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 vollmer_duschl.tex  A&A, Aug 2001, in press
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%astro-ph/0108354


\documentclass{aa}
\usepackage{graphics}

\begin{document}

   \title{The stability of the Circumnuclear Disk clouds\\ in the
          Galactic Centre}

   \titlerunning{The stability of the CND clouds in the GC}

   \author{B.~Vollmer\inst{1,2} \and  W.J.~Duschl\inst{2,1}}

   \offprints{B.~Vollmer, e-mail: bvollmer@mpifr-bonn.mpg.de}

   \institute{Max-Planck-Institut f\"ur Radioastronomie, Auf dem
              H\"ugel 69, 53121 Bonn, Germany. \and
              Institut f\"ur Theoretische Astrophysik der
              Universit\"at Heidelberg, Tiergartenstra{\ss}e 15,
              69121 Heidelberg, Germany.}


   \date{Received / Accepted}


\abstract{The influence of rotation and magnetic fields
on the physical properties of isothermal gas clouds is discussed. 
The presence of rotation and/or magnetic fields
results in an increase of the critical cloud mass with respect
to gravitational instability for clouds of a
given temperature and external pressure. Rotating clouds have
higher densities. Consequently, they are more stable against tidal
shear than non-rotating clouds. They can approach the Galactic
Centre up to a radius of $\sim$2~pc without being disrupted by the
tidal shear due to the gravitational potential. For smaller radii
the clouds either collapse or become tidally disrupted. We suggest
that this mechanism is responsible for the formation of the inner
edge of the Circumnuclear Disk in the Galactic Centre. \keywords{
ISM: clouds -- ISM: evolution -- Galaxy: center} }

\maketitle

\end{document}





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