Abstract
Oort showed long ago in a classic paper (Oort 1932) that one can in principle derive the run of the acceleration perpendicular to the galactic plane by comparing the spatial distribution of stars in the z-direction with the Z-velocity distribution of stars of the same type. In practice, however, no one has succeeded in deriving a valid curve of the acceleration K z; typically the curve turns over in a way that implies negative densities at some distance from the galactic plane. What I would like to do in this brief note is to suggest some possible reasons for this difficulty--specifically, that the types of stars used have been unsuitable.
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Eggen, O.J.: 1965, in Galactic Structure, ed. A. Blaauw and M. Schmidt, p. 111 ( Chicago: Univ. of Chicago Press ).
McCuskey, S.W.: 1965, in Galactic Structure, ed. A. Blaauw and M. Schmidt, p. 1 (Chicago: Univ. of Chicago Press).
Oort, J.H.: 1932, Bull. Astr. Inst. Neth. 6, p. 249.
Sandage, A.: 1957, Astrophys. J. 125, p. 435.
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© 1983 D. Reidel Publishing Company, Dordrecht, Holland
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King, I.R. (1983). On the Analysis of Motions Perpendicular to the Galactic Plane. 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_9
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DOI: https://doi.org/10.1007/978-94-009-7060-1_9
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