scholarly journals Weak gravity versus de Sitter

2021 ◽  
Vol 2021 (4) ◽  
Author(s):  
N. Cribiori ◽  
G. Dall’Agata ◽  
F. Farakos
Keyword(s):  
Supergravity Models ◽  
Critical Points ◽  
Mass Matrix ◽  
De Sitter ◽  
Weak Gravity

Abstract We show that one can uncover a Dine-Seiberg problem for de Sitter critical points in supergravity theories by utilizing the magnetic weak gravity conjecture. We present a large variety of N=2 gauged supergravity models that include vector multiplets and in all cases we find that the weak gravity conjecture threatens de Sitter. A common feature in all such examples is a degenerate mass matrix for the gravitini, which we therefore deem a swampland criterion for de Sitter critical points.

scholarly journals The unbearable lightness of charged gravitini

2021 ◽  
Vol 2021 (10) ◽  
Author(s):  
Gianguido Dall’Agata ◽  
Maxim Emelin ◽  
Fotis Farakos ◽  
Matteo Morittu
Keyword(s):  
Critical Points ◽  
De Sitter ◽  
Large Classes ◽  
Stable Solutions ◽  
De Sitter Vacua ◽  
Weak Gravity

Abstract We prove that charged gravitini cannot have parametrically small or vanishing Lagrangian mass in de Sitter vacua of extended supergravity while respecting the magnetic weak gravity conjecture. This places large classes of de Sitter solutions of gauged supergravity in the swampland, including all known stable solutions of the N=2 theory. We illustrate this result by analyzing a variety of de Sitter critical points of N=2 matter-coupled supergravity that also include new stable de Sitter solutions. Our results provide concrete evidence that (quasi) de Sitter with charged light gravitini should belong to the swampland, which also strongly resonates with the “festina lente” bound.

scholarly journals Weak gravity bounds in asymptotic string compactifications

2021 ◽  
Vol 2021 (6) ◽  
Author(s):  
Brice Bastian ◽  
Thomas W. Grimm ◽  
Damian van de Heisteeg
Keyword(s):  
Black Holes ◽  
Moduli Space ◽  
Mass Formula ◽  
Complex Structure ◽  
Mass Ratio ◽  
De Sitter ◽  
String Compactifications ◽  
Type Iib String Theory ◽  
Bps States ◽  
Weak Gravity

Abstract We study the charge-to-mass ratios of BPS states in four-dimensional $$ \mathcal{N} $$ N = 2 supergravities arising from Calabi-Yau threefold compactifications of Type IIB string theory. We present a formula for the asymptotic charge-to-mass ratio valid for all limits in complex structure moduli space. This is achieved by using the sl(2)-structure that emerges in any such limit as described by asymptotic Hodge theory. The asymptotic charge-to-mass formula applies for sl(2)-elementary states that couple to the graviphoton asymptotically. Using this formula, we determine the radii of the ellipsoid that forms the extremality region of electric BPS black holes, which provides us with a general asymptotic bound on the charge-to-mass ratio for these theories. Finally, we comment on how these bounds for the Weak Gravity Conjecture relate to their counterparts in the asymptotic de Sitter Conjecture and Swampland Distance Conjecture.

scholarly journals Stability and phase space analysis in f(R) theory with generalized exponential f(R) model

2016 ◽  
Vol 25 (10) ◽  
pp. 1650098 ◽  
Author(s):  
R. D. Boko ◽  
M. J. S. Houndjo ◽  
J. Tossa
Keyword(s):  
Dynamical System ◽  
Power Law ◽  
Critical Points ◽  
Dynamical Analysis ◽  
Model Parameters ◽  
Stability Conditions ◽  
De Sitter ◽  
Text Model ◽  
The Stability ◽  
Specific Phase

We have studied in this paper, the stability of dynamical system in [Formula: see text] gravity. We have considered the [Formula: see text] [Formula: see text]-gravity and explored its dynamical analysis. We found six critical points among which only one describes a universe filled of both matter and dominated dark energy. It is shown that these critical points present specific phase spaces described by the corresponding fluids. Furthermore, we have investigated the stability conditions of these critical points and find that these conditions are dependent of the model parameters. We also study the stability of a new power-law [Formula: see text] model with de Sitter and power law solutions.

scholarly journals     2 supergravity models with stable de Sitter vacua

2003 ◽  
Vol 20 (12) ◽  
pp. S487-S493 ◽  
Author(s):  
Pietro Fr ◽  
Mario Trigiante ◽  
Antoine Van Proeyen
Keyword(s):  
Supergravity Models ◽  
De Sitter ◽  
De Sitter Vacua

