($α=3$) quantum fields living on a noncommutative, partially toroidal spacetime are investigated. Simple poles show up at $s=0$, as well as in other places (simple or double, depending on the number of compactified, noncompactified, and noncommutative dimensions of the spacetime). This poses a challenge to the zeta-function regularization procedure.

hep-th↗

Explicit Zeta Functions for Bosonic and Fermionic Fields on a Noncommutative Toroidal Spacetime

Explicit formulas for the zeta functions $ζ_α(s)$ corresponding to bosonic ($α=2$) and to fermionic ($α=3$) quantum fields living on a noncommutative, partially toroidal spacetime are derived. Formulas for the most general case of the zeta function associated to a quadratic+linear+constant form (in {\bf Z}) are obtained. They provide the analytical continuation of the zeta functions in question to the whole complex $s-$plane, in terms of series of Bessel functions (of fast, exponential convergence), thus being extended Chowla-Selberg formulas. As well known, this is the most convenient expression that can be found for the analytical continuation of a zeta function, in particular, the residua of the poles and their finite parts are explicitly given there. An important novelty is the fact that simple poles show up at $s=0$, as well as in other places (simple or double, depending on the number of compactified, noncompactified, and noncommutative dimensions of the spacetime), where they had never appeared before. This poses a challenge to the zeta-function regularization procedure.

hep-th↗

A family of quantum interiors for ordinary and stringy black holes II: Geometric considerations and global properties

A family of spacetimes suitable for describing the matter conditions of a static, spherically symmetric quantum vacuum is studied, as well as its reliability for describing a regular model for the interior of a semiclassical, static black hole ---without ever invoking a mass shell for the final object. In paper I, this condition was seen to limit the search to only one, distinguished family, that was investigated in detail. Here it will be proven that, aside from being mathematically generic (in its uniqueness), this family exhibits beautiful physical properties, that one would reasonably demand from a collapse process, including the remarkable result that isotropization may take place conveniently far from the (unavoidable) regularization scale. The analysis is also extended in order to include the possibility of a stringy core, always within the limits imposed by the semiclassical approach to gravitation. This constitutes a first approximation to the final goal of trying to characterize a regular, self-gravitating, stringy black hole.

gr-qc↗

Quantum deletion is possible via a partial randomization procedure

An alternative kind of deleting/erasing operation is introduced which differs from the commonly used {\it controlled-not} (C-not) conditional logical operation $-$to flip to a standard, `zero' value the (classical or quantum) state of the last copy in a chain, in a deletion process. It is completely reversible, in the classical case, possessing a most natural cloning operation counterpart. We call this deleting procedure R-deletion since, in a way, it can be viewed as a `randomization' of the standard C-not operator. It has the remarkable property of by-passing in a simple manner the `impossibility of deletion of a quantum state' principle, put forward by Pati and Braunstein recently \cite{pbn1}.

quant-ph↗

Gravitational Evolution of the Large-Scale Density Distribution: The Edgeworth & Gamma Expansions

The gravitational evolution of the cosmic one-point Probability Distribution Function (PDF) can be estimated using an analytic approximation that combines gravitational Perturbation Theory (PT) with the Edgeworth expansion around a Gaussian PDF. We present an alternative to the Edgeworth series based on an expansion around the Gamma PDF, which is more appropriate to describe a realistic PDF. The Gamma expansion converges when the PDF exhibits exponential tails, which are predicted by PT and N-body simulations in the weakly non-linear regime (i.e, when the variance, $σ^2$, is small). We compare both expansions to N-body simulations and find that the Gamma expansion yields a better overall match to the numerical results.

astro-ph↗

Data Processing and Compression of Cosmic Microwave Background Anisotropies on Board the PLANCK Satellite

We present a simple way of coding and compressing the data on board the Planck instruments (HFI and LFI) to address the problem of the on board data reduction. This is a critical issue in the Planck mission. The total information that can be downloaded to Earth is severely limited by the telemetry allocation. This limitation could reduce the amount of diagnostics sent on the stability of the radiometers and, as a consequence, curb the final sensitivity of the CMB anisotropy maps. Our proposal to address this problem consists in taking differences of consecutive circles at a given sky pointing. To a good approximation, these differences are independent of the external signal, and are dominated by thermal (white) instrumental noise. Using simulations and analytical predictions we show that high compression rates, $c_r \simeq 10$, can be obtained with minor or zero loss of CMB sensitivity. Possible effects of digital distortion are also analized. The proposed scheme allows for flexibility to optimize the relation with other critical aspects of the mission. Thus, this study constitutes an important step towards a more realistic modeling of the final sensitivity of the CMB temperature anisotropy maps.

