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Hyeong-Chan Kim

Publications and source records attributed to Hyeong-Chan Kim.

At least 19 recordsLinked to original sources

Thermalization-Induced Entropy-Rate Representation of Internal Energy in a Damped Quantum Oscillator

We study a harmonic oscillator weakly coupled to a thermal bath and evolving under the standard quantum-optical master equation. For zero-mean Gaussian states, entropy alone does not determine the internal energy because the latter also depends on nonequilibrium Gaussian structure. We show, however, that thermal relaxation yields the exact representation $ E=E(S,\dot S) $ for every mixed Gaussian state evolving under this thermal quantum-optical master equation. Explicitly, \[ E(S,\dot S)= \frac{ων(S)}{ν_{\rm th}} \left[ ν(S)+ \frac{\dot S}{γS'(ν(S))} \right]. \] Once the thermal GKLS equation is assumed, no further expansion in the damping rate, entropy rate, or distance from equilibrium is made. The entropy rate is not an alternative instantaneous state coordinate: it depends on the open-system dynamics and therefore carries information about the coupling to the bath. This is exposed by the isolated limit, where $\dot S=0$ for all Gaussian states and the representation no longer determines the energy. The result thus identifies an exact thermalization-induced dynamical energetic relation, distinct from rate dependence generated by an external driving protocol. We also describe an operational test based on time-resolved purity and energy measurements. At fixed frequency the bath only relaxes pre-existing squeezing. We therefore also consider frequency modulation, which can drive an initially thermal state away from the instantaneous Gibbs family by generating off-Gibbs Gaussian structure. Within a local Gaussian continuation, the bath then relaxes this driven deformation, providing a dynamical realization of the entropy-rate dependence.

cond-mat.stat-mech

Particle creation, clock variables, and relabelling symmetry in pull-back variational fluids

Particle-number conservation is usually built into the pull-back variational formulation of relativistic fluids because the conservative Eulerian variation of the number current is compatible with flow-aligned relabellings only when \(\nabla_a n^a=0\). We revisit this obstruction when the matter-space density itself carries particle-creation information. The result is best organized by the fate of the flow-aligned relabelling. If creation is encoded by the proper-time functional of the deformed worldline, the endpoint variation of proper time cancels the timelike creation residual, so that the relabelling remains a current-level gauge symmetry even when \(Γ_N\neq0\). The price is a history term proportional to acceleration, which vanishes on geodesic flows, including homogeneous FLRW backgrounds. Local descriptions behave differently. With an independent scalar clock or interacting matter spaces, the Eulerian current variation generally retains a timelike residual proportional to \(Γ_Nu^a\). In the Andersson--Comer multi-fluid construction this residual is absorbed by the coupled force balance and represents inter-species conversion. In single-flow self-creation, where no partner matter-space force is available, the same residual becomes the physical scalar mode of the creation clock. A standard local scalar clock satisfying \(u^a\nabla_aΘ=1\) supplies, through its dynamics or constraint, the scalar equation replacing particle-number conservation; in dissipative systems it may be interpreted as entropic time. Clock choices that reproduce the same homogeneous FLRW creation history need not agree at linear order: the proper-time clock gives a creation-rate perturbation locked to the perturbed expansion, whereas a local scalar clock generically produces a gauge-invariant creation-rate mismatch, sourcing non-adiabatic creation pressure and modifying the effective sound speed.

gr-qc

Collective modes and screening in an electric-magnetic dual plasma

We study the linear response of an effective relativistic two-fluid medium carrying separately conserved electric and magnetic charge currents. The model is defined by the duality-symmetric Maxwell equations with electric and magnetic sources, together with Lorentz-force dynamics for two fluids with independent inertia and possible Carter-type entrainment. The magnetic component is treated as an effective charge-carrying constituent, so the analysis uses only the closed two-fluid equations. Around a homogeneous, neutral, and unmagnetized background, the transverse electromagnetic response contains two stable branches whose cutoffs are set by the electric and magnetic plasma frequencies and are exchanged by electric--magnetic duality. In the longitudinal sector, entrainment mixes the electric and magnetic density oscillations, turns their crossing into an avoided crossing, and gives the stability condition $ κ^2<1 ,$ equivalent to positive definiteness of the two-fluid momentum matrix. Resolving the magnetic component into monopole and antimonopole species gives a neutral branch selected by magnetic charge conjugation \(C_m\). In this branch the net magnetic current vanishes, so the long-range monopole field is absent, while the total magnetic density can still produce screened collective response. The resulting picture is that magnetic charge can be statically hidden but dynamically visible. A robust observable signature is the density scaling $ω_{\rm coll}^2\simω_{pm}^2\propto n^0_{(m)},$ which may survive dissipative broadening even when sharp ideal-plasma poles are not resolved. We briefly comment on possible dyonic interpretations of magnetically neutral composites, but the linear-response results do not rely on that interpretation.

