Abstract
High-quality X-ray observations of planetary nebulae (PNe) have demonstrated that the X-ray-emitting gas in their hot bubbles have temperatures in the small range TX = (1 − 3) × 106 K. However, according to theoretical expectations, adiabatically-shocked wind-blown bubbles should have temperatures up to two orders of magnitude higher. Numerical simulations show that instabilities at the interface between the hot bubble and the nebular material form clumps and filaments that generate an intermediate-temperature turbulent mixing layer. We describe the X-ray properties resulting from simulations of PNe in our Galaxy and the Magellanic Clouds.
Highlights
One of the major probes of the interacting stellar winds model of planetary nebulae (PNe) formation scenario is the detection of hot bubbles
Similar to wind-blown bubbles around massive stars, the X-ray temperatures obtained by means of spectral fitting from hot bubbles in PNe are in the TX = (1 − 3) × 106 K range [5,6], which is not in accordance to what is expected from analytical predictions
All of our models present a clumpy interface between the hot bubble and the outer nebular material formed as a result of a diversity of hydrodynamical and cooling instabilities
Summary
One of the major probes of the interacting stellar winds model of planetary nebulae (PNe) formation scenario is the detection of hot bubbles. Hydrodynamical ablation and photoevaporation of the dense clumps and filaments leads to turbulent mixing of cooler material into the hot gas producing favorable conditions for soft X-ray emission.
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