Stiff Fluid Research Articles

POROELASTICITY AND ROCK PHYSICS TEMPLATES

Two common rock physics templates (RPTs) that are used to identify geological facies and fluid trends derived from well log or pre-stack inverted seismic data involve cross-plotting VP/VS ratio against acoustic impedance, IP (the product of P-wave velocity, VP, and density) and mu-rho against lambda-rho, where mu and lambda are the Lam矣oefficients extracted from P and S-wave velocity, called the LMR, or LambdaMuRho, method. Using well log examples from an Alberta gas well and a deeper North Sea oil well, we show how to superimpose constant mu-rho and lambda-rho curves on a VP/VS versus IP cross-plot, which produce orthogonal trends of stiffness or porosity (from mu-rho) and fluid saturation (from lambda-rho) that match the data trends reasonably well. We then consider the related technique of KMR, or KMuRho, where K represents bulk modulus, and show how to superimpose constant K-rho trends on a VP/VS versus IP cross-plot. Again, we get orthogonal trends of stiffness or porosity (from mu-rho) and fluid saturation (from K-rho), but the fit to our real data examples is less accurate than with LMR. Using Biot-Gassmann poroelasticity theory, we generalize the LMR and KMR approaches into a technique we call FMR (Fluid-Mu-Rho). In the FMR techniques we introduce two new fitting parameters, f and d, where f is a fluid term derived from Biot-Gassmann theory, and d is the dry rock VP/VS ratio squared. When we superimpose fluid trends from the FMR technique on our two well log datasets, and adjust the f and d parameters, we achieve accurate fits to the datasets. Finally, we apply the FMR technique to a seismic case study from the Gulf of Mexico. In an appendix, we compare the FMR technique to the empirical Curved Pseudo-Elastic impedance, or CPEI, and Pseudo-Elastic Impedance for Lithology, or PEIL, methods.

Investigation on hyperbolic Ricci soliton in a perfect fluid spacetime

The aim of this paper is to inspect the geometrical aspects of a perfect fluid spacetime conveying hyperbolic Ricci soliton with torse-forming vector field [Formula: see text]. Next, we have investigated some physical perceptions of perfect fluid spacetime such as dark fluid spacetime, stiff matter fluid spacetime, dust fluid spacetime and radiation fluid spacetime with hyperbolic Ricci soliton in terms of isotropic pressure, the cosmological constant, energy density and gravitational constant. We have also provided two examples of hyperbolic Ricci soliton and hyperbolic Ricci–Bourguignon soliton. Later, we explore the relativistic magneto-fluid spacetime obeying hyperbolic Ricci soliton along with different vector fields.

Charged gravastar model in Rastall theory of gravity

Gravastars are considered as exotic compact objects, may be found at the end of gravitational collapse of massive stars, to resolve the complexities of black holes. In this paper, we analyse the role of charge on the possible formation of an isotropic spherically symmetric gravastar configuration in the framework of Rastall gravity. Gravastar contains three distinct layers viz. (i) Interior region characterised by the equation of state, p=−ρ, which defines the repulsive outward pressure in the radial direction at all points on the thin shell, (ii) Thin shell contains an ultra-relativistic stiff fluid, which is denoted by the equation of state p=ρ following Zel'dovich's criteria for a cold baryonic universe, and can withstand the repulsive pressure exerted by the interior region, and (iii) Exterior region which is the vacuum space-time represented by the Reissner-Nordström solution. Following above specifications, we construct and analyse charged gravastar model in the framework of Rastall gravity, which represents several salient features. The basic physical attributes, viz. proper length, energy, entropy and equation of state parameter of the shell are investigated. In this model, it is interesting to note that for a large radius of the hypersurface (R), the equation of state parameter of the thin shell corresponds to a dark energy equation of state with W(R)→−1. However, for small value of R, W(R)→0, defines dust shell. The stability of the model is ensured through the study of gravitational surface redshift and maximisation of shell entropy within the framework of Rastall theory of gravity.