physics.plasm-ph

Local Origin of Hidden Symmetry in Rotating Spacetimes

We show that, within a broad stationary-axisymmetric class, Kerr-type separability and hidden symmetry arise as a local consequence of the Einstein equations. Without assuming separability, algebraic speciality, Killing--Yano symmetry, or global boundary conditions, we analyze stationary and axisymmetric geometries in a locally non-rotating orthonormal frame and impose a minimal local equilibrium condition, namely the absence of mixed energy-momentum fluxes. We find that the mixed Einstein equations enforce a rigid projective alignment between radial and angular sectors, uniquely characterized by a constant-Schwarzian constraint. This constraint yields a universal classification of local solutions into Möbius, exponential, and trigonometric branches, of which global regularity selects precisely the Kerr-type sector. In this sense, the kinematical core of Kerr geometry is already fixed locally, and the Schwarzian structure provides the local origin of Kerr rigidity.

gr-qc

Electromagnetism from two matter spaces: mutual helicity and the nondegenerate completion

We show that generic Maxwell fields can be represented within the matter-space framework by introducing two independent matter-space flows. In the one-flow formulation the electromagnetic field strength is the pull-back of a two-form on a three-dimensional matter space and therefore satisfies $F\wedge F=0$, so that a single flow captures only a degenerate, helicity-carrying sector. The minimal completion is obtained by writing $$F=G^{(1)}+G^{(2)},$$ where each sector field $G^{(I)}$ is the pull-back of a matter-space two-form from an independent flow. Each sector is individually degenerate, $G^{(I)}\wedge G^{(I)}=0$, while the full field satisfies $F\wedge F=2G^{(1)}\wedge G^{(2)}$; the invariant excluded by the one-flow theory is thus recovered as an inter-flow quantity. We interpret this structure in terms of mutual helicity: the total helicity decomposes into two self-helicity contributions and a mutual term whose exterior derivative is $F\wedge F$. Hence a configuration with vanishing mutual helicity lies in the degenerate sector, whereas a nondegenerate Maxwell field necessarily carries a nontrivial mutual helicity. A variational principle for the total field recovers the sourced Maxwell equation, the two matter-space variations combining into the full equation whenever the sector kernels intersect trivially. Generic electromagnetism is thereby reconstructed as the minimal coupled completion of two individually degenerate matter-space sectors.

gr-qc

A master equation for Carter-separable stationary axisymmetric spacetimes and compatible sources

We show that the remaining diagonal Einstein equations in the Carter-projective sector of stationary axisymmetric spacetimes are equivalent to a single sourced master equation. The projective structure is taken as the input fixed by the off-diagonal Einstein equations. In the anti-aligned exponential branch, which contains the Kerr--Carter and Plebański--Demiański real section, the remaining diagonal Einstein system reduces to \[ \mathcal L_{\rm CP}[Δ,Y] =16πΣ\left( T_{\hat0\hat0}+T_{\hat3\hat3} \right), \] where \(Δ(r)\) and \(Y(x)\) are the radial and angular structure functions. The reduction is accompanied by two geometric diagonal identities of the Einstein tensor, which become algebraic compatibility conditions on admissible matter sources. In the homogeneous limit, the vacuum--\(Λ\) Kerr--Carter and Plebański--Demiański families are recovered as solutions of the same master operator. We also show the projective covariance of the construction and discuss compatible sources, including the aligned Maxwell field and separable anisotropic examples.

