Abstract
The determination of the rotation curve of the Galaxy, θ(R), where θ is the circular velocity at galactocentric distance R, involves the synthesis of a large body of complementary (and sometimes contradictory) data. The synthesis has to be guided to some extent by theoretical considerations such as studying the distribution of mass in the Galaxy, i.e. by what one “expects” to find. For many years, Galactic structure studies have been guided by the seminal work of Schmidt (1965).
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© 1983 D. Reidel Publishing Company, Dordrecht, Holland
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Knapp, G.R. (1983). The Rotation Curve of the Galaxy. In: Shuter, W.L.H. (eds) Kinematics, Dynamics and Structure of the Milky Way. Astrophysics and Space Science Library, vol 100. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7060-1_34
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DOI: https://doi.org/10.1007/978-94-009-7060-1_34
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