Simulations of the Formation and X-ray Emission from Hot Bubbles in Planetary Nebulae

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 T X = (1 − 3) × 10 6 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.

Models of the Mass-ejection Histories of Pre-planetary Nebulae. II. The Formation of Minkowski’s Butterfly and its Proboscis in M2–9

“…The bulb and the surrounding sheath are approximate analogues of the wind-heated bubble and rim in the inner zones of classical round and elliptical PNe, respectively; see Kwok, Purton, &Fitzgerald, 1978ApJ...219L.125K andToalá &Arthur, 2014MNRAS.443.3486T. The latter paper shows that the radial streamlines can induce highly disruptive thin-shell instabilities along the inner shock rim at the bulb's surface.…”