gr-qc

Electromagnetism from relativistic fluid dynamics

We reformulate classical electromagnetism within the matter-space framework of relativistic fluid dynamics. The central assumption is that the relevant degrees of freedom are encoded in differential forms on a three-dimensional matter space and mapped to spacetime by pull-back. The absence of four-forms in matter space imposes nontrivial kinematical constraints on the induced spacetime fields and restricts gauge transformations to those compatible with the flow. Because of this (matter-space) gauge symmetry, the physically relevant sector is retained, and the Aharonov-Bohm phase is naturally associated with the matter-space potential. The construction admits two electromagnetic frames. We argue that the frame identifying the spacetime field strength directly with the intrinsic matter-space two-form is geometrically preferred. In the first frame, the homogeneous sector is fixed by the matter-space structure, while the sourced equation follows from an action-based relativistic-fluid formulation in a first-order setting where the potential and field strength are varied independently and the matter-space constraints are imposed on shell. In the massless case and to quadratic order, locality and the (matter-space) gauge symmetry fix the leading field term in the action uniquely, so the resulting equations provide the minimal dynamical completion once charge carriers are included. We also clarify how duality controls the status of the Bianchi identity in the absence of magnetic charge carriers, and we briefly discuss helicity conservation and a natural nonlinear extension implied by the one-fluid constraints. In the second frame, on the other hand, the matter space 1-form is not directly related with the gauge potential.

physics.gen-ph

Relic Magnetic Fields from Non-Adiabatic Photon Freeze-Out at Recombination

We propose a new mechanism for generating a primordial electromagnetic relic during the recombination--decoupling transition, based on the rate-dependent thermodynamics of the cosmic photon gas. Treating the photon sector as an open system coupled to the electron plasma, we show that a finite Thomson relaxation rate generates a departure from instantaneous thermal equilibrium, leading to non-adiabatic mode squeezing. As this relaxation rate rapidly decreases across recombination, the system quickly loses the ability to further amplify the deviation, and the squeezing freezes out at a small but finite value. This dynamics is naturally described as a narrow transition layer between an adiabatic tracking regime and a post-relaxation freeze-out regime. By a canonical transformation, the reduced evolution equation is recast into a forced oscillator with a smooth effective potential, clarifying the origin of the squeezing and the selection of the relic scale. Projecting the resulting non-equilibrium electromagnetic relic onto the magnetic sector, we derive the corresponding spectrum and show that its characteristic peak is controlled not by the squeezing parameter alone but by the weighted combination \(k^3\mathscr S_k\). In representative realizations, the peak corresponds today to scales of order \(10\)--\(20\) Mpc, while the present-day field amplitude remains extremely small. The mechanism is therefore better viewed as a source of a frozen non-equilibrium electromagnetic relic than as a complete explanation of the observed cosmic magnetic fields.

astro-ph.CO

Stationary axisymmetric systems that allow for a separability structure

We develop a systematic framework for formulating and solving the conditions that lead to separability in stationary, axisymmetric spacetimes in the presence of matter fields. Guided by Carter's metric form, we introduce a general stationary, axisymmetric metric ansatz that allows for a transparent separation of radial and angular variables. This construction yields a broad family of stationary rotating solutions admitting separability structures. To illustrate the applicability of the formalism, we explicitly construct several examples, including a rotating black hole with a global monopole supported by anisotropic matter, as well as a new class of rotating wormhole geometries.

gr-qc

Charged traversable wormholes: charge without charge

We present and investigate charged wormhole solutions of the Einstein-Maxwell equations supported by anisotropic matter fields, with the purpose of establishing their physical plausibility as traversable wormholes. To this end, we examine the flare-out condition and evaluate tidal forces to confirm their traversability. We also analyze light deflection around these wormholes to provide observational implications. Additionally, we attempt to construct rotating generalizations of the solutions by applying and modifying the Newman-Janis algorithm. Our results suggest that the obtained geometries offer a concrete realization of the concept of ``charge without charge".

gr-qc

Charged wormholes in (anti-)de Sitter spacetime

We present a family of charged, traversable wormhole solutions in the presence of a cosmological constant. In de Sitter spacetime, two types of wormhole throats can exist--referred to as typical and cosmological throat--located at small and large radial values, respectively. In anti-de Sitter spacetime, the throat geometry allows for positive, zero, or negative curvature, enabling the possibility of an infinite throat area. We analyze the flare-out condition, a key requirement for the existence of traversable wormholes, which imposes constraints on the equation of state parameters governing the supporting matter. These solutions are shown to be of Petrov type D. Furthermore, we examine radial geodesics of null and timelike particles. In the de Sitter case, particles traverse the wormhole, passing from one throat to the other. In contrast, in the anti-de Sitter case, particles exhibit recurrent oscillatory motion between two asymptotic regions, cyclically disappearing and reappearing across the throats.

