Modern Physics Letters A

In this paper, an information theoretic approach to bounds in superconformal field theories is proposed. It is proved that the supersymmetric Rényi entropy ${\bar{S}}_{\alpha }$ is a monotonically decreasing function of $\alpha$ and $(\alpha -1){\bar{S}}_{\alpha }$ is a concave function of $\alpha$. Under the assumption that the thermal entropy associated with the “replica trick” time circle is bounded from below by the charge at $\alpha \to \infty$, it is further proved that both $\frac{\alpha -1}{\alpha }{\bar{S}}_{\alpha }$ and $(\alpha -1){\bar{S}}_{\alpha }$ monotonically increase as functions of $\alpha$. Because ${\bar{S}}_{\alpha }$ enjoys universal relations with the Weyl anomaly coefficients in even-dimensional superconformal field theories, one therefore obtains a set of bounds on these coefficients by imposing the inequalities of ${\bar{S}}_{\alpha }$. Some of the bounds coincide with Hofman–Maldacena bounds and the others are new. We also check the inequalities for examples in odd-dimensions.

The Weakly Interacting Massive Particles (WIMPs) so far remain one of the most popular candidates for dark matter. If captured gravitationally inside the core of the Sun, these WIMPs may produce high-energy neutrinos as the end product in case they undergo self-annihilations at the solar core. In this work, we address the detectability of such neutrinos at the proposed KM3NeT detector. Upper bounds of the detection rate for such neutrinos at KM3NeT are computed for the case of a generic dark matter scenario and also when specific models for particle dark matter are chosen. In this work, upper bounds of muon event rates for different annihilating dark matter masses are computed for each of the cases of dark matter annihilation channels (e.g. $b\bar{b}$, $W^{+}{W}^{-}$, $Z\bar{Z}$, etc.). These upper bounds are also computed by considering the dark matter scattering cross-section using upper bounds obtained from PandaX-4T direct dark matter search experiment.

In this paper, we consider Dirac equation in (2 + 1)-dimensional curved spacetime in the presence of a scalar potential. It is then shown that the zero energy states are degenerate and they can be obtained when the momentum $k_y$ in the y direction satisfies certain constraints involving the mass parameter and the scalar potential coupling.

In this paper, we apply the method of QCD sum rules to study the doubly heavy tetraquark states $QQ\bar{q}\bar{n}$ with spin-parity $J^P=1^{+}$ and strangeness $S=0,-1$ using careful estimates of the Borel and threshold parameters involved. Masses of the doubly bottom and charmed tetraquarks with isospin $I=0,1/2,1$ are computed precisely via taking into account multifarious condensates up to dimension 10. Compared with the two-heavy meson thresholds, we find that all nonstrange doubly-bottom tetraquarks and a doubly-charmed tetraquarks associated with $J_3$ with $J^P=1^{+}$ are stable against strong decay into two bottom mesons while a doubly-charmed tetraquark associated with current $J_2$ is unstable against strong decay. By the way, weak decay widths of the doubly bottom tetraquarks are also given.

A Bose–Einstein condensation theory for any integer spin using noncommutative quantum mechanics methods is considered. The effective potential is derived as a multipolar expansion in the non-commutativity parameter $(𝜃)$ and, at second order in $𝜃$, our procedure yields to the standard dipole–dipole interaction with ${𝜃}^2$ playing the role of the strength interaction parameter. The generalized Gross–Pitaevskii equation containing nonlocal dipolar contributions is found. For ${}^{52}\mathrm{\text{Cr}}$ isotopes $𝜃=C_{dd}/4\pi$ becomes $\sim$$10^{-11}\mathrm{\text{cm}}$ and, thus for this value of $𝜃$ one cannot distinguish interactions coming from non-commutativity or those of dynamical origin.

In this paper, we study the $F(R,G)$ gravity model with an interacting model by flat-FRW metric in a viscous fluid. We consider that the universe dominates with components of dark matter and dark energy. This means that the dark matter component derives from Extended Bose–Einstein Condensate (EBEC) and the components of dark energy arise from the $F(R,G)$ gravity. After obtaining the Einstein equation, the energy density and the pressure of dark energy are written in terms of the geometry of the curvature and the Gauss–Bonnet terms, and components of dark matter and viscous fluid. Also, the corresponding continuity equations are written with the presence of interaction terms. In what follows, we employ the EBEC regime instead of the normal dark matter by the dark matter Equation of State (EoS) as $p_{\mathrm{\text{dm}}}=\alpha {\rho }_{\mathrm{\text{dm}}}+\beta {\rho }_{\mathrm{\text{dm}}}^2$, which arises from the gravitational form. The EoS can be expressed from the perspective of the virial expansion, in which the first and second terms represent normal dark matter and quantum ground state. Next, the corresponding Friedmann equations reconstruct in terms of the redshift parameter, then by using the scenario of the power-law cosmology for the scale factor, we fit the present model with the Hubble amounts of 51 supernova data by the likelihood analysis. In that case, we acquire the cosmological parameters of dark energy in terms of the redshift parameter, and by plotting these graphs, we see that the universe is currently undergoing an accelerated expansion phase. Finally, we investigate the stability of the present model with the sound speed parameter.

In this paper, we have assumed that the thermodynamic pressure may be generated by the negative cosmological constant and the thermodynamic parameters of the n-dimensional asymptotically Anti-de Sitter (AdS)-Tangherlini black holes are identical with the polytropic gas and modified Chaplygin gas separately. The black hole mass, volume, entropy, and temperature have been written due to the assigned gases’ thermodynamic system. We found the solutions of Einstein’s field equations of n-dimensional black hole for polytropic gas and modified Chaplygin gas. The null energy condition, weak energy condition, strong energy condition, and dominant energy condition have been examined for the fluid sources in n-dimensional black hole system due to both the gases. We found that the four energy conditions completely depend on the model parameters and the dimensions of the spacetime. We have studied the heat engine phenomena for both the black holes and analyzed the work done with the efficiencies due to the Carnot and other cycles.

State $g^{\widehat{n}}{â}^{†m}\left|\alpha \right.〉$ and state ${â}^{†m}{g}^{\widehat{n}}\left|\alpha \right.〉$ are same to state ${â}^{†m}\left|g\alpha \right.〉$, which is called as multi-photon-addition amplified coherent state (MPAACS) by us. Here, $\widehat{n}$, ${â}^{†}$, $\left|\alpha \right.〉$, $g(\ge 1)$, and $m$ are photon number operator, creation operator, coherent state, gain factor, and an integer, respectively. We study mathematical and physical properties for these MPAACSs, including normalization, photon component analysis, Wigner function, effective gain, quadrature squeezing, and equivalent input noise. Actually, the MPAACS, which contains more nonclassicality, is an amplified version of photon-added coherent state (PACS) introduced by Agarwal and Tara [Phys. Rev. A 43, 492 (1991)]. Our work provides theoretical references for implementing amplifiers for light fields.

In this paper, we present a novel measurement-device-independent quantum protocol for Private Set Intersection/ Union Cardinality. This protocol takes weak coherent pulses in the BB84 polarization states as quantum resources, instead of ideal single photons, and only needs to perform Bell state identifications, instead of perfect Bell state measurements. With the current technology, our protocol has better feasibility and higher security than the related quantum protocol. Finally, we verify the correctness and feasibility of the proposed quantum protocol by circuit simulations in IBM Qiskit.