Accretion mechanism for regular black holes with asymptotically Minkowski Cores and improved Schwarzschild black holes

In this paper, we investigate the fascinating implications of the accretion process for two different kinds of black holes. A detailed analysis of the moving fluid in this accretion process is provided. The radial velocity u(r), the energy density ρ(r), speed of sound a2s and the mass accretion rate Ṁ of the regular black holes and improved Schwarzschild black hole are explored. Interestingly, we consider the most generic black hole space–times with isotropic fluid for this accretion process. The required and necessary physical behaviors around the black holes, such as the radial velocity, the energy density of the moving fluid within the scope of dust, stiff fluid and quintessence, are achieved. Our findings suggest that critical parameters like l in regular black holes, Γ in improved Schwarzschild black holes and the state parameter k are responsible for the accretion mechanism.

Thermal comfort and mechanical analysis of vigorous diamond and diaper weaves; warp, weft and balanced float fabrics with equal thread densities

Diamond (pointed twill) and diaper (herringbone twill) woven assemblies are considered ideal for applications where thermal insulation, heat retention, wrinkle resistance, strength, softness, and breathability attributes are crucial. Limited research has been found on the optimization of thermal comfort and mechanical performance of warp face, weft face and balanced float diaper and diamond woven assemblies. In this work six different woven assemblies have been engineered using cotton (cellulosic yarn) on a dobby machine, having warp face (4/2) weft face (2/4) and balanced float (3/3) based diamond and diaper weave designs with equal number of thread densities. Thermal comfort (dry fluid transmission, thermal resistance, stiffness, and overall wet fluid management capability) and mechanical (tensile, puncture and tear strength) tests were performed for developed woven fabrics. The results of diamond warp face sample showed the highest dry fluid transmission and volume porosity. Diamond weft face specimens showed the highest thermal conductivity behavior and diaper weft face exhibited the highest overall wet fluid management capability behavior. Stiffness was the highest in diamond balanced float. Diamond warp faced fabric showed the highest tearing durability and diaper weft face showed the highest tensile resilience in mechanical performance attributes.

Symmetry-based study and dynamics of casual bulk viscous matter-dominated universe

The dynamics of cosmological expansion is studied for a spatially flat matter-dominated universe filled with barotropic casual bulk viscous fluid. The evolution equation for the Hubble parameter is derived using Friedmann equations and conservation law for the viscous fluid, in which the viscous pressure is modeled by truncated version of the full Israel-Stewart theory of bulk viscosity. We use a Lie symmetry-based approach to study the evolution of the expansion rate of the Universe. The model equation possesses eight-parameter Lie symmetry generators and gives two different analytic group invariant solutions for the Hubble parameter. Expressions for various important cosmological parameters are obtained and values are estimated analytically for the explanation of the evolution dynamics of the Universe. The interesting features of the obtained symmetry-based solutions are that, one satisfies the present acceleration of the Universe, while the other could not support present accelerating phase, rather represents a universe dominated by non-viscous stiff fluid. We make useful checks on the observational constraints on the model parameters from the latest released observational data. The accelerating phase of the current universe is investigated using observational bounds and compared the model under investigation with the Λ\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$\\Lambda $$\\end{document}CDM model. The evolutionary cosmic phases obtained from the analysis of the Lie symmetry-based solutions correspond to the association with the critical points in the equivalent phase space. These interesting features are investigated and analyzed using dynamical systems approach.

Abstract 588: Preclinical evaluation of novel chimeric vesiculovirus mediated expression of proteolytic enzymes targeting two major stromal components of pancreatic ductal adenocarcinoma

