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  • 1
    Electronic Resource
    Electronic Resource
    Magnetohydrodynamics problems in the interstellar medium : The 40th annual meeting of the division of plasma physics of the american physical society (1999)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Plasmas 6 (1999), S. 1725-1731 
    Details
    ISSN: 1089-7674
    Source: AIP Digital Archive
    Topics: Physics
    Notes: Many defining features of galaxies and their evolution are controlled by their interstellar gas. From 20% to 50% of the interstellar gas in the Milky Way is in molecular clouds, which are also the sites of star formation. Molecular clouds are turbulent, and magnetic fields are strong enough that the turbulence is believed to be magnetohydrodynamic in character. Analytical and numerical estimates suggest that the turbulence would be dissipated in less than the lifetime of the cloud if it were not driven. A small fraction of the mass in molecular clouds fails to be supported against self-gravity and collapses to form stars; star formation also is strongly influenced by magnetohydrodynamic effects. © 1999 American Institute of Physics.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.873431
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  • 2
    Electronic Resource
    Electronic Resource
    Fast reconnection of weak magnetic fields (1998)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Plasmas 5 (1998), S. 247-251 
    Details
    ISSN: 1089-7674
    Source: AIP Digital Archive
    Topics: Physics
    Notes: Fast magnetic reconnection refers to annihilation or topological rearrangement of magnetic fields on a timescale that is independent (or nearly independent) of the plasma resistivity. The resistivity of astrophysical plasmas is so low that reconnection is of little practical interest unless it is fast. Yet, the theory of fast magnetic reconnection is on uncertain ground, as models must avoid the tendency of magnetic fields to pile up at the reconnection layer, slowing down the flow. In this paper it is shown that these problems can be avoided to some extent if the flow is three dimensional. On the other hand, it is shown that in the limited but important case of incompressible stagnation point flows, every flow will amplify most magnetic fields. Although examples of fast magnetic reconnection abound, a weak, disordered magnetic field embedded in stagnation point flow will in general be amplified, and should eventually modify the flow. These results support recent arguments against the operation of turbulent resistivity in highly conducting fluids. © 1998 American Institute of Physics.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.872694
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  • 3
    Electronic Resource
    Electronic Resource
    Tilt stability of rotating current rings with resistive conductors (1985)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Fluids 28 (1985), S. 2517-2523 
    Details
    ISSN: 1089-7666
    Source: AIP Digital Archive
    Topics: Physics
    Notes: The combined effects of rotation and resistive passive conductors on the stability of a rigid current ring in an external magnetic field are studied. Numerical and approximate analytical solutions to the equations of motion are presented, which show that the ring is always tilt unstable on the resistive decay time scale of the conductors, although rotation and eddy currents may stabilize it over short times. Possible applications of our model include spheromaks which rotate or are encircled by energetic particle rings.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.865260
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  • 4
    Electronic Resource
    Electronic Resource
    Slow and steady spirals (1996)
    [s.l.] : Nature Publishing Group
    Nature 383 (1996), S. 758-759 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] SPIRAL nebulae were detected in the eighteenth century, long before it became clear that they were distant galaxies. The magnetic spiral arms reported in this journal in January1 are much subtler features, but their nature may already have been deduced. On page 800 of this issue2, Fan and Lou ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/383758a0
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  • 5
    Electronic Resource
    Electronic Resource
    Magnetic fields in galaxies and beyond (1997)
    [s.l.] : Nature Publishing Group
    Nature 385 (1997), S. 131-136 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Astronomical magnetic fields are generally strong enough to influence the dynamics of gas in present-day galaxies, and may have played an important role in the formation and early evolution of galaxies. Yet the origin of these magnetic fields remains controversial, and observational tests that ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/385131a0
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  • 6
    Electronic Resource
    Electronic Resource
    Astronomy Magnetic bubbles in space (2002)
    [s.l.] : Nature Publishing Group
    Nature 415 (2002), S. 31-33 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Magnetic fields are found in galaxies and clusters of galaxies throughout the Universe. There is even some evidence for magnetized plasma (ionized gases) bridging the space between two galaxy clusters. But the origin of these magnetic fields and their influence on the intergalactic environment ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/415031a
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  • 7
    Electronic Resource
    Electronic Resource
    Magnetostatic atmospheres: A family of isothermal solutions (1982)
    Springer
    Solar physics 76 (1982), S. 261-299 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Most models of large scale solar magnetic fields assume either that the fields are potential or that they are force free. We present a new, analytic, two parameter family of magnetic fields in equilibrium with isothermal plasma in a gravitational field. We discuss these models from the viewpoint of the insight into the balance of magnetic pressure gradient, and gravitational forces that they provide. We show that substantial deviations from the potential field configuration are obtained for plasma β of order unity, and we emphasize the variety of possible relationships between isobars and magnetic fieldlines.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00170987
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  • 8
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    Nonlocal transport of passive scalars in turbulent penetrative convection (2000)
    American Physical Society
    Details
    Publication Date: 2000-01-01
    Print ISSN: 1063-651X
    Electronic ISSN: 1095-3787
    Topics: Physics
    Published by American Physical Society
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  • 9
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    Fast reconnection of weak magnetic fields (1998)
    American Institute of Physics
    Details
    Publication Date: 1998-01-01
    Print ISSN: 1070-664X
    Electronic ISSN: 1089-7674
    Topics: Physics
    Published by American Institute of Physics
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  • 10
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    Interaction of Cosmic Rays with Cold Clouds in Galactic Halos (2017)
    Oxford University Press
    Details
    Publication Date: 2017-01-14
    Description: We investigate the effects of cosmic ray (CR) dynamics on cold, dense clouds embedded in a hot, tenuous galactic halo. If the magnetic field does not increase too much inside the cloud, the local reduction in Alfvén speed imposes a bottleneck on CRs streaming out from the star-forming galactic disc. The bottleneck flattens the upstream CR gradient in the hot gas, implying that multiphase structure could have global effects on CR-driven winds. A large CR pressure gradient can also develop on the outward-facing edge of the cloud. This pressure gradient has two independent effects. The CRs push the cloud upwards, imparting it with momentum. On smaller scales, the CRs pressurize cold gas in the fronts, reducing its density, consistent with the low densities of cold gas inferred in recent Cosmic Origins Spectrograph (COS) observations of local L* galaxies. They also heat the material at the cloud edge, broadening the cloud–halo interface and causing an observable change in interface ionic abundances. Due to the much weaker temperature dependence of CR heating relative to thermal-conductive heating, CR mediated fronts have a higher ratio of low-to-high ions compared to conduction fronts, in better agreement with observations. We investigate these effects separately using 1D simulations and analytic techniques.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press on behalf of The Royal Astronomical Society.
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