Dissipation of Magnetic Flux in Primordial Gas Clouds

Abstract

We report the strength of seed magnetic flux of accretion disk surrounding the PopIII stars. The magnetic field in accretion disk might play an important role in the transport of angular momentum because of the turbulence induced by Magneto-Rotational Instability (MRI). On the other hand, since the primordial star-forming clouds contain no heavy elements and grains, they experience much different thermal history and different dissipation history of the magnetic field in the course of their gravitational contraction, from those in the present-day star-forming molecular clouds. In order to assess the magnetic field strength in the accretion disk of PopIII stars, we calculate the thermal history of the primordial collapsing clouds, and investigate the coupling of magnetic field with primordial gas. As a result, we find that the magnetic field strongly couple with primordial gas cloud throughout the collapse, i.e. the magnetic field are frozen to the gas as far as initial field strength satisfies $B\lesssim 10^{-5}(n_{\mathrm{H}}/10^3\mathrm{c}{\mathrm{m}}^{-3}{)}^{0.55}\mathrm{G}$.

arXiv comment23 pages, 10 figures, accepted for publication in ApJ

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Cited by in corpus (35)

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