Kinematics of galactic planetary nebulae

Journal Article · Sun Jul 01 04:00:00 EDT 1979 · Astrophysics (Engl. Transl.); (United States)

DOI:https://doi.org/10.1007/BF01006095· OSTI ID:5840427

Kiosa, M I; Khromov, G S

The classical method of determining the components of the solar motion relative to the centroid of the system of planetary nebulae with known radial velocities is investigated. It is shown that this method is insensitive to random errors in the radial velocities and that low accuracy in determining the coordinates of the solar apex and motion results from the insufficient number of planetaries with measured radial velocities. The planetary nebulae are found not to satisfy well the law of differential galactic rotation with circular orbits. This is attributed to the elongation of their galactic orbits. A method for obtaining the statistical parallax of planetary nebulae is considered, and the parallax calculated from the tau components of their proper motion is shown to be the most reliable.

• Research Organization: AN SSSR, Astronomicheskii Sovet, Moscow, USSR
• OSTI ID: 5840427
• Journal Information: Astrophysics (Engl. Transl.); (United States), Journal Name: Astrophysics (Engl. Transl.); (United States) Vol. 15:1; ISSN ATPYA
• Country of Publication: United States
• Language: English

Related Subjects

640104 -- Astrophysics & Cosmology-- Solar Phenomena
640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
GALAXIES
MAIN SEQUENCE STARS
MEASURING METHODS
MILKY WAY
MOTION
NEBULAE
PLANETARY NEBULAE
RADIAL VELOCITY
ROTATION
STARS
SUN
VELOCITY