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Analysis of the X-ray spectrum of the hot bubble of BD+30°3639

Published online by Cambridge University Press:  08 August 2017

Detlef Schönberner ,
Ralf Jacob ,
René Heller  and
Matthias Steffen
Detlef Schönberner
Affiliation:
Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: deschoenberner@aip.de
Ralf Jacob
Affiliation:
Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: deschoenberner@aip.de
René Heller
Affiliation:
Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: deschoenberner@aip.de
Matthias Steffen
Affiliation:
Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: deschoenberner@aip.de
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Abstract

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We developed a model for wind-blown bubbles with temperature and density profiles based on self-similar solutions including thermal conduction. We constructed also heat-conduction bubbles with chemical discontinuities. The X-ray emission is computed using the well-documented CHIANTI code (v6.0.1). These bubble models are used to (re)analyse the high-resolution X-ray spectrum of the hot bubble of BD+30°3639, and they appeared to be much superior to constant temperature approaches.

We found for the X-ray emission of BD+30°3639 that temperature-sensitive and abundance-sensitive line ratios computed on the basis of heat-conducting wind-blown bubbles and with abundances as found in the stellar photosphere/wind can only be reconciled with the observations if the hot bubble of BD+30°3639 is chemically stratified, i.e. if it contains also a small mass fraction (≃ 3 %) of hydrogen-rich matter immediately behind the conduction front. Neon appears to be strongly enriched, with a mass fraction of at least about 0.06.

Keywords

conductionplanetary nebulae: individual: BD+30°3639stars: abundancesX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 109 - 113
Copyright
Copyright © International Astronomical Union 2017 

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