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Investigation of the recombination of the retarded shell of "born-again" CSPNe by time-dependent radiative transfer models
Astrophysics of Galaxies · Submitted 9 Sep 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Describing the physics of such behavior requires a fully time-dependent radiative transfer model.
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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | A standard planetary nebula stays more than 10 000 years in the state of a photoionized nebula. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| s1 | 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). | background 1.00 | 0.05 | 0.03 | asserted 0.92 |
| s2 | When the star exhibits a late Helium flash, however, its ionizing flux stops within a very short period. | background 1.00 | 0.06 | 0.04 | asserted 0.99 |
| s3 | The star then re-appears from itsopaque shell after a few years (or centuries) as a cold giant star without any hard ionizing photons. | background 0.99 | 0.05 | 0.06 | asserted 1.00 |
| s4 | Describing the physics of such behavior requires a fully time-dependent radiative transfer model. | background 0.51 | 0.09 | 0.07 | asserted 1.00 |
| s5 | 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. | background 1.00 | 0.03 | 0.03 | asserted 1.00 |
| s6 | Their argument was the long recombination time scale for such thin media. | background 0.81 | 0.04 | 0.04 | asserted 0.94 |
| s7 | 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. | background 0.60 | 0.05 | 0.06 | hedged possibility 0.65 |
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Original abstract
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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