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% 2005astro.ph.12373B

\documentstyle{article}
\begin{document}
\title{Turbulent Origin of the Galactic-Center Magnetic Field:
Nonthermal Radio Filaments}
\author{Stanislav Boldyrev and Farhad Yusef-Zadeh}
\begin{abstract}
A great deal of study has been carried out over the last twenty years on 
the origin of the magnetic activity in the Galactic center. One of the 
most popular hypotheses assumes milli-Gauss magnetic field with poloidal 
geometry, pervading the inner few hundred parsecs of the Galactic-center 
region. However, there is a growing observational evidence for the 
large-scale distribution of a much weaker field of $B \lesssim 10 {\rm 
\mu}G$ in this region. Here, we propose that the Galactic-center magnetic 
field originates from turbulent activity that is known to be extreme in 
the central hundred parsecs. In this picture the spatial distribution of 
the magnetic field energy is highly intermittent, and the regions of 
strong field have filamentary structures. We propose that the observed 
nonthermal radio filaments appear in (or, possibly, may be identified 
with) such strongly magnetized regions. At the same time, %our theory 
implies that the large-scale %diffuse medium has a weak magnetic field. 
the large-scale diffuse magnetic field is weak.  %We argue that Both 
results of our model can explain the magnetic field measurements of the 
the Galactic-center region. In addition, we discuss the role of ionized 
outflow from stellar clusters in producing the long magnetized filaments 
perpendicular to the Galactic plane.

\end{abstract}

\end{document}