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Hui Li

Publications and source records attributed to Hui Li.

1,044 records · Page 58Linked to original sources
arXiv2002

Implement Quantum Random Walks with Linear Optics Elements

The quantum random walk has drawn special interests because its remarkable features to the classical counterpart could lead to new quantum algorithms. In this paper, we propose a feasible scheme to implement quantum random walks on a line using only linear optics elements. With current single-photon interference technology, the steps that could be experimentally implemented can be extended to very large numbers. We also show that, by decohering the quantum states, our scheme for quantum random walk tends to be classical.

quant-ph↗
arXiv2002

$π_1$ of Hamiltonian $S^1$ manifolds

Let $(M, ω)$ be a connected, compact symplectic manifold equipped with a Hamiltonian $S^1$ action. We prove that, as fundamental groups of topological spaces, $π_1(M)=π_1(\hbox{minimum})=π_1(\hbox{maximum})=π_1(M_{red})$, where $M_{red}$ is the symplectic quotient at any value in the image of the moment map $ϕ$.

math.SG↗
arXiv2002

Semi-free Hamiltonian circle actions on 6 dimensional symplectic manifolds

Assume $(M, ω)$ is a connected, compact 6 dimensional symplectic manifold equipped with a semi-free Hamiltonian circle action, such that the fixed point set consists of isolated points or compact orientable surfaces. We restrict attention to the case $\dim$ $H^2(M)<3$. We give a complete list of the possible manifolds, determine their equivariant cohomology ring and equivariant Chern classes. Some of these manifolds are classified up to diffeomorphism. We also show the existence for a few cases.

math.SG↗
arXiv2002

Multi-Player and Multi-Choice Quantum Game

We investigate a multi-player and multi-choice quantum game. We start from two-player and two-choice game and the result is better than its classical version. Then we extend it to N-player and N-choice cases. In the quantum domain, we provide a strategy with which players can always avoid the worst outcome. Also, by changing the value of the parameter of the initial state, the probabilities for players to obtain the best payoff will be much higher that in its classical version.

quant-ph↗
arXiv2002

Experimental realization of quantum games on a quantum computer

We generalize the quantum Prisoner's Dilemma to the case where the players share a non maximally entangled states. We show that the game exhibits an intriguing structure as a function of the amount of entanglement with two thresholds which separate a classical region, an intermediate region and a fully quantum region. Furthermore this quantum game is experimentally realized on our nuclear magnetic resonance quantum computer.

quant-ph↗
arXiv2001

Nash Equilibrium in the Quantum Battle of Sexes Game

We investigate Nash Equilibrium in the quantum Battle of Sexes Game. We find the game has infinite Nash Equilibria and all of them leads to the asymmetry result. We also show that there is no unique but infinite Nash Equilibrium in it if we use the quantizing scheme proposed by Eisert et al and the two players are allowed to adopt any unitary operator as his/her strategies.

quant-ph↗
arXiv2001

Remark On Quantum Battle of The Sexes Game

Recently Quantum Battle of The Sexes Game has been studied by Luca Marinatto and Tullio Weber. Yet some important problems exist in their scheme. Here we propose a new scheme to quantize Battle of The Sexes Game, and this scheme will truly remove the dilemma that exists in the classical form of the game.

quant-ph↗
arXiv2000

Quantum Strategy Without Entanglement

In this paper we quantize the Card Game. In the classical version of this game, one player (Alice) can always win with propability 2/3. But when the other player (Bob) is allowed to apply quantum strategy, the original unfair game turns into a fair and zero-sum game. Further more, the procedure in which Bob perform his quantum strategy does not include any ingredient of entanglement.

quant-ph↗
arXiv2000

The Magnetic Fields of the Universe and Their Origin

Recent rotation measure observations of a dozen or so galaxy clusters have revealed a surprisingly large amount of magnetic fields, whose estimated energy and flux are, on average, $\sim 10^{58}$ ergs and $\sim 10^{41}$ G cm$^2$, respectively. These quantities are so much larger than any coherent sums of individual galaxies within the cluster that an efficient galactic dynamo is required. We associate these fields with single AGNs within the cluster and therefore with all galaxies during their AGN phase. Only the central, massive black hole (BH) has the necessary binding energy, $\sim 10^{61}$ ergs. Only the accretion disk during the BH formation has the winding number, $\sim 10^{11}$ turns, necessary to make the gain and magnetic flux. We present a model of the BH accretion disk dynamo that might create these magnetic fields, where the helicity of the $α- Ω$ dynamo is driven by star-disk collisions. The back reaction of the saturated dynamo forms a force-free field helix that carries the energy and flux of the dynamo and redistributes them within the clusters.

astro-ph↗
arXiv1999

Dynamical Symmetry Approach to Periodic Hamiltonians

We show that dynamical symmetry methods can be applied to Hamiltonians with periodic potentials. We construct dynamical symmetry Hamiltonians for the Scarf potential and its extensions using representations of su(1,1) and so(2,2). Energy bands and gaps are readily understood in terms of representation theory. We compute the transfer matrices and dispersion relations for these systems, and find that the complementary series plays a central role as well as non-unitary representations.

solv-int↗
arXiv1999

Group Theory Approach to Band Structure: Scarf and Lame Hamiltonians

The group theoretical treatment of bound and scattering state problems is extended to include band structure. We show that one can realize Hamiltonians with periodic potentials as dynamical symmetries, where representation theory provides analytic solutions, or which can be treated with more general spectrum generating algebraic methods. We find dynamical symmetries for which we derive the transfer matrices and dispersion relations. Both compact and non-compact groups are found to play a role.

