Abstract
a comparison of the velocity distributions of the two might illuminate the situation further. McLeod has previously studied the R stars,1 and Parenago has studied the carbon stars as a group,2 but to the writer's knowledge there has been no such work published on the N stars. Weaver has discussed the basic methods of determining velocity ellipsoids and the circumstances in which these methods may be used.3 Dyer has concluded that the fitting of a trivariate normal distribution does not give an adequate description of stellar motions except in a few very special cases.4 He suggests that plots of the residual velocity components in three mutually perpendicular planes be used in describing the kinematics of a given group of stars. The only reliable data available for a kinematical comparison of the R and N stars are radial velocities and thus descriptions as suggested by Dyer are not possible. In the present study the velocity ellipsoids of the two groups are determined even though in some respects, to be discussed further, this approach is not entirely adequate.
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