Volume 393, Number 3, October III 2002
|Page(s)||1027 - 1033|
|Published online||01 October 2002|
The correlation between expansion velocity and morphology in planetary nebulae
Instituto de Astronomia y Meteorologia, Avenida Vallarta No. 2602, Col. Arcos Vallarta, C.P. 44130 Guadalajara, Jalisco, Mexico
Corresponding author: email@example.com
Accepted: 11 June 2002
It is usually accepted that the differing morphological classes of planetary nebulae (PNe) arise from progenitors of differing mass. The primary evidence for this derives from the differing galactic distributions of the sources. This, if true, would be expected to result in other differences as well, including variations in the kinematics of the nebular envelopes. We point out here that there is now sufficient evidence to determine that this is the case. We find that BRET-type sources (i.e. nebulae possessing “bipolar rotating episodic jets") have the lowest velocities of expansion VEXP, followed (in order of increasing velocity) by bipolar (BPNe), elliptical and circular nebulae. In addition to this, we find that the distributions of circular, elliptical and bipolar sources are quite distinct, with BPNe being biased towards lower velocities, and circular sources distributed more uniformly. It appears therefore that bipolar outflows contain, within the same shells, evidence for both the highest and lowest velocities of expansion. Whilst the outer wings of these nebulae are expanding at ~175 km s-1, the brighter parts of the shells (probably corresponding to equatorial toroids) have velocities of only ~18 km s-1.
Key words: planetary nebulae: general / ISM: jets and outflows
© ESO, 2002
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