arXiv subjects

Samuele Silveravalle

Publications and source records attributed to Samuele Silveravalle.

16 recordsLinked to original sources

arXiv2026

Bridging Superfluid and Nonminimally Coupled BEC Dark Matter through RAQUAL

Motivated by their common condensed-matter inspiration and their shared aim of reconciling MOND-like phenomenology on galactic scales with particle dark matter on larger scales, we investigate the relation between Superfluid Dark Matter (SFDM) and Bose--Einstein Condensate Dark Matter (BECDM). Since SFDM is formulated in the Newtonian regime whereas BECDM is fully relativistic, we first show that the MONDian formulation of SFDM arises as the Newtonian, low-acceleration limit of a Relativistic AQUAdratic Lagrangian (RAQUAL) theory in the Einstein frame. We then transform its covariant interaction sector to the Jordan frame and compare it with BECDM. The phonon--baryon interaction of SFDM maps onto the BECDM derivative coupling to the Einstein tensor, supplemented by a small non-minimal coupling to the Ricci scalar. The interaction sectors are therefore equivalent up to a linear perturbation of the Einstein--Hilbert term. Their kinetic sectors, however, remain inequivalent: the standard quadratic kinetic term of BECDM cannot be mapped onto the non-analytic kinetic term required by SFDM. The two models are consequently related but not dynamically equivalent. This mapping provides a covariant interpretation of the SFDM interaction and clarifies which theoretical properties can be transferred between the two frameworks.

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arXiv2026

Cosmology with a Non-minimally Coupled Dark Matter Fluid II. Cosmological Perturbations

We extend our study of a cosmological scenario in which dark matter is non-minimally coupled to gravity at the fluid level. In previous work, we showed that this interaction can drive an early phase of accelerated expansion, addressing the horizon and flatness problems, and can also lead to a cosmological bounce in the presence of spatial curvature. Here we analyse the evolution of linear perturbations in this framework. We derive the equations governing scalar, vector and tensor perturbations, and obtain analytic solutions in the relevant cosmological regimes. We find that perturbations generated during the accelerated expansion phase produce a strongly blue scalar power spectrum and are therefore incompatible with observations. By contrast, in bouncing solutions primordial fluctuations can originate during the contracting phase before the bounce. In this case, the model yields an approximately scale-invariant scalar power spectrum while keeping the tensor-to-scalar ratio compatible with current bounds, without introducing additional scalar fields. Although our treatment relies on simplifying approximations that should be refined in future work, these results indicate that non-minimally coupled dark matter may provide a viable alternative mechanism for the generation of primordial cosmological perturbations.

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arXiv2025

Veiled Singularities in Einstein-Weyl Gravity: Stability and Physical Interpretation of Horizonless Solutions

We investigate a class of horizonless solutions in Einstein-Weyl gravity, corresponding to the so-called attractive naked singularities of the (-2,2) type. In contrast to General Relativity, where naked singularities are generically unstable and excluded by the cosmic censorship conjecture, we show that these configurations are linearly stable under tensor perturbations. By numerically evolving the perturbation equations in the time domain, we find that all modes decay with characteristic oscillatory tails, a behavior consistent with the dynamics of massive field perturbations in quadratic gravity. This establishes that attractive naked singularities in Einstein-Weyl gravity are dynamically stable and can persist as stationary configurations. We argue that these horizonless configurations are observationally concealed, and therefore we refer to them as veiled singularities. Their stability and phenomenological similarity to black holes suggest that they may represent viable horizonless alternatives in higher-derivative theories of gravity, offering a novel perspective on the interplay between singularity resolution, stability, and effective field dynamics beyond Einstein's theory.

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arXiv2025

Charting GLOBs in Asymptotically Safe Gravity

Computing the gravitational effective action provides a direct route to charting the landscape of admissible black hole spacetimes and their alternatives, which we will collectively call "gravitationally localized objects" (GLOBs). In this work, we provide a proof of principle of this idea within the framework of asymptotically safe gravity. Focusing on the Einstein-Weyl truncation, we identify the unique ultraviolet-complete trajectory emanating from the asymptotically safe fixed point and use it to extract the Wilson coefficient of the Weyl-squared term. This allows us to chart the corresponding GLOBs in a "phase diagram", showing that wormholes dominate a large portion of it, whereas the classical Bachian naked singularities become disfavored. Our results illustrate how quantum gravity can constrain effective field theory and the associated set of allowed spacetimes, yielding a rich landscape of beyond-general-relativity solutions rather than a single alternative to classical black holes.

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arXiv2025

Cosmology with a Non-minimally Coupled Dark Matter Fluid I. Background Evolution

We explore a cosmological model in which dark matter is non-minimally coupled to gravity at the fluid level. While typically subdominant compared to Standard Model forces, such couplings may dominate dark matter dynamics. We show that this interaction modifies the early-time Friedmann equations, driving a phase of accelerated expansion that can resolve the horizon and flatness problems without introducing additional fields. At even earlier times, the coupling to spatial curvature may give rise to a cosmological bounce, replacing the initial singularity of standard cosmology. These results suggest that non-minimally coupled dark matter could offer a unified framework for addressing both the singularity and fine-tuning problems.

