77 research outputs found

    Symmetry analysis of the 1+1 dimensional relativistic imperfect fluid dynamics

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    The flow of the relativistic imperfect fluid in two dimensions is discussed. We calculate the symmetry group of the energy-momentum tensor conservation equation in the ultrarelativistic limit. Group-invariant solutions for the incompressible fluid are obtainedComment: 11 pages PS format at http://theor1.ifa.ro/~alexa/iop.p

    On the treatment of ℓ\ell-changing proton-hydrogen Rydberg atom collisions

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    Energy-conserving, angular momentum-changing collisions between protons and highly excited Rydberg hydrogen atoms are important for precise understanding of atomic recombination at the photon decoupling era, and the elemental abundance after primordial nucleosynthesis. Early approaches to ℓ\ell-changing collisions used perturbation theory for only dipole-allowed (Δℓ=±1\Delta \ell=\pm 1) transitions. An exact non-perturbative quantum mechanical treatment is possible, but it comes at computational cost for highly excited Rydberg states. In this note we show how to obtain a semi-classical limit that is accurate and simple, and develop further physical insights afforded by the non-perturbative quantum mechanical treatment

    Numerical solution of perturbed Kepler problem using a split operator technique

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    An efficient geometric integrator is proposed for solving the perturbed Kepler motion. This method is stable and accurate over long integration time, which makes it appropriate for treating problems in astrophysics, like solar system simulations, and atomic and molecular physics, like classical simulations of highly excited atoms in external fields. The key idea is to decompose the hamiltonian in solvable parts and propagate the system according to each term. Two case studies, the Kepler atom in an uniform field and in a monochromatic field, are presented and the errors are analyzed.Comment: 17 pages, 5 figures, submitted to the Journal of Computational Physic

    Theory and simulation of spectral line broadening by exoplanetary atmospheric haze

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    Atmospheric haze is the leading candidate for the flattening of expolanetary spectra, as it's also an important source of opacity in the atmospheres of solar system planets, satellites, and comets. Exoplanetary transmission spectra, which carry information about how the planetary atmospheres become opaque to stellar light in transit, show broad featureless absorption in the region of wavelengths corresponding to spectral lines of sodium, potassium and water. We develop a detailed atomistic model, describing interactions of atomic or molecular radiators with dust and atmospheric haze particulates. This model incorporates a realistic structure of haze particulates from small nano-size seed particles up to sub-micron irregularly shaped aggregates, accounting for both pairwise collisions between the radiator and haze perturbers, and quasi-static mean field shift of levels in haze environments. This formalism can explain large flattening of absorption and emission spectra in haze atmospheres and shows how the radiator - haze particle interaction affects the absorption spectral shape in the wings of spectral lines and near their centers. The theory can account for nearly all realistic structure, size and chemical composition of haze particulates and predict their influence on absorption and emission spectra in hazy environments. We illustrate the utility of the method by computing shift and broadening of the emission spectra of the sodium D line in an argon haze. The simplicity, elegance and generality of the proposed model should make it amenable to a broad community of users in astrophysics and chemistry.Comment: 16 pages, 4 figures, submitted to MNRA

    Demonstrating Universal Scaling in Quench Dynamics of a Yukawa One-Component Plasma

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    The Yukawa one-component plasma (OCP) is a paradigm model for describing plasmas that contain one component of interest and one or more other components that can be treated as a neutralizing, screening background. In appropriately scaled units, interactions are characterized entirely by a screening parameter, Îș\kappa. As a result, systems of similar Îș\kappa show the same dynamics, regardless of the underlying parameters (e.g., density and temperature). We demonstrate this behavior using ultracold neutral plasmas (UNP) created by photoionizing a cold (T≀10T\le10 mK) gas. The ions in UNP systems are well described by the Yukawa model, with the electrons providing the screening. Creation of the plasma through photoionization can be thought of as a rapid quench from Îș0=∞\kappa_{0}=\infty to a final Îș\kappa value set by the electron density and temperature. We demonstrate experimentally that the post-quench dynamics are universal in Îș\kappa over a factor of 30 in density and an order of magnitude in temperature. Results are compared with molecular dynamics simulations. We also demonstrate that features of the post-quench kinetic energy evolution, such as disorder-induced heating and kinetic-energy oscillations, can be used to determine the plasma density and the electron temperature.Comment: 10 pages, 12 figures, to be submitted to Physical Review

    Long-range interactions between a He(23S2 ^3S) atom and a He(23P2 ^3P) atom for like isotopes

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    For the interactions between a He(23S2 ^3S) atom and a He(23P2 ^3P) atom for like isotopes, we report perturbation theoretic calculations using accurate variational wave functions in Hylleraas coordinates of the coefficients determining the potential energies at large internuclear separations. We evaluate the coefficient C3C_{3} of the first order resonant dipole-dipole energy and the van der Waals coefficients C6C_{6}, C8C_{8}, and C10C_{10} for the second order energies arising from the mutual perturbations of instantaneous electric dipole, quadrupole, and octupole interactions. We also evaluate the coefficient C9C_{9} of the leading contribution to the third order energy. We establish definitive values including treatment of the finite nuclear mass for the 3{}^3He(23S2 ^3S)--3{}^3He(23P2 ^3P) and 4{}^4He(23S2 ^3S)--4{}^4He(23P2 ^3P) interactions.Comment: This article has been accepted by Physical Review