Astronomy Letters

, Volume 33, Issue 9, pp 571–583

Kinematics of the Scorpius-Centaurus OB association


DOI: 10.1134/S1063773707090010

Cite this article as:
Bobylev, V.V. & Bajkova, A.T. Astron. Lett. (2007) 33: 571. doi:10.1134/S1063773707090010


A fine structure related to the kinematic peculiarities of three components of the Scorpius-Centaurus association (LCC, UCL, and US) has been revealed in the UV-velocity distribution of Gould Belt stars. We have been able to identify the most likely members of these groups by applying the method of analyzing the two-dimensional probability density function of stellar UV velocities that we developed. A kinematic analysis of the identified structural components has shown that, in general, the center-of-mass motion of the LCC, UCL, and US groups follows the motion characteristic of the Gould Belt, notably its expansion. The entire Scorpius-Centaurus complex is shown to possess a proper expansion with an angular velocity parameter of 46 ± 8 km s−1 kpc−1 for the kinematic center with l0 = −40° and R0 = 110 pc found. Based on this velocity, we have estimated the characteristic expansion time of the complex to be 21 ± 4 Myr. The proper rotation velocity of the Scorpius-Centaurus complex is lower in magnitude, is determined less reliably, and depends markedly on the data quality.

Key words

star clusters and associations stellar dynamics Scorpius-Centaurus association Gould Belt kinematics open star clusters 

PACS numbers

98.20.-d 98.10.+z 

Copyright information

© Pleiades Publishing, Inc. 2007

Authors and Affiliations

  1. 1.Pulkovo Astronomical ObservatoryRussian Academy of SciencesSt. PetersburgRussia

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