Radial Velocity Analysis of Galactic Planetary Nebulae

Details Radial Velocity Analysis of Galactic Planetary Nebulae Radial Velocity Analysis of Galactic Planetary Nebulae

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..362..222h&link_type=abstract

The Seventh Pacific Rim Conference on Stellar Astrophysics, ASP Conference Series, Vol. 362, Proceedings of the conference held

Astronomy and Astrophysics

Astrophysics

Scientific paper

The spatial distribution of the Galactic planetary nebulae (PNe) and their radial velocities were analyzed for planetary nebulae with known distances. The average radial velocities are derived from 20° × 20° sky area of the galactic plane at 6 azimuthal positions, i.e. l = 0°, 45°, ....., and 315°. A large number of PNe are found in the solar apex direction, while a relatively small number are distributed in the solar antapex direction. Planetary nebulae at l = 90° rapidly approach the LSR or Sun (V_Θ = -51.4 km s-1), while those at l = 180° recede slowly (V_Θ = 6.7 km s-1). The noticeable large velocity difference in the azimuthal direction is likely to be due to the PNs' highly elongated orbits in a particular direction. Although the radial velocities relative to the Local Standard of Rest display a double sinusoidal curve, the large velocity dispersion and other evidence suggest that some interaction between the Sun and PNe exists.

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