45 research outputs found

    Probing Noncommutative Space-Time in the Laboratory Frame

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    The phenomenological investigation of noncommutative space-time in the laboratory frame are presented. We formulate the apparent time variation of noncommutativity parameter ΞΌΜ\theta_{\mu\nu} in the laboratory frame due to the earth's rotation. Furthermore, in the noncommutative QED, we discuss how to probe the electric-like component ΞE→=(Ξ01,Ξ02,Ξ03)\overrightarrow{\theta_{E}}=(\theta_{01},\theta_{02},\theta_{03}) by the process e−e+→γγe^-e^+\to\gamma\gamma at future e−e+e^-e^+ linear collider. We may determine the magnitude and the direction of ΞE→\overrightarrow{\theta_{E}} by detailed study of the apparent time variation of total cross section. In case of us observing no signal, the upper limit on the magnitude of ΞE→\overrightarrow{\theta_E^{}} can be determined independently of its direction.Comment: 12 pages, 7 figures, typos are corrected, one graph have been added in figure

    Reforming Watershed Restoration: Science in Need of Application and Applications in Need of Science

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    The Physics of Star Cluster Formation and Evolution

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    © 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00689-4.Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.Peer reviewe

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