cond-mat↗
arXiv1997

The Halo Beaming Model for Gamma-Ray Bursts

We consider a model for gamma-ray bursts (GRBs) from high-velocity neutron stars in the galactic halo. In this model, bursters are born in the galactic disk with large recoil velocities V_r, and GRBs are beamed to within emission cones of half-angle ϕcentered on V_r. We describe scenarios for magnetically -channeled GRBs that have such beaming characteristics. We then make detailed comparisons of this halo beaming model (HBM) to BATSE and PVO data for GRB intensity & angular position distributions. Acceptable fits to observations of over 1000 bursts are obtained for ϕ= 15 - 30 degrees and for a BATSE sampling depth ~ 180 kpc. Present data favor a truly isotropic (cosmological) model over the HBM, but not by a statistically compelling margin. Bursters born in nearby external galaxies, such as M31, are almost entirely undetectable in the HBM because of misdirected beaming. We analyze several refinements of the basic HBM: gamma-ray intensities that vary with angle from the beam axis; non-standard-candle GRB luminosity functions; and models including a subset of bursters that do not escape from the galaxy. We also discuss the energy budgets for the bursters, the origins of their recoils, and the physics of burst beaming and alignment. One possible physical model is based on the magnetar model of soft gamma repeaters (SGRs). Empirical bounds on the rate of formation and peculiar velocities of SGRs imply that there exist ~ 10^4 to ~ 10^7 aged SGRs in the galactic halo within a distance of 100 kpc. The HBM gives an acceptable fit to observations only if it satisfies certain conditions (e.g. ϕ~ 20 deg) which are possible, but for which there exist no clear & compelling theoretical justifications. The cosmological burster hypothesis is more generic and thus more attractive in this sense. (Abbreviated Abstract).

astro-ph↗
arXiv1997

Electron Acceleration and the Production of Nonthermal Electron Distributions in Accretion Disk Coronae

We consider electron acceleration by obliquely propagating fast mode waves in magnetically dominated accretion disk coronae. For low coronal plasma densities, acceleration can exceed Coulomb drag at lower energies and energize electrons out of the thermal background, resulting in a nonthermal tail. The extent of this tail is determined by the balance between acceleration and radiative cooling via inverse Compton scattering and synchrotron emission, and usually goes out to tens of MeV. This will have direct applications for explaining the gamma-rays from several galactic black hole candidates, such as Cyg X-1 and GRO J0422, which show 0.5--5 MeV emissions in excess over what most thermal models predict. Detailed time evolutions of the particle distributions and wave spectra are also presented.

astro-ph↗
arXiv1996

Log-Normal Distributions in Gamma-Ray Burst Time Histories

We propose a new, simple but powerful algorithm to analyze the gamma-ray burst temporal structures based on identifying non-statistical variations (``peaks'') in the time histories. Detailed analyses of the bursts from the third BATSE catalog show that $\sim 30$ bursts have more than 20 peaks individually. Upon identifying most of the peaks in those bursts, we show that the peak fluence $S_i$ and peak interval $δ_i$ distributions within each burst are consistent with log-normal distributions. Furthermore, we show that Gaussian (in linear space) and power-law distributions for peak fluences are ruled out, as is the Poisson distribution for peak intervals.

astro-ph↗
arXiv1996

Gamma-rays from Galactic Black Hole Candidates with Stochastic Particle Acceleration

We consider stochastic particle acceleration in plasmas around stellar mass black holes to explain the emissions above 1 MeV from Galactic black hole candidates. We show that for certain parameter regimes, electrons can overcome Coulomb losses and be accelerated beyond the thermal distribution to form a new population, whose distribution is broad and usually not a power law; the peak energy of the distribution is determined by the balance between acceleration and cooling, with particles piling up around it. Radiation by inverse Compton scattering off the thermal (from background) and non-thermal (produced by acceleration) particles can in principle explain the hard X-ray to gamma-ray emissions from black hole candidates. We present model fits of Cyg X-1 and GRO J0422 in 50 keV -- 5 MeV region observed with OSSE and COMPTEL.

astro-ph↗
arXiv1995

Formation and Radiation Acceleration of Pair Plasmoids Near Galactic Black Holes

We study quantitatively the formation and radiation acceleration of electron-positron pair plasmoids produced by photon-photon collisions near Galactic black holes (GBHs). The terminal ejecta velocity is found to be completely determined by the total disk luminosity, proton loading factor and disk size, with no dependence on the initial velocity. We discuss potential applications to the recently discovered Galactic superluminal sources GRS1915, GROJ1655 and possibly other GBHs.

astro-ph↗
arXiv1995

Stochastic Particle Acceleration near Accreting Black Holes

We consider the stochastic acceleration of particles which results from resonant interactions with plasma waves in black hole magnetospheres. We calculate acceleration rates and escape time scales for protons and electrons resonating with Alfvén waves, and for electrons resonating with whistlers. Assuming either a Kolmogorov or Kraichnan wave spectrum, accretion at the Eddington limit, magnetic field strengths near equipartition, and turbulence energy densities $\sim 10\%$ of the total magnetic field energy density, we find that Alfvén waves accelerate protons to Lorentz factors $\lte 10^4$--$10^6$ before they escape from the system. Acceleration of electrons by fast mode and whistler waves can produce a nonthermal population of relativistic electons whose maximum energy is determined by a competition with radiation losses. Particle energization and outflow is not possible at lower accretion rates, magnetic field strengths, or turbulence levels due to dominant Coulomb losses. Increases in the accretion luminosity relative to the Eddington luminosity can trigger particle acceleration out of the thermal background, and this mechanism could account for the differences between radio-quiet and radio-loud active galactic nuclei. Observations of outflowing radio-emitting components following transient X-ray events in galactic X-ray novae and gamma-ray flares in blazars are in accord with this scenario.

astro-ph↗