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 spatial separation between these two components is expected.
Original language | English |
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Pages (from-to) | 563-568 |
Number of pages | 6 |
Journal | New Astronomy |
Volume | 13 |
Issue number | 8 |
DOIs | |
State | Published - Nov 2008 |
Externally published | Yes |
Keywords
- ISM: jets and outflows
- ISM: planetary nebulae: general
- Stars: mass loss
- X-rays: ISM