X-Ray Emission from Jet-Wind Interaction in Planetary Nebulae
arXiv:0711.3265 · doi:10.1016/j.newast.2008.03.002
Abstract
We conduct 2D numerical simulations of jets expanding into the slow wind of asymptotic giant branch stars. We show that the post-shock jets' material can explain the observed extended X-ray emission from some planetary nebulae (PNs). Such jets are thought to shape many PNs, and therefore it is expected that this process will contribute to the X-ray emission from some PNs. In other PNs (not simulated in this work) the source of the extended X-ray emission is the shocked spherical wind blown by the central star. In a small fraction of PNs both sources might contribute, and a two-temperatures gas will fit better the X-ray properties than a one-temperature gas. A spacial separation between these two components is expected.
20 pages, 8 figures
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- Diffuse X-ray Emission from Planetary Nebulae with Nebular O VI
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