Other
Scientific paper
Nov 1954
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1954mmarc..69...31b&link_type=abstract
Osservazioni e memorie dell'Osservatorio astrofisico di Arcetri, vol. 69, pp.31-62
Other
Scientific paper
The physical and space characteristics of stars of apparent magnitude < 5.5, with peculiar space velocities > 40 km/sec are investigated in this Note. This is a consequence of a study inditiated in 1946 by A. Colacevich and M. C. Ballario concerning a group of 2459 stars. In some other Notes (1), (2), (3), we have given the methods employed for the determination of the space velocities and for the study of the Taurus and Ursa Major clusters, named C1 and C2. We have considered the stars with velocity V < 40 km/sec and V < 49.5 km/sec respectively belonging to C1 and C2, whether because beyond those values the distribution of the velocities is discontinous and with small values, or because of the habit to discuss separately the high velocity stars. The purpose of this Note is to examine the stars omitted in the preceding Notes and among these the stars with V > 40 km/sec. The distribution of the celestial spheres of the apices of the stars proves the existence of two preferential zones indicated with K1 and K2 (fig. 1). Zone K2 includes the apices of 92 stars from galactic longitudes l = 288° and l = 349° and from latitude b = -30° and b = +20°. The mean values of the space velocities, corrected for the sun's motion, and of the apex are given in table III, in wich [sic] are considered, all the stars (v > 40 km/sec), stars with V > 50 km/sec, stars with V > 63 km/sec. This division has been made to bring out the eventual differences between the physical and space characteristics of stars with various velocities and therefore to prove or disprove the necessity to consider separately the stars with V > 63 km/sec wich [sic] show the well known “Oort effect”.
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