gr-qc

Dressing rotating black holes with anisotropic matter

We present a new rotating black hole solution to the Einstein equations as an extension of the Kerr spacetime. Interestingly, the solution we find may not be uniquely characterized by asymptotic parameters such as mass, angular momentum, and charge, thereby it would be the additional hair. We also analyze in detail how this additional characteristics or this hair affects the thermodynamic properties of the black hole.

gr-qc

Temperature upper bound of an ideal gas

We study thermodynamics of a heat-conducting ideal gas system. The study is based on i) the first law of thermodynamics from action formulation which expects heat-dependence of energy density and ii) the existence condition of a (local) Lorentz boost between an Eckart observer and a Landau-Lifshitz observer--a condition that extends the stability criterion of thermal equilibrium. The implications of these conditions include: i) Heat contributes to the energy density through the combination $q/nΘ^2$ where $q$, $n$, and $Θ$ represent heat, the number density, and the temperature, respectively. ii) The energy density has a unique minimum at $q=0$. iii) The temperature upper bound suppresses the heat dependence of the energy density inverse quadratically. This result explains why the expected heat dependence is difficult to observe in ordinary situation thermodynamics.

cond-mat.stat-mech

Collision of two spinning billiard balls and the role of table

We study the collision dynamics of a spinning cue ball approaching a static object ball with equal mass on a plane, common in billiards. While typical collisions in billiards are nearly perfectly elastic, with a restitution coefficient close to 1 and low friction, we explore three deviations from ideal elastic collisions: The non-elastic nature, the friction effects between the balls during collision, the friction between the ball and the table. We describe the detailed collision outcomes, emphasizing the importance of considering frictions. We reveal that friction, both between the balls and with the table, significantly influences the post-collision motions, deviating from the expectations of a purely elastic collision. The insights gained contribute to a better understanding of ball dynamics, impacting strategies and gameplay in billiards.

physics.pop-ph

Temperature of a steady system around a black hole

We study the issue of temperature in a steady system around a black hole event horizon, contrasting it with the appearance of divergence in a thermal equilibrium system. We focus on a spherically symmetric system governed by general relativity, particularly examining the steady state with radial heat conduction. Employing an appropriate approximation, we derive exact solutions that illuminate the behaviors of number density, local temperature, and heat in the proximity of a black hole. We demonstrate that a carefully regulated heat inflow can maintain finite local temperatures at the black hole event horizon, even without considering the back-reaction of matter. This discovery challenges conventional expectations that the local temperature near the event horizon diverges in scenarios of thermal equilibrium. This implications shows that there's an intricate connection between heat and gravity in the realm of black hole thermodynamics.

gr-qc

Steady heat conduction in general relativity

We investigate the steady state of heat conduction in general relativity using a variational approach for two-fluid dynamics. We adopt coordinates based on the Landau-Lifschitz observer because it allows us to describe thermodynamics with heat, formulated in the Eckart decomposition, on a static geometry. Through our analysis, we demonstrate that the stability condition of a thermal equilibrium state arises from the fundamental principle that heat cannot propagate faster than the speed of light. We then formulate the equations governing steady-state heat conduction and introduce a binormal equilibrium condition that the Tolman temperature gradient holds for the directions orthogonal to the heat flow. As an example, we consider radial heat conductions in a spherically symmetric spacetime. We find that the total diffusion over a spherical surface satisfies a red-shifted form, $J(r) \sqrt{-g_{tt}} =$ constant. We also discuss the behavior of local temperature around an event horizon and specify the condition that the local temperature is finite there.

gr-qc

Quantum harmonic oscillators and thermalization

We study a quantum harmonic oscillator undergoing thermalization. To describe the thermalization process, we generalize the Ermakov-Lewis-Riesenfeld (ELR) invariant method for the oscillator. After imposing appropriate conditions on the thermalization process, we introduce an ansatz equation that describes the time evolution effectively. We write down the first law for thermalization in the same form as that for ordinary thermodynamics. Here, the thermalization effect appears through a change of the ELR frequency. Finally, we obtain the oscillator's energy undergoing thermalization as a function of entropy and its time derivative.

quant-ph