Magnetized Turbulent Dynamo in Protogalaxies
Abstract
The prevailing theory for the origin of cosmic magnetic fields is that they have been amplified to their present values by the turbulent dynamo inductive action in the protogalactic and galactic medium. Up to now, in calculation of the turbulent dynamo, it has been customary to assume that there is no back reaction of the magnetic field on the turbulence, as long as the magnetic energy is less than the turbulent kinetic energy. This assumption leads to the kinematic dynamo theory. However, the applicability of this theory to protogalaxies is rather limited. The reason is that in protogalaxies the temperature is very high, and the viscosity is dominated by magnetized ions. As the magnetic field strength grows in time, the ion cyclotron time becomes shorter than the ion collision time, and the plasma becomes strongly magnetized. As a result, the ion viscosity becomes the Braginskii viscosity. Thus, in protogalaxies the back reaction sets in much earlier, at field strengths much lower than those which correspond to fieldturbulence energy equipartition, and the turbulent dynamo becomes what we call the magnetized turbulent dynamo. In this paper we lay the theoretical groundwork for the magnetized turbulent dynamo. In particular, we predict that themore »
 Authors:
 Publication Date:
 Research Org.:
 Princeton Plasma Physics Lab., NJ (US)
 Sponsoring Org.:
 USDOE Office of Science (US)
 OSTI Identifier:
 796126
 Report Number(s):
 PPPL3672.pdf
TRN: US0201455
 DOE Contract Number:
 AC0276CH03073
 Resource Type:
 Technical Report
 Resource Relation:
 Other Information: PBD: 28 Jan 2002
 Country of Publication:
 United States
 Language:
 English
 Subject:
 43 PARTICLE ACCELERATORS; 70 PLASMA PHYSICS AND FUSION TECHNOLOGY; CYCLOTRONS; ION COLLISIONS; KINETIC ENERGY; MAGNETIC FIELDS; ORIGIN; PLASMA; TURBULENCE; VISCOSITY
Citation Formats
Leonid Malyshkin, and Russell M. Kulsrud. Magnetized Turbulent Dynamo in Protogalaxies. United States: N. p., 2002.
Web. doi:10.2172/796126.
Leonid Malyshkin, & Russell M. Kulsrud. Magnetized Turbulent Dynamo in Protogalaxies. United States. doi:10.2172/796126.
Leonid Malyshkin, and Russell M. Kulsrud. 2002.
"Magnetized Turbulent Dynamo in Protogalaxies". United States.
doi:10.2172/796126. https://www.osti.gov/servlets/purl/796126.
@article{osti_796126,
title = {Magnetized Turbulent Dynamo in Protogalaxies},
author = {Leonid Malyshkin and Russell M. Kulsrud},
abstractNote = {The prevailing theory for the origin of cosmic magnetic fields is that they have been amplified to their present values by the turbulent dynamo inductive action in the protogalactic and galactic medium. Up to now, in calculation of the turbulent dynamo, it has been customary to assume that there is no back reaction of the magnetic field on the turbulence, as long as the magnetic energy is less than the turbulent kinetic energy. This assumption leads to the kinematic dynamo theory. However, the applicability of this theory to protogalaxies is rather limited. The reason is that in protogalaxies the temperature is very high, and the viscosity is dominated by magnetized ions. As the magnetic field strength grows in time, the ion cyclotron time becomes shorter than the ion collision time, and the plasma becomes strongly magnetized. As a result, the ion viscosity becomes the Braginskii viscosity. Thus, in protogalaxies the back reaction sets in much earlier, at field strengths much lower than those which correspond to fieldturbulence energy equipartition, and the turbulent dynamo becomes what we call the magnetized turbulent dynamo. In this paper we lay the theoretical groundwork for the magnetized turbulent dynamo. In particular, we predict that the magnetic energy growth rate in the magnetized dynamo theory is up to ten times larger than that in the kinematic dynamo theory. We also briefly discuss how the Braginskii viscosity can aid the development of the inverse cascade of magnetic energy after the energy equipartition is reached.},
doi = {10.2172/796126},
journal = {},
number = ,
volume = ,
place = {United States},
year = 2002,
month = 1
}

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