12,839 research outputs found

    Relativistic k-fields with Massless Soliton Solutions in 3+1 Dimensions

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    In this work, the relativistic non-standard Lagrangian densities (k-fields) with massless solutions are generally introduced. Such solutions are not necessarily energetically stable. However, in 3+1 dimensions, we introduce a new k-field model that results in a single non-topological massless solitary wave solution. This special solution is energetically stable; that is, any arbitrary deformation above its background leads to an increase in the total energy. In other words, its energy is zero which is the least energy in all solutions. Hence, it can be called a massless soliton solution

    Noncommutative QED+QCD and Ξ²\beta-function for QED

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    QED based on ΞΈ\theta-unexpanded noncomutative space-time in contrast with the noncommutative QED based on ΞΈ\theta-expanded U(1) gauge theory via the Seiberg-Witten map, is one-loop renormalizable. Meanwhile it suffers from asymptotic freedom that is not in agreement with the experiment. We show that QED part of U⋆(3)Γ—U⋆(1)U_\star(3)\times U_\star(1) gauge group as an appropriate gauge group for the noncommutative QED+QCD, is not only one-loop renormalizable but also has a Ξ²\beta function that can be positive, negative and even zero. In fact the Ξ²\beta function depends on the mixing parameter Ξ΄13\delta_{13} as a free parameter and it will be equal to its counterpart in the ordinary QED for Ξ΄13=0.367Ο€\delta_{13}=0.367\pi.Comment: 33 pages, 30 figures, to appear in PR

    A Class of Nonconvex Penalties Preserving Overall Convexity in Optimization-Based Mean Filtering

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    β„“1\ell_1 mean filtering is a conventional, optimization-based method to estimate the positions of jumps in a piecewise constant signal perturbed by additive noise. In this method, the β„“1\ell_1 norm penalizes sparsity of the first-order derivative of the signal. Theoretical results, however, show that in some situations, which can occur frequently in practice, even when the jump amplitudes tend to ∞\infty, the conventional method identifies false change points. This issue is referred to as stair-casing problem and restricts practical importance of β„“1\ell_1 mean filtering. In this paper, sparsity is penalized more tightly than the β„“1\ell_1 norm by exploiting a certain class of nonconvex functions, while the strict convexity of the consequent optimization problem is preserved. This results in a higher performance in detecting change points. To theoretically justify the performance improvements over β„“1\ell_1 mean filtering, deterministic and stochastic sufficient conditions for exact change point recovery are derived. In particular, theoretical results show that in the stair-casing problem, our approach might be able to exclude the false change points, while β„“1\ell_1 mean filtering may fail. A number of numerical simulations assist to show superiority of our method over β„“1\ell_1 mean filtering and another state-of-the-art algorithm that promotes sparsity tighter than the β„“1\ell_1 norm. Specifically, it is shown that our approach can consistently detect change points when the jump amplitudes become sufficiently large, while the two other competitors cannot.Comment: Submitted to IEEE Transactions on Signal Processin

    Nucleon-Nucleon Scattering in a Strong External Magnetic Field and the Neutrino Emissivity

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    The nucleon-nucleon scattering in a large magnetic background is considered to find its potential to change the neutrino emissivity of the neutron stars. For this purpose we consider the one-pion-exchange approximation to find the NN cross-section in a background field as large as 1015Gβˆ’1018G10^{15}\texttt{G}-10^{18}\texttt{G}. We show that the NN cross-section in neutron stars with temperatures in the range 0.1-5 \texttt{MeV} can be changed up to the one order of magnitude with respect to the one in the absence of the magnetic field. In the limit of the soft neutrino emission the neutrino emissivity can be written in terms of the NN scattering amplitude therefore the large magnetic fields can dramatically change the neutrino emissivity of the neutron stars as well.Comment: 21 pages, 5 figures, to appear in PR
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