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Dynamical Models for the Milky Way

Abstract:

The only way to map the Galaxy's gravitational potential $\Phi({\bf x})$ and the distribution of matter that produces it is by modelling the dynamics of stars and gas. Observations of the kinematics of gas provide key information about gradients of $\Phi$ within the plane, but little information about the structure of $\Phi$ out of the plane. Traditional Galaxy models {\em assume}, for each of the Galaxy's components, arbitrary flattenings, which together with the components' relative masses ...

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Publication date:
1996-01-10
URN:
uuid:17bccae7-de06-47d3-9bc0-493e14d0e4da
Source identifiers:
167491
Local pid:
pubs:167491
Keywords:

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