arXiv subjects

L. Herrera

Publications and source records attributed to L. Herrera.

At least 19 recordsLinked to original sources

arXiv2026

The imprints of the instantaneous appearance of a conformal Killing vector field on the evolution of self-gravitating fluid spheres

We study the influence of the instantaneous appearance of a conformal Killing vector (CKV) in self-gravitating fluid spheres during their evolution. For doing that we introduce a tensor variable whose time dependence allows the existence of a CKV for a given value of the time-like coordinate. We consider adiabatic and dissipative fluids. The analysis of different relevant physical variables in this process provides a smoking gun signature from the emergence of CKV at some point of the evolution. Prospective applications of these results, as well as open questions and pending issues related to this problem, are discussed.

gr-qc↗

arXiv2025

Noisy dynamics of confined quantum walks on a chip

Quantum walks represent an excellent testbed for investigating the interplay between unitary coherent and incoherent dissipative processes. Thanks to photonic quantum interferometers of considerable size, experimental studies could be performed, devoted to investigating the consequences of different sorts of realistic noise in these systems. In this work we employ a 20x20 on-chip multimode interferometer to introduce another key aspect in the problem: the presence of edges in the walker lattice, enforcing a confined evolution. We show how noise can disrupt translational symmetry and reshape interference patterns. The non trivial probability distributions obtained along the temporal evolution of the system demonstrate how speed up effects, localization and coherent oscillations are pillar concepts to be fully characterized and understood when applied in realistic quantum dynamics.

quant-ph↗

arXiv2025

Complexity hierarchies in Euclidean stars

We establish a hierarchy of Euclidean stars according to their degree of complexity, as measured by the complexity factor and the complexity of the pattern of evolution. We consider both, nondissipative and dissipative systems. Solutions are ranged from the simplest one, in order of increasing complexity. Some specific models are found and analyzed in detail.

gr-qc↗

arXiv2025

The hyperbolically symmetric black hole

We describe some properties of the hyperbolically symmetric black hole (hereafter referred to as the $HSBH$) proposed a few years ago. We start by explaining the main motivation behind such an idea, and we determine the main differences between this scenario and the classical black hole (hereafter referred to as the $CBH$) scenario. Particularly important are the facts that, in the $HSBH$ scenario, (i) test particles in the region inside the horizon experience a repulsive force that prevents them from reaching the center, (ii) test particles may cross the horizon outward only along the symmetry axis, and (iii) the spacetime within the horizon is static but not spherically symmetric. Next, we examine the differences between the two models of black holes in light of the Landauer principle and the Hawking results on the eventual evaporation of the black hole and the paradox resulting thereof. Finally, we explore what observational signature could be invoked to confirm or dismiss the model.

gr-qc↗

arXiv2025

Axially symmetric ghost stars

We present static axially symmetric fluid distributions not producing gravitational field outside their boundaries (i.e. fluid sources which match smoothly on the boundary surface to Minkowski space-time). These solutions provide further examples of ghost stars. A specific model is fully described, and its physical and geometrical properties are analyzed in detail. This includes the multipole moment structure of the source and its complexity factors, both of which vanish for our solution.

gr-qc↗

arXiv2025

The birth of a ghost star

We present a model of an evolving spherically symmetric dissipative self-gravitating fluid distribution which tends asymptotically to a ghost star, meaning that the end state of such a system corresponds to a static fluid distribution with vanishing total mass, and energy-density distribution which is negative in some regions of the fluid. The model is inspired in a solution representing a fluid evolving quasi-homologously and with vanishing complexity factor. However in order to satisfy the asymptotic behavior mentioned above, the starting solution has to be modified, as a consequence of which the resulting model only satisfies the two previously mentioned conditions, asymptotically. Additionally a condition on the variation of the infinitesimal proper radial distance between two neighboring points per unit of proper time is imposed, which implies the presence of a cavity surrounding the center. Putting together all these conditions we are able to obtain an analytical model depicting the emergence of a ghost star. Some potential observational consequences of this phenomenon are briefly discussed at the last section.

