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12) become identical with the and 8, if we put ^ = and Gik = 0, when one of the indices Among 39 results of Sects. 7 A=)=0. g. l2 and m^, are 21 in principle observable vanish. Ox, , , quantities whithin the local region which may serve for the determination of the 20 parameters *o. ~, Un -r> Ua ~, Co E Ec> L k > and K ik . Heckmann and Strassl apply an analysis in accordance with their stream formula to the results obtained by Mineur and Guintini 1 for the two-dimensional streaming parallel to the galactic plane of the B stars in our surroundings.

5) 2C-, C 9 The values of q> c and k in this approximation may be derived from accurately determined values of the coefficients of differential rotation A and B. 1) R2 Eqs. 8) ' finally cl = (A C3 H B -B) 2 50 150 Relation between velocity of rotation and 7. distance from the centre for Cepheids in the surroundings of the Sun (Parenago). Fig. 4, B = — 13 (km/sec) /kpc and finally derives ' {A = - \ R% AB J^ = « 10 cmVsec*. 0288 kpc" The velocity of escape 0^ = |/2 may readily be calculated. For the neighbourhood Wc 9?

1 1 J In the case of non-steady states of general ellipsoidal velocity distribution the rotational symmetry will remain, and the characteristics of the motions in the galactic plane may be treated as a two-dimensional case. The essential difference with the presentation in Sects. 7 and 8 ist that, in addition to differential rotations represented by <9 we have motions in the radial directions specified by a velocity 77 proportional to R. A consequence is that we shall have a K, term proportional to the distance (positive or negative) in the radial velocities case of spherical velocity distributions is developed in an approach to a general explanation of spiral structure.

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