Abstract The vesiculovirus genus has recently garnered interest as an oncolytic virotherapy for pancreatic ductal adenocarcinoma (PDAC). A new synthetic chimeric vesiculovirus, VMG, demonstrated efficacy and safety against PDAC both in vitro and in vivo. The therapeutic effectiveness of virotherapies against PDAC is often hindered by immunosuppressive factors in the tumor environment, as well as the presence of hyaluronic acid (HA) and collagen (CN), which increase tumor stiffness and interstitial fluid pressure, leading to reduced drug/oncolytic virus and immune cell penetration into tumor. To address this, we engineered VMG viruses incorporating enzymes PH20, collagenase (CNase), and novel proteolytic enzyme SMC, the latter exhibits both PH20 and CNase-like activity. We characterized these modified viruses for their cytotoxicity and performance in vitro. Various PDAC cell lines displayed varied sensitivity to VMG vectors, yet they showed consistent oncolytic effects relative to the parent VMG-GFP virus. Our results revealed no compromise in viral replication or apoptosis-inducing ability after transgene insertion, which is evident as infectious viral progenies were produced to approximately similar level of magnitude of around 108 TCID50/ml in all the cell line tested. Additionally, the VMG-SMC and VMG-hPH20-CNase variants demonstrated notable enzyme activity. To enhance clinical relevance, we utilized an ex vivo live tumor platform, which indicated around 20% tumor cell death using VMG vectors compared to that of the control, signifying tumor viability and virus replicability 72 hours post-infection. Fluorescent imagery highlighted the viruses' ability to spread and express functional enzymes within tumors. In summary, VMG vectors expressing stroma-degrading proteolytic enzymes can effectively express PH20, CNase and SMC enzymes that degrade stromal barrier of HA and CN without interrupting the replicability, performance, and oncolytic characteristics of the VMG vectors. Future research should prioritize the safety of these vectors and their potential to augment neoantigen expression and immune cell infiltration in vivo, which are the hallmarks of antitumor efficacy. Citation Format: Khandoker Usran Ferdous, Mulu Z. Tesfay, Camila C. Simoes, Aleksandra Cios, Bolni Marius Nagalo. Preclinical evaluation of novel chimeric vesiculovirus mediated expression of proteolytic enzymes targeting two major stromal components of pancreatic ductal adenocarcinoma [abstract]. In: Proceedings of the American Association for Cancer Research Annual Meeting 2024; Part 1 (Regular Abstracts); 2024 Apr 5-10; San Diego, CA. Philadelphia (PA): AACR; Cancer Res 2024;84(6_Suppl):Abstract nr 588.

Lyra cosmologies with the dynamical system perspective

In this study, we revisit the homogeneous and isotropic, spatially curved model in the Lyra geometry framework. We apply the dynamical system approach to study the Universe evolution in model. The present cosmic dynamical system formulation is independent of the model parameter which yields the Universe expansion phases dominated by the stiff fluid, radiation, dark matter and dark energy. These expansion phases in the Lyra model are consistent with the General relativity model. In addition, the displacement vector field of the Lyra geometry model will give rise to the stiff matter dominated phase during early times of the Universe evolution. The cosmographic parameters, EoS parameter and statefinder diagnostic have been utilized in the dynamical system to illustrate the cosmic evolution of the Universe. The numerical solution technique is used to illustrate graphical behaviors of the cosmological parameters. On the basis of dynamical system and numerical analysis, we exhibit that the model explains accelerating universe expansion with transition from the decelerating phase and it will lead to the Λ cold dark matter (ΛCDM) model in the near future.

Preserving non-negative porosity values in a bi-phase elasto-plastic material under Terzaghi’s effective stress principle

Poromechanics is a well-established field of continuum mechanics which seeks to model materials with multiple phases, usually a stiff solid phase and fluid phases of liquids or gases. Applications are widespread particularly in geomechanics where Terzaghi’s effective stress is widely used to solve engineering soil mechanics problems. This approach assumes that the solid phase is incompressible, an assumption that leads to many advantages and simplifications without major loss of fidelity to the real world. Under the assumption of finite (as opposed to infinitesimal) strains, the poromechanics of two- or bi-phase materials gains complexity and while the compressible solid phase case has received attention from researchers, the incompressible case has received less. For the finite strain - incompressible solid phase case there is a fundamental issue with standard material models, in that for some loadings solid skeleton mass conservation is violated and negative Eulerian porosities are predicted. While, to the authors’ best knowledge, acknowledgement of this essential problem has been disregarded in the literature, an elegant solution is presented here, where the constraint on Eulerian porosity can be incorporated into the free energy function for a material. The formulation is explained in detail, soundly grounded in the laws of thermodynamics and validated on a number of illustrative examples.

On the Possibility of a Static Universe

After a century of cosmological observations, we have a solid standard model of cosmology. However, from a theoretical viewpoint, it is a compelling question if the cosmological data inevitably require an expanding universe independently of the theoretical framework. The possibility of obtaining a viable cosmological model with a constant scale-factor is discussed in the context of the Brans–Dicke class of scalar–tensor theories. It is shown that a flat spatial section requires the presence of a stiff matter fluid. However, some kinematical properties of the standard cosmological model can be reproduced. A realistic scenario may require a more complex class of scalar–tensor theories.

