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Investigation of the recombination of the retarded shell of “born-again” CSPNe by time-dependent radiative transfer models

Published online by Cambridge University Press:  30 August 2012

Antti Koskela ,
Silvia Dalnodar ,
Ralf Kissmann ,
Anita Reimer ,
Alexander Ostermann  and
Stefan Kimeswenger
Antti Koskela
Affiliation:
1Department of Mathematics, University Innsbruck, Technikerstrasse 13/7, A-6020 Innsbruck, Austria
Silvia Dalnodar
Affiliation:
Institute of Astro- and Particle Physics, University Innsbruck, Technikerstrasse 25/8, A-6020 Innsbruck, Austria
Ralf Kissmann
Affiliation:
Institute of Astro- and Particle Physics, University Innsbruck, Technikerstrasse 25/8, A-6020 Innsbruck, Austria
Anita Reimer
Affiliation:
Institute of Theoretical Physics, University Innsbruck, Technikerstrasse 25/2, A-6020 Innsbruck, Austria
Alexander Ostermann
Affiliation:
1Department of Mathematics, University Innsbruck, Technikerstrasse 13/7, A-6020 Innsbruck, Austria
Stefan Kimeswenger
Affiliation:
Institute of Astro- and Particle Physics, University Innsbruck, Technikerstrasse 25/8, A-6020 Innsbruck, Austria
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Abstract

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A standard planetary nebula stays more than 10 000 years in the state of a photoionized nebula. As long as the timescales of the most important ionizing processes are much smaller, the ionization state can be characterized by a static photoionization model and simulated with codes like CLOUDY (Ferland et al. 1998). When the star exhibits a late helium flash, however, its ionizing flux stops within a very short period. The star then re-appears from its opaque shell after a few years (or centuries) as a cold giant star without any hard ionizing photons. Describing the physics of such behavior requires a fully time-dependent radiative transfer model. Pollacco (1999), Kerber et al. (1999) and Lechner & Kimeswenger (2004) used data of the old nebulae around V605 Aql and V4334 Sgr to derive a model of the pre-outburst state of the CSPN in a static model. Their argument was the long recombination time scale for such thin media. With regard to these models Schönberner (2008) critically raised the question whether a significant change in the ionization state (and thus the spectrum) has to be expected after a time of up to 80 years, and whether static models are applicable at all.

Keywords

radiation mechanisms: generalISM: generalplanetary nebulae: individual (V604 Aql, V4334 Sgr)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 412 - 413
Copyright
Copyright © International Astronomical Union 2012

References

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