astro-ph↗

On the continuum limit of the lattice chiral anomaly trace relation

Different aspects concerning the rigorous definition of the traces and determinants of the operators involved in a procedure ---proposed by Neuberger and others--- for avoiding fermion doublers on the lattice, are considered. A result of the analysis is that it seems unclear that the consequences derived from the independent treatment of the traces of the two operators contributing to the index relation on the lattice, as carried out in recent manuscripts, can be given rigorous mathematical footing, in particular, that these treatments can commute with the continuum limit ---the lattice regularized trace being additive all the way through the limit, while the otherwise regularized trace in the continuum is not so.

hep-lat↗

On the concept of determinant for the differential operators of Quantum Physics

The concept of determinant for a linear operator in an infinite-dimensional space is addressed, by using the derivative of the operator's zeta-function (following Ray and Singer) and, eventually, through its zeta-function trace. A little play with operators as simple as $\pm I$ ($I$ being the identity operator) and variations thereof, shows that the presence of a non-commutative anomaly (i.e., the fact that det $(AB) \neq$ det $A$ det $B$), is unavoidable, even for commuting and, remarkably, also for almost constant operators. In the case of Dirac-type operators, similarly basic arguments lead to the conclusion ---contradicting common lore--- that in spite of being $\det (\slash D +im) = \det (\slash D -im)$ (as follows from the symmetry condition of the $\slash D$-spectrum), it turns out that these determinants may {\it not} be equal to $\sqrt{\det (\slash D^2 +m^2)}$, simply because $\det [(\slash D +im) (\slash D -im)] \neq \det (\slash D +im) \det (\slash D -im)$. A proof of this fact is given, by way of a very simple example, using operators with an harmonic-oscillator spectrum and fulfilling the symmetry condition. This anomaly can be physically relevant if, in addition to a mass term (or instead of it), a chemical potential contribution is added to the Dirac operator.

hep-th↗

Gravitational Evolution of the Large-Scale Probability Density Distribution: The Edgeworth & Gamma Expansions

The gravitational evolution of the cosmic one-point probability distribution function (PDF) has been estimated using an analytic approximation that combines gravitational perturbation theory with the Edgeworth expansion around a Gaussian PDF. Despite the remarkable success of the Edgeworth expansion in modeling the weakly non-linear growth of fluctuations around the peak of the cosmic PDF, it fails to reproduce the expected behaviour in the tails of the distribution. Besides, this expansion is ill-defined as it predicts negative densities and negative probabilities for the cosmic fields. This is a natural consequence of using an expansion around the Gaussian distribution, which is not rigorously well-defined when describing a positive variate, such as the density field. Here we present an alternative to the Edgeworth series based on an expansion around the Gamma PDF. The Gamma expansion is designed to converge when the PDF exhibits exponential tails. The proposed expansion is better suited for describing a real PDF as it always yields positive densities and the PDF is effectively positive-definite. We compare the performance of the Edgeworth and the Gamma expansions for a wide dynamical range making use of cosmological N-body simulations and assess their range of validity. In general, the Gamma expansion provides an interesting and simple alternative to the Edgeworth series and it should be useful for modeling non-gaussian PDFs in other contexts, such as in the cosmic microwave background.

astro-ph↗

Possible quantum instability of primordial black holes

Evidence for the possible existence of a quantum process opposite to the famous Hawking radiation (evaporation) of black holes is presented. This new phenomenon could be very relevant in the case of exotic multiple horizon Nariai black holes and in the context of common grand unified theories. This is clearly manifested in the case of the SO(10) GUT, that is here investigated in detail. The remarkable result is obtained, that anti-evaporation can occur there only in the SUSY version of the theory. It is thus concluded that the existence of primordial black holes in the present Universe might be considered as an evidence for supersymmetry.