Bianchi type III inflationary universe with flat potential and stiff fluid distribution in general relativity

In this study, we looked at the “Bianchi Type III stiff fluid cosmological model in general relativity”. To get an inflationary solution we have used appropriate condition between matric potential. Here n is non-negative integer and B and C are dependent function of time “t”. The structure characteristics of model are also pointed. The behaviour of the model under different physical conditions is also discussed.

New gravastar model in generalised cylindrically symmetric space–time and prediction of mass limit

We present a class of new Gravastar solutions following the works of Mazur and Mottola for a Gravitational Bose–Einstein Condensate (GBEC) star in generalised cylindrically symmetric space–time. A stable gravastar consists of 3 distinct regions, namely: (i) an interior de-Sitter space (p=−ρ), which exerts an outwards repulsive force at all points on the thin shell, (ii) an intermediate thin shell with a slice of finite length separating the interior and exterior regions is supposed to be consisting of an ultra-relativistic stiff fluid, with the equation of state p=ρ and (iii) an exterior vacuum region. This thin shell, which is considered as the critical surface for the quantum phase transition, replaces both the classical de-Sitter space and Schwarzschild event horizon. The new solutions are free from any singularities. The energy density, total energy, proper length, and the entropy of this shell are explored in this model. From the thin shell solution and using Lanczos equations for stress energy density, we have predicted the mass contained into the gravastar shell. The stability of the gravastar model is analysed through the consideration of gravitational surface redshift and entropy calculation. We have also obtained a constraint on the possible mass of the thin shell without violating the condition for stable gravastar configuration. All these features indicate that the present model is physically viable.

Bianchi Type-VIII Inflationary Cosmological Models with Flat Potential and Stiff perfect Fluid Distribution in General Relativity

The objective of this paper is to investigate the behaviour of Bianchi Type-VIII Inflationary Cosmological Models with Flat Potential for Stiff Fluid Distribution. To find the solution of thes models we consider that the expansion theta is proportional to the shear sigma, which leads to B = An and potential V (phi ) as a constant. The behaviour of these models from physical and geometrical aspects are also discussed.

Motion of spinning particles around dynamic phantom AdS black holes

This work is devoted to discussing spinning particles’ motion in the surrounding dynamic phantom AdS Black hole (BH) with phantom scalar field k. The primary goal of this research is to differentiate between the effects of electric and magnetic charges on dynamic phantom AdS BH. The study analyzes the dependence of the innermost stable circular orbit (ISCO), responsible for interactions between charged particles and the external magnetic field, and observes the circular orbits of particles revolving around the compact object. It is also observed that as electric and magnetic charges increase, the ISCO radius decreases. Additionally, stability of orbit, Keplerian frequency, and harmonic oscillations of charged particles are also discussed. We also find the condition, electric and magnetic charges of the dynamic phantom AdS BH effect the energy of the center of mass with magnetized, electrically charged, and neutral particles due to the collision. Lastly, we discuss the accretion process and obtain generalized equations for the speed of sound cs2\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$c^2_{s}$$\\end{document} sec, 4-velocity u(r), energy density ρ(r)\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$\\rho (r)$$\\end{document} and mass (M˙\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$${\\dot{M}}$$\\end{document}). We also plot these physical parameters against constant values of mass, electric and magnetic charges, and distinct values of state parameter ω\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$\\omega $$\\end{document} to study the accretion process. We observe that radial velocity and energy density of the fluid remain positive and negative, and the rate of change of mass is increased and decreased for stiff, dust, quintessence, and phantom-like fluid, respectively.

Structure of 3D gravastars in the context of massive gravity

In this paper, we investigate a new model of (2+1)−dimensional (3D) gravitational vacuum stars (gravastars) with an isotropic matter distribution anti-de Sitter (AdS) spacetime in the context of massive gravity. For this purpose, we explore free singularity models with a specific equation of state. Using Mazur-Mottola's approach, we predict 3D gravastars as alternatives to BTZ black holes in massive gravity. We find analytical solutions to the interior of gravastars free of singularities and event horizons. For a thin shell containing an ultra-relativistic stiff fluid, we discuss length, energy, and entropy. In conclusion, the parameter of massive gravity plays a significant role in predicting the proper length, energy contents and entropy and parameters of gravastars.