gr-qc↗

arXiv2024

Modified Landauer principle according to Tsallis entropy

The Landauer principle establishes a lower bound in the amount of energy that should be dissipated in the erasure of one bit of information. The specific value of this dissipated energy is tightly related to the definition of entropy. In this article, we present a generalization of the Landauer principle based on the Tsallis entropy. Some consequences resulting from such a generalization are discussed. These consequences include the modification to the mass ascribed to one bit of information, the generalization of the Landauer principle to the case when the system is embedded in a gravitational field, and the number of bits radiated in the emission of gravitational waves.

gr-qc↗

arXiv2024

Evolution of self-gravitating fluid spheres involving ghost stars

Exact solutions are presented which describe, either the evolution of fluid distributions corresponding to a ghost star (vanishing total mass), or describing the evolution of fluid distributions which attain the ghost star status at some point of their lives. The first two solutions correspond to the former case, they admit a conformal Killing vector (CKV) and describe the adiabatic evolution of a ghost star. Other two solutions corresponding to the latter case are found, which describe evolving fluid spheres absorbing energy from the outside, leading to a vanishing total mass at some point of their evolution. In this case the fluid is assumed to be expansion-free. In all four solutions the condition of vanishing complexity factor was imposed. The physical implications of the results, are discussed

gr-qc↗

arXiv2024

Ghost stars in general relativity

We explore an idea put forward many years ago by Zeldovich and Novikov concerning the existence of compact objects endowed with arbitrarily small mass. The energy-density of such objects, which we call ``Ghost stars'', is negative in some regions of the fluid distribution, producing a vanishing total mass. Thus, the interior is matched on the boundary surface to Minkowski space-time. Some exact analytical solutions are exhibited and their properties are analyzed. Observational data that could confirm or dismiss the existence of this kind of stellar object is commented.

gr-qc↗

arXiv2024

Cracking and complexity of self-gravitating dissipative compact objects

The concept of cracking refers to the tendency of a fluid distribution to "split'', once it abandons the equilibrium. In this manuscript we develop a general formalism to describe the occurrence of cracking within a dissipative fluid distribution, in comoving coordinates. The role of dissipative processes in the occurrence of cracking is brought out. Next, we relate the occurrence of cracking with the concept of complexity for self-gravitating objects defined in [1-3]. More specifically we relate the occurrence of cracking with the condition of the vanishing of the scalar function intended to measure the complexity of the fluid distribution (the complexity factor). We also relate the occurrence of cracking with the specific mode of leaving the equilibrium. Thus, we prove that leaving the equilibrium in either, the homologous (H), or the quasi--homologous regime (QH), prevents the occurrence of cracking. Also, it is shown that imposing the condition of vanishing complexity factor alone, (independently of the mode of leaving the equilibrium) prevents the occurrence of cracking in the non-dissipative geodesic case, and in the non-dissipative isotropic case. These results bring out further the relevance of the complexity factor and its related definition of complexity, in the study of self-gravitating systems.

gr-qc↗

arXiv2024

The post--quasi-static approximation: An analytical approach to gravitational collapse

A semi--numerical approach proposed many years ago for describing gravitational collapse in the post--quasi--static approximation, is modified in order to avoid the numerical integration of the basic differential equations the approach is based upon. For doing that we have to impose some restrictions on the fluid distribution. More specifically, we shall assume the vanishing complexity factor condition, which allows for analytical integration of the pertinent differential equations and leads to physically interesting models. Instead, we show that neither the homologous nor the quasi--homologous evolution are acceptable since they lead to geodesic fluids, which are unsuitable for being described in the post--quasi--static approximation. Also, we prove that, within this approximation, adiabatic evolution also leads to geodesic fluids and therefore we shall consider exclusively dissipative systems. Besides the vanishing complexity factor condition, additional information is required for a full description of models. We shall propose different strategies for obtaining such an information, which are based on observables quantities (e.g. luminosity and redshift), and/or heuristic mathematical ansatz. To illustrate the method, we present two models. One model is inspired in the well known Schwarzschild interior solution, and another one is inspired in Tolman VI solution.

gr-qc↗

arXiv2024

Irreversibility and gravitational radiation: A proof of Bondi's conjecture

It is shown that the evolution of an axially and reflection symmetric fluid distribution, satisfying the Tolman condition for thermal equilibrium, is not accompanied by the emission of gravitational radiation. This result, which was conjectured by Bondi many years ago, expresses the irreversibility associated to the emission of gravitational waves. The observational consequences emerging from this result are commented. The resulting models are not only non--dissipative and vorticity free, but also shear--free and geodesic, furthermore all their complexity factors vanish.

