By Alan H. Batten (auth.), Elias G. Mariolopoulos, Pericles S. Theocaris, L. N. Mavridis (eds.)
When we first approached a few colleagues allover the realm to sound them a few quantity devoted to Professor John Xanthakis at the party of finishing twenty-five years of clinical actions as fellow of the nationwide Academy of Athens, any attainable doubts as to the feasibility of the venture have been quick dispelled by means of their hot and inspiring reaction. very quickly 50 authors from 15 nations, coming from a variety of Professor Xanthakis' quick colleagues, scholars and neighbors joined to supply the 36 contributions integrated during this quantity. a few of those that the place initially approached discovered themselves un capable of give a contribution, a result of time-limit unavoidably imposed. Happi ly, they have been basically few in quantity, and we should always wish to checklist our grat itude to them for his or her reliable needs for the good fortune of the enterprise. Their hot phrases have been one of several resources of inspiring encouragement prolonged to us.
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Additional resources for Compendium in Astronomy: A Volume Dedicated to Professor John Xanthakis on the Occasion of Completing Twenty-five Years of Scientific Activities as Fellow of the National Academy of Athens
It may, in our view, be useful to make comparison of the two groups of information by the methods of the Science of Science. This, first of all, because the determination of star positions has been one of the leading preoccupations of astronomers throughout the past centuries and it might, therefore, be of interest to "detach" this activity from that in Astronomy in general. Secondly, the period 1600 to 1880 witnessed an all-out blossom of sciences, including Astronomy, so it is useful to compare the scientific expansion of Astronomy as a whole with that of one of its parts.
BOUVIER the solution of which yields here a hyperbolic orbit of external focus S (Fig. 2). , ~,,' , , , , ,, ,, ,P C '- --- c 5 Fig. 2. In standard notation we thus write r = p e cos (8-w)-l where e 2 (lO) and w is the polar angle of the hyperbola axis SCP with the direction of V, which is also an asymptotic direction of the hyperbola (Fig. 2). We therefore obtain a one-parameter family of hyperbolae, the parameter being precisely the angle w of any hyperbola axis with the asymptotic V-direction common to all the hyperbolae (Fig.
The distance SS', along the star's line of sight LS is arbitrary. reflection nebula associated with S and we denote by L the line of sight to any other point N' of that contour; L is obviously parallel to L , both making an angle a with the axis Sx, which is also the directiog of the cloud's velocity V. The polar coordinates of M in the xy plane are r = SM and e, the angle PSM; the paraboloid's surface of revolution is described by equation (15) in section 3, namely RADIATION PRESSURE EFFECT ON DUST r = 53 4a (AI) l+cose where cose = x r 2a = SP The line of sight L lies in a plane z = c parallel to Sxy, and letting z = 0 in (AI) brings us back to the equation of the meridional parabola PM, while if z = c, we find the equation (A2) describing a parabola of vertex Q, passing through N and contained in the plane z = C; its parameter is 4a, so that its focus lies below the reference plane Syz.