78,048 research outputs found

    Can the turbulent galactic dynamo generate large-scale magnetic fields?

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    Large-scale magnetic fields in galaxies are thought to be generated by a turbulent dynamo. However the same turbulence also leads to a small-scale dynamo which generates magnetic noise at a more rapid rate. The efficiency of the large-scale dynamo depends on how this noise saturates. We examine this issue taking into account ambipolar drift, which obtains in a galaxy with significant neutral gas. We argue that, (1) the small-scale dynamo generated field does not fill the volume, but is concentrated into intermittent rope like structures. The flux ropes are curved on the turbulent eddy scales. Their thickness is set by the diffusive scale determined by the effective ambipolar diffusion; (2) For a largely neutral galactic gas, the small-scale dynamo saturates, due to inefficient random stretching, when the peak field in a flux rope has grown to a few times the equipartition value; (3) The average energy density in the saturated small-scale field is sub equipartition, since it does not fill the volume; (4) Such fields neither drain significant energy from the turbulence nor convert eddy motion of the turbulence on the outer scale into wavelike motion. The diffusive effects needed for the large-scale dynamo operation are then preserved until the large-scale field itself grows to near equipartition levels.Comment: 11 pages LaTeX, 2 postscript figures, included. Submitted to MNRA

    Is a Firm\u27s Market Orientation Related to Performance?

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    What Attracts People to the Life Sciences Industry, and What Motivates Them to Stay?

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    Life Sciences is seen as a hub for innovation and an industry that is working to improve the world by creating products to eradicate major diseases and improve the lives of people. One major technology company is a part of this rapidly growing industry that even in tough economic conditions provides a lot of scope for growth and development. This growth is driven, in part, by expanded consumer access to health care in the US through the 2010 Patient Protection and Affordable Care Act. Health care spending is expected to increase on average 4.9% during 2014-2018. Growth is also expected in other parts of the world, like Asia, Australia, Middle East, and Africa. This company faces challenges from competitors. As a result of mergers and consolidations between customers, this company\u27s customer base could become even more concentrated. In order to stay ahead of its competitors, this Fortune 500 company needs to spur innovation and attract and retain the best talent

    Evolving turbulence and magnetic fields in galaxy clusters

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    We discuss, using simple analytical models and MHD simulations, the origin and parameters of turbulence and magnetic fields in galaxy clusters. Three physically distinct regimes can be identified in the evolution of cluster turbulence and magnetic fields. Firstly, the fluctuation dynamo will produce microgauss-strong, random magnetic fields during cluster formation and major mergers. Turbulent velocity of about 300 km/s can be maintained at scales 100-200 kpc. The magnetic field is intermittent, has a smaller scale of 20-30 kpc and average strength of 2 microgauss. Secondly, when major mergers end, turbulent speed and magnetic field undergo a power-law decay, decreasing in strength but increasing in scale by a factor of about two. Thirdly, smaller-mass subclusters and cluster galaxies produce turbulent wakes, with turbulent speeds and magnetic field strengths similar to those quoted above. The velocity scales are about 200 kpc and 10 kpc respectively, and the magnetic field scale is about 6 times smaller. Although these wakes may fill only a small fraction of the cluster volume, their area covering factor can be close to unity. So one can potentially reconcile observations that indicate the coexistence of turbulence with ordered filamentary gas structures, as in the Perseus cluster. Random Faraday rotation measure is estimated to be typically 100-200 rad/m^2, in agreement with observations. We predict detectable synchrotron polarization from cluster radio halos at wavelengths 3-6 cm, if observed at sufficiently high resolution (abridged).Comment: 20 pages, 9 figures, Replaced to match version accepted by MNRA

    A Re-scaled Version of the Foster-Greer-Thorbecke Poverty Indices based on an Association with the Minkowski Distance Function

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    This note advances a family of poverty measures, ??, which are derived as simple, normalized Minkowski distance functions. The ?? indices turn out to be the ?th roots of the corresponding Foster, Greer and Thorbecke P? indices. The re-calibration of P? terms of ?? could have certain possible advantages, which are reviewed in the note. While the ?? indices are not decomposable in the ordinarily understood sense of that term, they are amenable to the completely general decomposition procedure advanced by Shorrocks (?Decomposition Procedures for Distributional Analysis: A Unified Framework Based on the Shapley Value?) and discussed, here, as an application in the poverty context.poverty measures, decomposition
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