Kinematics of Disk Stars in the Solar Neighbourhood

Details Kinematics of Disk Stars in the Solar Neighbourhood Kinematics of Disk Stars in the Solar Neighbourhood

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997esasp.402..621g&link_type=abstract

Proceedings of the ESA Symposium `Hipparcos - Venice '97', 13-16 May, Venice, Italy, ESA SP-402 (July 1997), p. 621-624

Computer Science

27

Scientific paper

Using Hipparcos parallaxes and proper motions together with radial velocity complementary data (Coravel for late type stars and new ground-based data for early type stars) for several thousand B-F type stars, the velocity ellipsoid has been determined as a function of age. The variations with age of the ratio of the velocity dispersions, of the vertex deviation and the age-velocity dispersion relation (AVR) have been estimated. Our results confirm that mixing is not complete at about 0.8 - 1 Gyr. The shape of the velocity ellipsoid changes with time, getting rounder from sigma_U/sigma_V/sigma_W = 1/0.63/0.42 +/- 0.04 at about 1 Gyr to 1/0.7/0.62 +/- 0.04 at 4 - 5 Gyr. The AVR rises to a maximum, thereafter remaining roughly constant; there is no dynamically significant evolution of the disk after about 4 - 5 Gyr. The velocity dispersion in the direction perpendicular to the galactic plane saturates at about 15 - 17 km/s for thin disk stars. The vertex deviation declines with age and remains near zero after 5 Gyr.

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