Gould Belt Kinematics on the Base of the Open Clusters and Ob-Associations

Abstract

The kinematic parameters of the Gould Belt are redetermined using modern data on the motion of nearby young ($\log t<7.91$) open clusters, OB-associations and moving stellar groups. The modelling carried out shows that the residual velocities achieve the maximal values equal to -4 km s${}^{-1}$ for rotation (in the direction of the Galactic rotation) and $+4$ km s${}^{-1}$ for expansion, when the distance from the kinematic centre is about 300 pc. We assumed the following parameters of the Gould Belt centre: $l_{\circ }=128^{\circ }$ and $R_{\circ }=150$ pc. It is shown that the whole structure of the Gould Belt is moving relative to the local standard of rest with a velocity of $10.7\pm 0.7$ km s${}^{-1}$ in the direction towards $l=274\pm 4^{\circ }$, $b=-1\pm 3^{\circ }$. Using the rotation velocity, we obtained the virial estimation of the Gould Belt mass as $1.5\times 10^6{M}_{\odot }$.

5 pages, 2 figures

References in corpus (6)

• The Geneva-Copenhagen survey of the Solar neighbourhood: Ages, metallicities, and kinematic properties of 14,000 F and G dwarfs
• A Hipparcos census of the nearby OB associations
• Local stellar kinematics from Hipparcos data
• Local kinematics of K and M giants from Coravel/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters
• Revisiting the population of Galactic open clusters
• 3D dynamical evolution of the interstellar gas in the Gould Belt