Kinematics and ages of Mira variables in the greater solar neighborhood

Details Kinematics and ages of Mira variables in the greater solar neighborhood Kinematics and ages of Mira variables in the greater solar neighborhood

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...275..225w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 275, Dec. 1, 1983, p. 225-239.

Astronomy and Astrophysics

Astrophysics

31

Milky Way Galaxy, Mira Variables, Radial Velocity, Stellar Evolution, Stellar Motions, Variable Stars, Interstellar Gas, Kinematics, Main Sequence Stars, Planetary Nebulae, Red Dwarf Stars, Stellar Mass

Scientific paper

The kinematical information at hand for 124 Mira variables in the greater solar neighborhood leads to a new assessment of the galactic velocity components of each star relative to local circular velocity, and period-spectrum data for the same stars lead to an estimate of their individual main sequence masses and ages. The U, V, and W velocity dispersions are larger for the oldest group of Miras. A comparison of these results with previous investigations of the motions of main sequence stars, in view of two major selection effects, yields good accord between the kinematical properties of the two groups. A study of the motions of planetary nebulae in the greater solar neighborhood leads to the conclusions that the star-spawning interstellar clouds have apparently undergone a slow and largely linear collapse toward the galactic plane, and that the rotary motions of the interstellar medium in the plane have slowly but steadily become less eccentric.

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