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arXiv2025

Spontaneous ghostification: how a dying black hole comes back as a naked singularity

A quantum ghost that destabilizes the Schwarzschild solution, transforming it into a naked singularity, may seem like a physicist's worst nightmare. However, we argue that this scenario represents the natural evolution of a black hole within a conservative high-energy gravity framework and may, in fact, be a desirable outcome. Quadratic curvature terms typically appear as corrections to the Einstein-Hilbert action at high energies; nonetheless, such theories are generally considered incomplete due to the presence of ghost particles at the quantum level, which can spoil vacuum stability. We argue that this instability can only be triggered at the final stages of black hole evaporation, starting a phase transition-like process that alters the nature of the spacetime, similarly to spontaneous scalarization. We propose that the endpoint is a stable, exotic naked singularity, possible only in modified gravity theories, and avoids some of the pathological features associated with standard naked singularities.

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arXiv2025

Ghost-induced phase transition in the final stages of black hole evaporation

We explore a novel scenario in which a quantum-induced ghost instability drives the natural evolution of an evaporating Schwarzschild black hole toward a stable naked singularity. This process, arising from quadratic curvature corrections to the Einstein-Hilbert action at high energies, circumvents the inconsistencies associated with classical naked singularities. The onset of ghost-driven instability signals a phase transition that fundamentally alters black hole evaporation, rendering the information paradox moot as it merges with the singularity issue. Our findings suggest a new pathway for black hole evolution at high-energy scales, offering insights that may bridge key gaps until a full theory of quantum gravity is realized.

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arXiv2024

A Relativistic Tensorial Model for Fractional Interaction between Dark Matter and Gravity

In a series of recent papers it was shown that several aspects of Dark Matter (DM) phenomenology, such as the velocity profiles of individual dwarfs and spiral galaxies, the scaling relations observed in the latter, and the pressure and density profiles of galaxy clusters, can be explained by assuming the DM component in virialized halos to feel a non-local fractional interaction mediated by gravity. Motivated by the remarkable success of this model, in a recent work we have looked for a general relativistic extension, proposing a theory, dubbed Relativistic Scalar Fractional Gravity or RSFG, in which the trace of the DM stress-energy tensor couples to the scalar curvature via a non-local operator constructed with a fractional power of the d'Alembertian. In this work we construct an extension of that model in which also a non-local coupling between the Ricci tensor and the DM stress energy tensor is present. In the action we encode the normalization between these scalar and tensorial term into two operators $F_0(\Box)$ and $F_2(\Box)$, and we derive the general field equations. We then take the weak field limit of the latter, showing that they reduce to general relativity sourced by an effective stress energy tensor, featuring a non local isotropic pressure and anisotropic stress, even if one starts with the assumption of a pressureless DM fluid. Finally, after having worked out the lensing theory in our setup, we test particularly interesting realizations of our framework against the measured convergence profiles of the individual and stacked clusters of the CLASH sample, finding remarkable consistency with the data.

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arXiv2024

Ultra-compact Objects of Non-minimally Coupled Dark Matter

In the framework of a collisionless dark matter fluid which is non-minimally coupled to gravity, we investigate the existence and properties of static, spherically symmetric solutions of the general relativistic field equations. We show that the non-minimal coupling originates an (anisotropic) pressure able to counteract gravity and to allow the formation of regular, horizonless ultra-compact objects of dark matter (NMC-UCOs). We then analyze the orbits of massive and massless particles in the gravitational field of NMC-UCOs, providing some specific example and a general discussion in terms of phase portraits. Finally, we study the gravitational lensing effects around NMC-UCOs, and effectively describe these in terms of a pseudo-shadow.

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arXiv2024

Scalar Perturbations of Regular Black Holes derived from a Non-Singular Collapse Model in Asymptotic Safety

We investigate the massless scalar field perturbations, focusing on the quasinormal modes spectrum and the ringdown waveform of regular black hole spacetimes derived within the Asymptotic Safety program. In particular, we discuss the stability of a new class of AS black holes recently derived dynamically within a non-singular model of collapse and explore the possibility of detecting signatures of the horizon structure with high-order overtones.

