Physics
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt.........2h&link_type=abstract
Ph.D. Thesis Wesleyan Univ., Middletown, CT.
Physics
1
Energy Dissipation, Interstellar Magnetic Fields, Ambipolar Diffusion, Background Radiation, Galactic Evolution, Magnetic Flux, Thomson Scattering
Scientific paper
The dissipation of magnetic fields capable of of influencing galaxy formation is calculated through the recombination period and beyond. When ambipolar diffusion is appreciable, the field decreases in strength immediately and steeply. After the ionization has reached its minimum value, decay is more gradual. For initial field strengths at recombination ranging from 1 G to 10 to the -8th power G, the calculated fields at z = 100 vary from 10 to the -8th power G to 10 to the -12th power G, respectively. The spectral density peak shifts dramatically to smaller values, corresponding to a magnetic field length scale at z = 100 that may be six orders of magnitude larger than the length scale implied by flux conservation in an expanding universe. The dissipated magnetic field energy does not cause a temperature rise becasue the coupling between free electrons and photons through Thomson scattering and the enormous heat capacity of the background radiation ensure that the radiation acts as a heat sink.
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