hep-th↗

Heat Kernel Coefficients for Chern-Simons Boundary Conditions in QED

We consider the four dimensional Euclidean Maxwell theory with a Chern-Simons term on the boundary. The corresponding gauge invariant boundary conditions become dependent on tangential derivatives. Taking the four-sphere as a particular example, we calculate explicitly a number of the first heat kernel coefficients and obtain the general formulas that yields any desired coefficient. A remarkable observation is that the coefficient $a_2$, which defines the one-loop counterterm and the conformal anomaly, does not depend on the Chern-Simons coupling constant, while the heat kernel itself becomes singular at a certain (critical) value of the coupling. This could be a reflection of a general property of Chern-Simons theories.

hep-th↗

Data compression on board the PLANCK Satellite Low Frequency Instrument: optimal compression rate

Data on board the future PLANCK Low Frequency Instrument (LFI), to measure the Cosmic Microwave Background (CMB) anisotropies, consist of $N$ differential temperature measurements, expanding a range of values we shall call $R$. Preliminary studies and telemetry allocation indicate the need of compressing these data by a ratio of $c_r \simgt 10$. Here we present a study of entropy for (correlated multi-Gaussian discrete) noise, showing how the optimal compression $c_{r,opt}$, for a linearly discretized data set with $N_{bits}=\log_2{N_{max}}$ bits is given by: $c_r \simeq {N_{bits}/\log_2(\sqrt{2πe} ~σ_e/Δ)}$, where $σ_e\equiv (det C)^{1/2N}$ is some effective noise rms given by the covariance matrix $C$ and $Δ\equiv R / N_{max}$ is the digital resolution. This $Δ$ only needs to be as small as the instrumental white noise RMS: $Δ\simeq σ_T \simeq 2 mK$ (the nominal $μK$ pixel sensitivity will only be achieved after averaging). Within the currently proposed $N_{bits}=16$ representation, a linear analogue to digital converter (ADC) will allow the digital storage of a large dynamic range of differential temperature $R= N_{max} Δ$ accounting for possible instrument drifts and instabilities (which could be reduced by proper on-board calibration). A well calibrated signal will be dominated by thermal (white) noise in the instrument: $σ_e \simeq σ_T$, which could yield large compression rates $c_{r,opt} \simeq 8$. This is the maximum lossless compression possible. In practice, point sources and $1/f$ noise will produce $σ_e > σ_T$ and $c_{r,opt} < 8$. This strategy seems safer than non-linear ADC or data reduction schemes (which could also be used at some stage).

astro-ph↗

Dynamical symmetry breaking in Nambu-Jona-Lasinio model under the influence of external electromagnetic and gravitational fields

Dynamical symmetry breaking is investigated for a four-fermion Nambu-Jona-Lasinio model in external electromagnetic and gravitational fields. An effective potential is calculated in the leading order of the large-N expansion using the proper-time Schwinger formalism. Phase transitions accompanying a chiral symmetry breaking in the Nambu-Jona-Lasinio model are studied in detail. A magnetic calalysis phenomenon is shown to exist in curved spacetime but it turns out to lose its universal character because the chiral symmetry is restored above some critical positive value of the spacetime curvature.

hep-th↗

Dynamical symmetry restoration for a higher-derivative four-fermion model in an external electromagnetic field

A four-fermion model with additional higher-derivative terms is investigated in an external electromagnetic field. The effective potential in the leading order of large-N expansion is calculated in external constant magnetic and electric fields. It is shown that, in contrast to the former results concerning the universal character of "magnetic catalysis" in dynamical symmetry breaking, in the present higher-derivative model the magnetic field restores chiral symmetry broken initially on the tree level. Numerical results describing a second-order phase transition that accompanies the symmetry restoration at the quantum level are presented.

hep-ph↗

Dynamical symmetry breaking in the Nambu-Jona-Lasino model with external gravitational and constant electric fields

An investigation of the Nambu-Jona-Lasino model with external constant electric and weak gravitational fields is carried out in three- and four- dimensional spacetimes. The effective potential of the composite bifermionic fields is calculated keeping terms linear in the curvature, while the electric field effect is treated exactly by means of the proper- time formalism. A rich dynamical symmetry breaking pattern, accompanied by phase transitions which are ruled, independently, by both the curvature and the electric field strength is found. Numerical simulations of the transitions are presented.

hep-th↗