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Session 54 - Star Clusters, Kinematics and the Galactic Center.
Display session, Wednesday, June 10
Atlas Ballroom,

[54.09] Magnetic Flux Accumulation at the Galactic Center and its Implications for the Strength of the Pre-Galactic Magnetic Field

B. D. G. Chandran, S. C. Cowley, M. Morris (UCLA)

We study the inflow of disk gas towards the Galactic center during the lifetime of the Galaxy and its effect on magnetic field lines frozen-in to the interstellar plasma. While compression leads to a large amplification of the ``vertical'' magnetic field (pointing perpendicular to the disk), ambipolar diffusion efficiently removes from the disk magnetic flux components oriented parallel to the Galactic plane. Contrary to some previous studies, we argue that turbulent diffusion is not effective at removing flux from the disk. On the other hand, we argue that turbulent interchange motions of nearly parallel vertical field lines at the Galactic center enhance the efficiency of magnetic reconnection of neighboring regions of oppositely directed vertical field. This argument suggests that the sign of the present-day vertical field at the Galactic center is uniform. If the Galactic-center field originates in the entrainment of a pre-Galactic field B_0 in radially inflowing interstellar plasma, then observations of the vertical flux through the central 200 pc of our Galaxy yield a measure of the pre-Galactic field that depends on the total mass accreted into the central 200 pc during the Galaxy's lifetime. If this mass is 3\times 10^9 M_\sun, and if the surface density of disk gas is roughly constant over the lifetime of the Galaxy, then B_0 \gtrsim 2\times 10^-7 G, regardless of the angle of the pre-Galactic field with respect to the Galactic plane. The abundance of mechanisms for radial accretion of disk gas suggests that strong magnetic fields should be a generic feature of the centers of spiral galaxies. We also note that cosmic-ray confinement in the strong vertical field at the Galactic center is poor.

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