Abstract
The stellar winds of the central stars of planetary nebulae play an essential role in the shaping of planetary nebulae. In the interacting stellar winds model, the fast stellar wind injects energy and momentum, which are transferred to the nebular envelope through an X-ray-emitting hot bubble. Together with other physical processes, such as the ionization of the nebular envelope, the asymmetrical mass-loss in the asymptotic giant branch (AGB), and the action of collimated outflows and magnetic fields, the pressurized hot gas determines the expansion and evolution of planetary nebulae. Chandra and XMM-Newton have provided us with detailed information of this hot gas. Here in this talk I will review our current understanding of the effects of the fast stellar wind in the shaping and evolution of planetary nebulae and give some hints of the promising future of this research.
Highlights
Planetary nebulae (PNe) are the descendants of low- to intermediate-mass (0.8–1.0 M ≤ Mi ≤8–10 M ) stars
I review our current understanding of the hot gas in PNe and describe some of the advances that can be achieved by future X-ray observatories
The stellar evolution determines the mechanical luminosity of the stellar wind
Summary
Planetary nebulae (PNe) are the descendants of low- to intermediate-mass As the hot stellar core is exposed, the sudden increase in ionizing flux and fast stellar wind (1000–4000 km·s−1 ) [1] developed by the central star will ionize and sweep up the slow AGB wind to form a PN. In the classical interacting stellar winds (ISW) model [2,3], the expansion of PNe is powered by isotropic fast stellar winds. As these stellar winds encounter the slow AGB wind, a reverse-shock heats the stellar wind up to X-ray-emitting million-Kelvin temperatures, resulting in an onion-like structure similar to that proposed for Wolf–Rayet bubbles by Weaver et al [4]. I review our current understanding of the hot gas in PNe and describe some of the advances that can be achieved by future X-ray observatories
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