gr-qc↗

arXiv2023

Quasi--hyperbolically symmetric $γ$-metric

We carry out a systematic study on the motion of test particles in the region inner to the naked singularity of a quasi--hyperbolically symmetric $γ$-metric. The geodesic equations are written and analyzed in detail. The obtained results are contrasted with the corresponding results obtained for the axially symmetric $γ$-metric, and the hyperbolically symmetric black hole. As in this latter case, it is found that test particles experience a repulsive force within the horizon (naked singularity), which prevents them to reach the center. However in the present case this behavior is affected by the parameter $γ$ which measures the departure from the hyperbolical symmetry. These results are obtained for radially moving particles as well as for particles moving in the $θ-r$ subspace. Possible relevance of these results in the explanation of extragalactic jets, is brought out.

gr-qc↗

arXiv2023

Non-spherical sources of Schwarzschild space-time

While it is known that any spherical fluid distribution may only source the spherically symmetric Schwarzschild space-time, the inverse is not true. Thus, in this manuscript, we find exact axially symmetric and static fluid (interior) solutions to Einstein equations, which match smoothly on the boundary surface to the Schwarzschild (exterior) space-time, even though the fluid distribution is not endowed with spherical symmetry. The solutions are obtained by using the general approach outlined in [1], and satisfy the usual requirements imposed to any physically admissible interior solution. A discussion about the physical and geometric properties of the source is presented. The relativistic multipole moments (RMM) are explicitly calculated in terms of the physical variables, allowing to prove that spherical sources can only match to the Schwarzschild space-time. The complexity of the source is evaluated through the complexity factors. It is shown that there is only one independent complexity factor, as in the spherically symmetric case.

gr-qc↗

arXiv2023

Complexity and simplicity of self-gravitating fluids

We review a recently proposed definition of complexity of the structure of self--gravitating fluids \cite{ch1}, and the criterium to define the simplest mode of their evolution. We analyze the origin of these concepts and their possible applications in the study of gravitation collapse. We start by considering the static spherically symmetric case, extending next the study to static axially symmetric case. Afterward we consider the non--static spherically symmetric case. Two possible modes of evolution are proposed to be the simplest one. One is the homologous conditio,, however, as was shown later on, it may be useful to relax this last condition to enlarge the set of possible solutions, by adopting the so-called quasi-homologous condition. As another example of symmetry, we consider fluids endowed with hyperbolical symmetry. Exact solutions for static fluid distributions satisfying the condition of minimal complexity are presented.. An extension of the complexity factor to the vacuum solutions of the Einstein equations represented by the Bondi metric is discussed. A complexity hierarchy is established in this case, ranging from the Minkowski spacetime (the simplest one) to gravitationally radiating systems (the most complex). Finally we propose a list of questions which, we believe, deserve to be treated in the future

gr-qc↗

arXiv2023

Expansion-free dissipative fluid spheres: Analytical models

We search exact analytical solutions of spherically symmetric dissipative fluid distributions satisfying the vanishing expansion condition (vanishing expansion scalar $Θ$). To do so we shall impose additional restrictions allowing the integration of the field equations. A detailed analysis of the obtained solutions, their prospective applications to astrophysical scenarios, as well as alternative approaches to obtain new solutions, are discussed.

gr-qc↗

arXiv2022

Non-static hyperbolicallly symmetric fluids

We present the general properties of dynamic dissipative fluid distribution endowed with hyperbolical symmetry. All the equations required for its analysis are exhibited and used to contrast the behavior of the system with the spherically symmetric case. Several exact solutions are exhibited and prospective applications to astrophysical and cosmological scenarios are discussed.

gr-qc↗

arXiv2022

Non-static fluid spheres admitting a conformal Killing vector: Exact solutions

We carry on a general study on non--static spherically symmetric fluids admitting a conformal Killing vector (CKV). Several families of exact analytical solutions are found for different choices of the CKV, in both, the dissipative and the adiabatic regime. To specify the solutions, besides the fulfillment of the junction conditions on the boundary of the fluid distribution, different conditions are imposed, such as vanishing complexity factor and quasi--homologous evolution. A detailed analysis of the obtained solutions, its prospective applications to astrophysical scenarios, as well as alternative approaches to obtain new solutions, are discussed.

gr-qc↗