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

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

2011-09-09

arxiv.org/abs/1109.1930v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

(3 pages, 1 figure, to appear in proceedings of the IAU Symposium 283: "Planetary Nebulae: An Eye to the Future", Eds.: A. Man

Scientific paper

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 itsopaque 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 Schoenberner (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.

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