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The modelling of the X-ray emission of planetary nebulae

Published online by Cambridge University Press:  15 December 2006

D. Schönberner ,
M. Steffen  and
A. Warmuth
D. Schönberner
Affiliation:
Astrophysikalisches Institut Potsdam, 14482 Potsdam, Germany email: deschoenberner@aip.de, msteffen@aip.de, awarmuth@aip.de
M. Steffen
Affiliation:
Astrophysikalisches Institut Potsdam, 14482 Potsdam, Germany email: deschoenberner@aip.de, msteffen@aip.de, awarmuth@aip.de
A. Warmuth
Affiliation:
Astrophysikalisches Institut Potsdam, 14482 Potsdam, Germany email: deschoenberner@aip.de, msteffen@aip.de, awarmuth@aip.de
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Abstract

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We report on our recent efforts to compute the X-ray emission from the hot, shocked stellar wind gas filling the inner cavity of planetary nebulae. To this end, we updated our 1D hydrodynamics code NEBEL by including a module that computes the heat transfer by thermal conduction across the contact discontinuity separating the hot shocked wind gas from the much cooler nebular material. Given the temperature and density structure of the hot bubble the X-ray emission is computed by means of the CHIANTI code. We find a reasonably close agreement of the computed X-ray luminosities with recent observations of Newton-XMM and Chandra. Our simulations also predict how the X-ray emission depends on the wind luminosity and the stellar parameters.

Keywords

hydrodynamics – radiative transfer – planetary nebulae:general – X-rays:stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 161 - 164
Copyright
© 2006 International Astronomical Union