Mechanism of Magnetic Flux Loss in Molecular Clouds

Takenori Nakano; Ryoichi Nishi; Toyoharu Umebayashi

doi:10.1086/340587

paper

Mechanism of Magnetic Flux Loss in Molecular Clouds

arXiv:astro-ph/0203223 · doi:10.1086/340587

Abstract

We investigate the detailed processes working in the drift of magnetic fields in molecular clouds. To the frictional force, whereby the magnetic force is transmitted to neutral molecules, ions contribute more than half only at cloud densities $n_{H} < 1 0^{4} cm^{- 3}$ , and charged grains contribute more than 90% at $n_{H} > 1 0^{6} cm^{- 3}$ . Thus grains play a decisive role in the process of magnetic flux loss. Approximating the flux loss time $t_{B}$ by a power law $t_{B} \propto B^{- γ}$ , where $B$ is the mean field strength in the cloud, we find $γ \approx 2$ , characteristic to ambipolar diffusion, only at $n_{H} < 1 0^{7} cm^{- 3}$ . At higher densities, $γ$ decreases steeply with $n_{H}$ , and finally at $n_{H} \approx n_{dec} \approx afew \times 1 0^{11} cm^{- 3}$ , where magnetic fields effectively decouple from the gas, $γ << 1$ is attained, reminiscent of Ohmic dissipation, though flux loss occurs about 10 times faster than by Ohmic dissipation. Ohmic dissipation is dominant only at $n_{H} > 1 \times 1 0^{12} cm^{- 3}$ . While ions and electrons drift in the direction of magnetic force at all densities, grains of opposite charges drift in opposite directions at high densities, where grains are major contributors to the frictional force. Although magnetic flux loss occurs significantly faster than by Ohmic dissipation even at very high densities as $n_{H} \approx n_{dec}$ , the process going on at high densities is quite different from ambipolar diffusion in which particles of opposite charges are supposed to drift as one unit.

34 pages including 9 postscript figures, LaTex, accepted by Astrophysical Journal (vol.573, No.1, July 1, 2002)

Mechanism of Magnetic Flux Loss in Molecular Clouds

Abstract

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