Thermal corrections of Born–Infeld–anti-de Sitter black hole in massive gravity

2019 ◽  
Vol 34 (27) ◽  
pp. 1950222
Author(s):  
Abdul Jawad ◽  
Shahid Chaudhary
Keyword(s):  
Black Hole ◽  
Critical Points ◽  
Thermal Fluctuations ◽  
Massive Gravity ◽  
Vital Role ◽  
De Sitter ◽  
Logarithmic Corrections ◽  
The Impact

The impact of thermal fluctuations on the thermodynamics of Born–Infeld–anti-de Sitter black hole is being investigated. For this purpose, we analyze the consequences of logarithmic corrections on thermodynamics potentials like Helmholtz and Gibbs. We find out the relations for critical points and stability and observe that thermal corrections play a vital role in them.

scholarly journals Accelerated cosmological expansion without tension in the Hubble parameter

2018 ◽  
Vol 168 ◽  
pp. 08005
Author(s):  
Maurice H.P.M. van Putten
Keyword(s):  
Hubble Parameter ◽  
Accelerated Expansion ◽  
De Sitter ◽  
Local Universe ◽  
Galaxy Dynamics ◽  
Cosmological Expansion ◽  
Extended Range ◽  
Friedmann Robertson Walker ◽  
Galaxy Rotation Curves ◽  
Weak Gravity

The H0-tension problem poses a confrontation of dark energy driving latetime cosmological expansion measured by the Hubble parameter H(z) over an extended range of redshifts z. Distinct values H0 ≃ 73 km s–1 Mpcs–1 and H0 ≃ 68 km s–1 Mpcs–1 obtain from surveys of the Local Universe and, respectively, ΛCBM analysis of the CMB. These are representative of accelerated expansion with H′(0) ≃ 0 by [see formula in PDF] and, respectively, H′(0) > 0 in ΛCDM, where [see formula in PDF] is a fundamental frequency of the cosmological horizon in a Friedmann-Robertson-Walker universe with deceleration parameter q(z) = -1 + (1+z)H–1 H′(z). Explicit solution H(z) = H0 [see formula in PDF] and, respectively, H(z) = H0[see formula in PDF] are here compared with recent data on H(z) over 0 ≲ z ≲ 2.The first is found to be free of tension with H0 from local surveys, while the latter is disfavored at 2:7σ A further confrontation obtains in galaxy dynamics by a finite sensitivity of inertia to background cosmology in weak gravity, putting an upper bound of m ≲ 10–30 eV on the mass of dark matter. A C0 onset to weak gravity at the de Sitter scale of acceleration adS = cH(z), where c denotes the velocity of light, can be seen in galaxy rotation curves covering 0 ≲ z ≲ 2 Weak gravity in galaxy dynamics hereby provides a proxy for cosmological evolution.

scholarly journals Dynamics of quintessence in generalized uncertainty principle

2020 ◽  
Vol 80 (10) ◽  
Author(s):  
Alex Giacomini ◽  
Genly Leon ◽  
Andronikos Paliathanasis ◽  
Supriya Pan
Keyword(s):  
Uncertainty Principle ◽  
Critical Points ◽  
System Analysis ◽  
Field Model ◽  
Generalized Uncertainty Principle ◽  
De Sitter ◽  
Exponential Potential ◽  
Isotropic Universe ◽  
General Potential ◽  
Quintessence Model

AbstractWe investigate the quintessence scalar field model modified by the generalized uncertainty principle in the background of a spatially flat homogeneous and isotropic universe. By performing a dynamical system analysis we examine the nature of the critical points and their stability for two potentials, one is the exponential potential and the other is a general potential. In the case of an exponential potential, we find some new critical points for this modified quintessence scenario that describe the de Sitter universes, and these critical points do not appear in the standard quintessence model with an exponential potential. This is one of the main results of this work. Now for the general potential our analysis shows that the physical properties of the critical points remain exactly the same as for the exponential potential which means that within this modified quintessence scenario all kind of potentials have same behaviour. This kind of result is completely new in cosmology because with the change of the potential, differences are usually expected in all respect.

