Structural properties of the Jagla fluid

Haro, M. López de; Rodríguez‐Rivas, Álvaro; Yuste, S. B.; Santos, Andrés

doi:10.1103/physreve.98.012138

Cited by 18 publications

(14 citation statements)

References 90 publications

(69 reference statements)

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“…7 has a very different form from the SW and AO results. Interestingly, the W line determined for sticky-spheres is similar to that calculated in a recent study of the Jagla model [47] -see their Fig. 8: the W line emanates from the critical point and shifts to higher ρ as T increases, then rises near vertically to the FW line.…”

Section: The Hard-core Yukawa Fluidsupporting

confidence: 84%

On the decay of the pair correlation function and the line of vanishing excess isothermal compressibility in simple fluids

Stopper

Hansen-Goos

Roth

et al. 2019

The Journal of Chemical Physics

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We re-visit the competition between attractive and repulsive interparticle forces in simple fluids and how this governs and connects the macroscopic phase behavior and structural properties as manifest in pair correlation functions. We focus on the asymptotic decay of the total correlation function h(r) which is, in turn, controlled by the form of the pair direct correlation function c(r). The decay of rh(r) to zero can be either exponential (monotonic) if attraction dominates repulsion and exponentially damped oscillatory otherwise. The Fisher-Widom (FW) line separates the phase diagram into two regions characterized by the two different types of asymptotic decay. We show that there is a new and physically intuitive thermodynamic criterion which approximates well the actual FW line. This new criterion defines a line where the isothermal compressibility takes its ideal gas value χT = χ id T . We test our hypothesis by considering four commonly used models for simple fluids. In all cases the new criterion yields a line in the phase diagram that is close to the actual FW line for the thermodynamic state points that are most relevant. We also investigate (Widom) lines of maximal correlation length, emphasizing the importance of distinguishing between the true and Ornstein-Zernike correlation lengths.

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Section: The Hard-core Yukawa Fluidsupporting

confidence: 84%

On the decay of the pair correlation function and the line of vanishing excess isothermal compressibility in simple fluids

Stopper

Hansen-Goos

Roth

et al. 2019

The Journal of Chemical Physics

View full text Add to dashboard Cite

show abstract

“…Thus, in the case of interaction potentials with an attractive tail, Eq. ( 5) must be discarded in the computational evaluation of KB integrals below the so-called Fisher-Widom line [27][28][29][30][31][32][33], where h(r) decays monotonically. On the other hand, even in that case, Eq.…”

Section: Discussionmentioning

confidence: 99%

Finite-size estimates of Kirkwood-Buff and similar integrals

Santos

2018

Phys. Rev. E

Self Cite

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Recently, Krüger and Vlugt [Phys. Rev. E 97, 051301(R) (2018)] have proposed a method to approximate an improper integral ∞ 0 dr F (r), where F (r) is a given oscillatory function, by a finite-range integral L 0 dr F (r)W (r/L) with an appropriate weight function W (x). The method is extended here to an arbitrary (embedding) dimensionality d. A study of three-dimensional Kirkwood-Buff integrals, where F (r) = 4πr 2 h(r), and static structure factors, where F (r) = (4π/q)r sin(qr)h(r), h(r) being the pair correlation function, shows that, in general, a choice d = 3 (e.g., d = 7) for the embedding dimensionality may significantly reduce the error of the approximation ∞ 0 dr F (r) ≃ L 0 dr F (r)W (r/L).

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“…To do that, first of all we study the dynamics in the contracting phase. Performing the change of variable [21]…”

Section: Dynamical Analysismentioning

confidence: 99%

The matter-ekpyrotic bounce scenario in Loop Quantum Cosmology

Haro

Amorós

Saló

2017

J. Cosmol. Astropart. Phys.

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We will perform a detailed study of the matter-ekpyrotic bouncing scenario in Loop Quantum Cosmology using the methods of the dynamical systems theory. We will show that when the background is driven by a single scalar field, at very late times, in the contracting phase, all orbits depict a matter dominated Universe, which evolves to an ekpyrotic phase. After the bounce the Universe enters in the expanding phase, where the orbits leave the ekpyrotic regime going to a kination (also named deflationary) regime. Moreover, this scenario supports the production of heavy massive particles conformally coupled with gravity, which reheats the universe at temperatures compatible with the nucleosynthesis bounds and also the production of massless particles non-conformally coupled with gravity leading to very high reheating temperatures but ensuring the nucleosynthesis success. Dealing with cosmological perturbations, these background dynamics produce a nearly scale invariant power spectrum for the modes that leave the Hubble radius, in the contracting phase, when the Universe is quasi-matter dominated, whose spectral index and corresponding running is compatible with the recent experimental data obtained by PLANCK's team. Big Bang singularity: for example violating the null energy condition in General Relativity by incorporating new forms of matter such as phantom [2] or quintom fields [3], Galileons [4] or phantom condensates [5], or by adding terms to Einstein-Hilbert action [6], but the simplest one is to go beyond General Relativity and consider holonomy corrected Loop Quantum Cosmology (LQC), where a Big Bounce replaces the Big Bang singularity [7]. In fact, other future singularities such as Type I (Big Rip) and Type III (Big Freeze) are also forbbiden in holonomy corrected LQC [8].On the other hand, it is well known that a matter domination period in the contracting phase is dual to the de Sitter regime in the expanding phase [9], which provides a flat power spectrum of cosmological perturbations in the matter bounce scenario. Moreover, an abrupt ekpyrotic phase transition is needed, in the contracting phase, in order to solve the famous Belinsky-Khalatnikov-Lifshitz (BKL) instability: the effective energy density of primordial anisotropy scales as a −6 in the contracting phase [10] and, more important, to produce enough particles which will be responsible for thermalizing the universe in the expanding phase [11,12]. This new scenario named matter-ekpyrotic scenario was introduced in [13], being developed within the two-field model in [14], while in [15] there is a numerical discussion on the primordial anisotropy issue (see [16] for a review). It was treated in the context of Loop Quantum Cosmology in [17], showing that it could be compatible with the new experimental data [18] provided by PLANCK's team (see also [19]).The main goal of the present work is to study mathematically, from the viewpoint of the dynamical systems theory, the matter-ekpyrotic scenario in the context of holonomy corrected LQC. More precisely...

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Structural properties of the Jagla fluid

Cited by 18 publications

References 90 publications

On the decay of the pair correlation function and the line of vanishing excess isothermal compressibility in simple fluids

On the decay of the pair correlation function and the line of vanishing excess isothermal compressibility in simple fluids

Finite-size estimates of Kirkwood-Buff and similar integrals

The matter-ekpyrotic bounce scenario in Loop Quantum Cosmology

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