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arXiv2024

Black holes at a crossroads: late-stage evaporation in quadratic gravity

In General Relativity black hole evaporation leads to sudden bursts of energy and loss of information. It can be argued that these phenomena happen in the final stages of evaporation, where the semiclassical approximation needs to be refined with quantum corrections also for the gravitational interaction. A natural way to describe gravity at high energies is to add quadratic curvature terms to the Einstein-Hilbert action, i.e. quadratic gravity. At the cosmological level it is known that its classical solutions can give rise to a model of inflation that matches observations strikingly well, while in an astrophysical context it allows for the possibility of non-Schwarzschild black holes at small masses. These solutions have very peculiar properties, due to the presence of a massive spin-2 particle corresponding to a ghost at the quantum level. The branch of non-Schwarzschild solutions crosses the one of Schwarzschild ones at a specific mass which could be between the one of an asteroid and the Planck mass, depending on the value of a slightly constrained free parameter. By analyzing their dynamical stability and thermodynamical properties, we investigate what could happen to a black hole that has evaporated to this crossing point. While this investigation might not solve the problem of the endpoint of evaporation, it can shed light on the directions it might take during its last moments.

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arXiv2022

The phase diagram of Einstein-Weyl gravity

Thanks to their interpretation as first order correction of General Relativity at high energies, quadratic theories of gravity gained much attention in recent times. Particular attention has been drawn to the Einstein-Weyl theory, where the addition of the squared Weyl tensor to the action opens the possibility of having non-Schwarzschild black holes in the classical spectrum of the theory. Static and spherically symmetric solutions of this theory have been studied and classified in terms of their small scales behaviour; however, a classification of these solutions in terms of the asymptotic gravitational field is still lacking. In this paper we address this point and present a phase diagram of the theory, where the different types of solutions are shown in terms of their mass and the strength of a Yukawa-like correction to the gravitational field. In particular we will show that, in the case of compact stars, different equations of state imply different Yukawa corrections to the gravitational potential, with possible phenomenological implications.

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arXiv2022

The gravitational field of isolated objects in quadratic gravity

When describing gravity at high energies it is natural to introduce terms quadratic in the curvature as first corrections to the Einstein-Hilbert action. Static, spherically symmetric classical solutions are studied in the case of the quantum-motivated $R+R^2+C^{μνρσ}C_{μνρσ}$ theory. In contrast with the case of General Relativity, where the metric is forced to be the Schwarzschild one, a large spectrum of solutions with different gravitational potentials has been found. It is shown how these solutions populate the parameter space of the theory, and some possible phenomenological implications of this modified potential are discussed.

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arXiv2022

Non-symmetric wormholes and localized Big Rip singularities in Einstein-Weyl gravity

The inclusion of the Weyl squared term in the gravitational action is one of the most simple, yet non trivial modifications to General Relativity at high energies. Nevertheless the study of the spherically-symmetric vacuum solutions of this theory has received much attention only in recent times. A new type of asymptotically flat wormhole which does not match symmetrically at a finite radius with another sheet of the spacetime is presented. The outer spacetime is characterized by a newtonian potential with a Yukawa correction, and has gravitational properties that can be arbitrarily close to the ones of a Schwarzschild black hole. The internal spacetime instead possesses a singularity at $r=\infty$ with the topology of a 2-dimensional sphere. The expansion scalar of geodesics reaching this singularity diverges in a finite amount of proper time, with a striking resemblance with the future singularity of the Big Rip cosmological scenario. In terms of the external Yukawa hair and mass $M$, these new wormholes fill a large region of the two-dimensional parameter space of physical solutions with $M>0$. On the contrary black holes, both of Schwarzschild and non-Schwarzschild nature, are confined on a line. We argue that this type of wormholes are ideal black hole mimickers.

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arXiv2021

The gravitational field of a star in quadratic gravity

The characterization of the gravitational field of isolated objects is still an open question in quadratic theories of gravity. We study static equilibrium solutions for a self-gravitating fluid in extensions of General Relativity including terms quadratic in the Weyl tensor $C_{μνρσ}$ and in the Ricci scalar $R$, as suggested by one-loop corrections to classical gravity. By the means of a shooting method procedure we link the total gravitational mass and the strength of the Yukawa corrections associated with the quadratic terms with the fluid properties at the center. It is shown that the inclusion of the $C_{μνρσ}C^{μνρσ}$ coupling in the lagrangian has a much stronger impact than the $R^2$ correction in the determination of the radius and of the maximum mass of a compact object. We also suggest that the ambiguity in the definition of mass in quadratic gravity theories can conveniently be exploited to detect deviations from standard General Relativity.

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arXiv2021

Characterizing black hole metrics in quadratic gravity

The recent discovery of non-Schwarzschild black hole spacetimes has opened new directions of research in higher-derivative gravitational theories. However, despite intense analytical and numerical efforts, the link with the linearized theory is still poorly understood. In this work we address this point for the Einstein-Weyl Lagrangian, whose weak field limit is characterized by the standard massless graviton and a spin-2 ghost. We show that the strength of the Yukawa term at infinity determines the thermal properties of the black hole and the structure of the singularity near $r=0$. Moreover, inspired by recent results in the Asymptotic Safety scenario we investigate the consequences of an imaginary ghost mass. In this case we find a countable set of solutions all characterized by spatial oscillations of typical wavelength determined by the mass of the spin-2 field.

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