Some curvature properties of perfect fluid spacetimes

In this paper we assume that a perfect fluid is the source of the gravitational field while analyzing the solutions to the Einstein field equations. With this new and innovative approach, we investigate some curvature properties of perfect fluid spacetimes. Firstly, we provide a necessary condition for a Lorentzian manifold to be a perfect fluid spacetime. We prove that a conformally flat perfect fluid space-time is a spacetime of quasi constant sectional curvature. Also, we acquire that a conharmonically flat perfect fluid spacetime represents the radiation era. Next, we show that if a stiff matter fluid obeys Yang’s equations, then the vorticity of the fluid vanishes. Moreover, we find that if the Ricci tensor is Killing, then the perfect fluid spacetime is (i) expansion-free and shear-free, and its flow is geodesic, however, not necessarily vorticity-free, and (ii) σ and p are constant. Besides, we establish that Ricci semi-symmetric or Ricci symmetric perfect fluid spacetimes represent either dark matter era, or phantom era. Finally, we acquire that if a perfect fluid is Ricci symmetric, then either the spacetime represents a dark matter era, or a static spacetime.

Efficiency Analysis of the Discrete Element Method Model in Gas‐Fluidized Beds

AbstractThe efficiency and accuracy of the Euler‐Lagrange/discrete element method model were investigated. Accordingly, the stiffness coefficient and fluid time step were changed for different particle numbers and diameters. To derive the optimum parameters for simulations, the obtained results were compared with the measurements. According to the results, the application of higher stiffness coefficients improves the simulation accuracy slightly, however, the average computing time increases exponentially. For time intervals larger than 5 ms, the results indicated that the average computation time is independent of the applied fluid time step, while the simulation accuracy decreases extremely by increasing the size of the fluid time step. Nevertheless, using time steps smaller than 5 ms leads to negligible improvements in the simulation accuracy, though to an exponential rise in the average computing time.

Generalized Vaidya spacetime: Horizons, conformal symmetries, surface gravity and diagonalization

In this paper, the different properties of generalized Vaidya spacetime are considered. We define the location of horizons. We show that the apparent horizon can contain the event horizon. The locations of all types of horizons are compared with the ones in the usual Vaidya spacetime. We investigate the time-like geodesics in this spacetime. New corrections to Schwarzschild and Vaidya cases appear and we give conditions when these corrections are not negligible. Also, we consider the conformal Killing vector and transform the metric to conformally static coordinates. We introduce a new constant of motion along null and time-like geodesics, which is generated by a homothetic Killing vector. The conformally static coordinates allow diagonalizing of the generalized Vaidya spacetime. The surface gravity has been calculated for the dust and stiff fluid cases.

Characterizations of weakly Ricci-symmetric spacetimes and f(ℛ)-gravity

In this paper, we characterize weakly Ricci-symmetric (shortly, [Formula: see text]) spacetimes and their solutions in [Formula: see text]-gravity. It is demonstrated that a [Formula: see text] spacetime represents a stiff matter fluid. In addition, we obtain that a conformally flat [Formula: see text] spacetime is a space of quasi-constant sectional curvature. Moreover, we establish that a Ricci symmetric [Formula: see text] spacetime represents a static spacetime. Finally, we investigate the effect of [Formula: see text] spacetime solutions in [Formula: see text]-gravity.

Mimetic tensor–vector–scalar cosmology: Incorporating dark matter, dark energy and stiff matter

Phenomenological implications of the Mimetic Tensor–Vector–Scalar theory (MiTeVeS) are studied. The theory is an extension of the vector field model of mimetic dark matter, where a scalar field is also incorporated, and it is known to be free from ghost instability. In the absence of interactions between the scalar field and the vector field, the obtained cosmological solution corresponds to the General theory of Relativity (GR) with a minimally-coupled scalar field. However, including an interaction term between the scalar field and the vector field yields interesting dynamics. There is a shift symmetry for the scalar field with a flat potential, and the conserved Noether current, which is associated with the symmetry, behaves as a dark matter component. Consequently, the solution contains a cosmological constant, dark matter and a stiff matter fluid. Breaking the shift symmetry with a non-flat potential gives a natural interaction between dark energy and dark matter.