Volume 378, Number 2, November I 2001
|Page(s)||587 - 596|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||15 November 2001|
The electron temperature of the inner halo of the Planetary Nebula NGC 6543
Korea Astronomy Observatory, 61-1 Whaam-dong, Yusong-gu, Taejon 305-348, Korea e-mail: email@example.com
2 Sterrewacht Leiden, PO Box 9513, 2300 RA, Leiden, The Netherlands e-mail: firstname.lastname@example.org
3 Dept. of Astronomy and Space Science, Chungnam National University, 220 Kung-dong, Yusong-gu, Taejon 305-764, Korea e-mail: email@example.com
4 Dept. of Earth Science Education, Korea National University of Education, Chung-Buk 363-791, Korea e-mail: firstname.lastname@example.org
Corresponding author: G. Mellema, email@example.com
Accepted: 16 August 2001
We investigate the electron temperature of the inner halo and nebular core regions of NGC 6543, using archival Hubble Space Telescope ( HST) Wide Field Planetary Camera 2 (WFPC2) images taken through narrow band [Oiii] filters. Balick et al. ([CITE]) showed that the inner halo consists of a number of spherical shells. We find the temperature of this inner halo to be much higher (~15 000 K) than that of the bright core nebula (~8500 K). Photo-ionization models indicate that hardening of the UV radiation from the central star cannot be the main source of the higher temperature in the halo region. Using a radiation hydrodynamic simulation, we show that mass loss and velocity variations in the AGB wind can explain the observed shells, as well as the higher electron temperature.
Key words: hydrodynamics / stars: AGB and post-AGB / stars: winds, outflows / ISM: kinematics and dynamics / planetary nebulae: individual: NGC 6543
© ESO, 2001
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