X-Ray Emission from Jet-Wind Interaction in Planetary Nebulae

Muhammad Akashi; Yohai Meiron; Noam Soker

doi:10.1016/j.newast.2008.03.002

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arXiv · 0711.3265

X-Ray Emission from Jet-Wind Interaction in Planetary Nebulae

Muhammad Akashi·Yohai Meiron·Noam Soker

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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.

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Muhammad Akashi, Yohai Meiron, Noam Soker. 2007-11-21. X-Ray Emission from Jet-Wind Interaction in Planetary Nebulae. https://doi.org/10.1016/j.newast.2008.03.002

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