A de-Sitter weak gravity conjecture

2021 ◽  
Author(s):  
Ignatios Antoniadis ◽  
Karim Benakli
Keyword(s):  
Black Holes ◽  
Mass Formula ◽  
Flat Space ◽  
De Sitter Space ◽  
Large Radius ◽  
De Sitter ◽  
Time Result ◽  
A Charge ◽  
Weak Gravity ◽  
Charge Formula

The study of de-Sitter Reissner–Nordstrøm black holes allows us to uncover a Weak Gravity Conjecture in de-Sitter space. It states that for a given mass [Formula: see text] there should be a state with a charge [Formula: see text] bigger than a minimal value [Formula: see text], depending on the mass and the de-Sitter radius [Formula: see text], in Planck units. This reproduces the well-known flat space–time result [Formula: see text] in the large radius limit (large [Formula: see text]). In the highly curved de-Sitter space, ([Formula: see text]) [Formula: see text] behaves as [Formula: see text]. Finally, we discuss the case of backgrounds from gauged R-symmetry in [Formula: see text] supergravity. This paper is based on [I. Antoniadis and K. Benakli, Fortsch. Phys. 68, 2000054 (2020), arXiv:2006.12512 [hep-th]].

scholarly journals Higher-derivative corrections to entropy and the weak gravity conjecture in Anti-de Sitter space

2020 ◽  
Vol 2020 (9) ◽  
Author(s):  
Sera Cremonini ◽  
Callum R.T. Jones ◽  
James T. Liu ◽  
Brian McPeak
Keyword(s):  
Black Holes ◽  
Equations Of Motion ◽  
Casimir Energy ◽  
Thermodynamic Quantities ◽  
Leading Order ◽  
De Sitter ◽  
Higher Derivative ◽  
Positive Meaning ◽  
Universal Relationship ◽  
Weak Gravity

Abstract We compute the four-derivative corrections to the geometry, extremality bound, and thermodynamic quantities of AdS-Reissner-Nordström black holes for general dimensions and horizon geometries. We confirm the universal relationship between the extremality shift at fixed charge and the shift of the microcanonical entropy, and discuss the consequences of this relation for the Weak Gravity Conjecture in AdS. The thermodynamic corrections are calculated using two different methods: first by explicitly solving the higher-derivative equations of motion and second, by evaluating the higher-derivative Euclidean on-shell action on the leading-order solution. In both cases we find agreement, up to the addition of a Casimir energy in odd dimensions. We derive the bounds on the four-derivative Wilson coefficients implied by the conjectured positivity of the leading corrections to the microcanonical entropy of thermodynamically stable black holes. These include the requirement that the coefficient of Riemann-squared is positive, meaning that the positivity of the entropy shift is related to the condition that c − a is positive in the dual CFT. We discuss implications for the deviation of η/s from its universal value and a potential lower bound.

scholarly journals More on the weak gravity conjecture via convexity of charged operators

2021 ◽  
Vol 2021 (12) ◽  
Author(s):  
Oleg Antipin ◽  
Jahmall Bersini ◽  
Francesco Sannino ◽  
Zhi-Wei Wang ◽  
Chen Zhang
Keyword(s):  
Field Theory ◽  
Conformal Field Theory ◽  
Global Symmetry ◽  
Convexity Property ◽  
De Sitter ◽  
Conformal Dimension ◽  
Conformal Field ◽  
Convexity Properties ◽  
Matter Fields ◽  
Weak Gravity

Abstract The Weak Gravity Conjecture has recently been re-formulated in terms of a particle with non-negative self-binding energy. Because of the dual conformal field theory (CFT) formulation in the anti-de Sitter space, the conformal dimension ∆(Q) of the lowest-dimension operator with charge Q under some global U(1) symmetry must be a convex function of Q. This property has been conjectured to hold for any (unitary) conformal field theory and generalized to larger global symmetry groups. Here we refine and further test the convex charge conjecture via semiclassical computations for fixed charge sectors of different theories in various dimensions. We analyze the convexity properties of the leading and next-to-leading order terms stemming from the semiclassical computation, de facto, extending previous tests beyond the leading perturbative contributions and to arbitrary charges. In particular, the leading contribution is sufficient to test convexity in the semiclassical computations. We also consider intriguing cases in which the models feature a transition from real to complex conformal dimensions either as a function of the charge or number of matter fields. As a relevant example of the first kind, we investigate the O(N) model in 4 + ϵ dimensions. As an example of the second type, we consider the U(N) × U(M) model in 4 − ϵ dimensions. Both models display a rich dynamics where, by changing the number of matter fields and/or charge, one can achieve dramatically different physical regimes. We discover that whenever a complex conformal dimension appears, the real part satisfies the convexity property.

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