A simplified approach to kinematics of stars in solar neighbourhood

Abstract

For a number of stars from the Solar neighbourhood the eccentricities of their galactocentric orbits are calculated by using a simplified procedure given by Ninković (2011). Eccentricities are calculated from the three-dimensional orbits around the centre of the Milky Way for the same sample of stars, by applying a model with the analytically given gravitational potential as well. The orbital eccentricities (radial span of each star) obtained in these two manners show a satisfactory agreement. It can be concluded that for typical thin-disk stars the use of such a simplified procedure, which requires much less computing time per star, in determining their motion around the Galactic centre is justified. [Projekat Ministarstva nauke Republike Srbije, br. ON176011: Kinematics and dynamics of celestial bodies and systems]

Keywords

• Galaxy: kinematics and dynamics
• solar neighbourhood