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We present a study of the X-ray emission from numerical simulations of hotbubbles in planetary nebulae (PNe). High-resolution, two-dimensional,radiation-hydrodynamical simulations of the formation and evolution of hotbubbles in PNe, with and without thermal conduction, are used to calculate theX-ray emission and study its time-dependence and relationship to the changingstellar parameters. Instabilities in the wind-wind interaction zone produceclumps and filaments in the swept-up shell of nebular material. Turbulentmixing and thermal conduction at the corrugated interface can producequantities of intermediate temperature and density gas between the hot, shockedwind bubble and the swept-up photoionized nebular material, which can emit insoft, diffuse X-rays. We use the CHIANTI software to compute synthetic spectrafor the models and calculate their luminosities. We find that models both withconduction and those without can produce the X-ray temperatures andluminosities that are in the ranges reported in observations, although themodels including thermal conduction are an order of magnitude more luminousthan those without. Our results show that at early times the diffuse X-rayemission should be dominated by the contribution from the hot, shocked stellarwind, whereas at later times the nebular gas will dominate the spectrum. Weanalyse the effect of sampling on the resultant spectra and conclude that aminimum of 200 counts is required to reliably reproduce the spectral shape.Likewise, heavily smoothed surface-brightness profiles obtained from low-countdetections of PNe do not provide a reliable description of the spatialdistribution of the X-ray emitting gas.

Formation and X-ray Emission from Hot Bubbles in Planetary Nebulae. II. Hot bubble X-ray emission