Astrophysik IV: Sternsysteme / Astrophysics IV: Stellar by Frank K. Edmondson (auth.), S. Flügge (eds.)

By Frank K. Edmondson (auth.), S. Flügge (eds.)

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B. V. KUKARKIN: Investigation of the structure and evolution of stellar systems on the basis of variable star studies. Pub!. House of Techn. and Theor. , Moscow-Leningrad 1949. German ed. Akademie-Verlag, Berlin 1954. 3 P. P. PARENAGO: Course of stellar astronomy, 3rd ed. Moscow 1954. 1 2 45 Force at right angles to the galactic plane. Sect. 15. l' being the galactic longitude counted from the centre and b the galactic latitude. 2 kpc and 8 0 at the Sun 234 km/sec, he finds the values of 8 0 (R) in Table 1.

Following OORT1 we may approach somewhat more in detail the process of mixing of the motions in z. Following a star in its orbital motion we call Zo the value of the velocity component Z when the star crosses the galactic plane z = 0. Let a full period of oscillation, until the star again crosses the galactic plane in the same direction, be T. The fraction of T spent in the layer between z and z+dz will be ~~. Most of the stars surrounding the Sun will move in orbits of a fairly limited range of variation in R so that the variation of K(z) for a given z along the orbit will be small.

3, 4, 6,13. 1 2 24 BERTIL LINDBLAD: Galactic Dynamics. Sect. 2. system in the galactic plane. The variation of the true galactic concentration from one sub-system to another is a direct consequence of the variation in the velocity dispersion, because for a greater general dispersion of the velocities relative to the centroid the binding of the objects to the galactic plane becomes less strong, the amplitudes in the motion at right angles to the plane on the average greater, and the true galactic concentration less pronounced.

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