The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts
- Autores
- Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Olano, Carlos Alberto; Jiménez, Noelia
- Año de publicación
- 2011
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We propose a scenario for the formation of DA white dwarfs with very thin helium buffers. For these stars we explore the possible occurrence of diffusion-induced CNO-flashes during their early cooling stage. In order to obtain very thin helium buffers, we simulate the formation of low-mass remnants through an asymptotic giant branch (AGB) final/late thermal pulse (AFTP/LTP scenario). Then we calculate the consequent white dwarf cooling evolution by means of a consistent treatment of element diffusion and nuclear burning. Based on physically sound white dwarf models, we find that the range of helium buffer masses for these diffusion-induced novae to occur is significantly smaller than that predicted by the only previous study of this scenario. As a matter of fact, we find that these flashes do occur only in some low-mass (M ≲ 0.6M⊙) and low-metallicity (ZZAMS ≲ 0.001) remnants about 106-107yr after departing from the AGB. For these objects, we expect the luminosity to increase by about 4 orders of magnitude in less than a decade. We also show that diffusion-induced novae should display a very typical eruption light curve, with an increase of about a few magnitudes per year before reaching a maximum ofMV~-5 to -6. Our simulations show that surface abundances after the outburst are characterized by logNH/NHe~-0.15...0.6 and N > C ≳ O by mass fractions. Contrary to previous speculations we show that these events are not recurrent and do not change substantially the final H-content of the cool (DA) white dwarf. Finally, with the aid of model predictions we discuss the possibility that Nova Vul 1670 (CK Vul) and the recently proposed [WN/WC]-central stars of planetary nebulae could be observational counterparts of this diffusion-induced nova scenario. We conclude that, despite discrepancies with observations, the scenario offers one of the best available explanations for CK Vul and, with minor modifications, explains the observed properties of [WN/WC]-central stars of planetary nebulae.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Stars: AGB and post-AGB
Stars: individual: CK Vul
Stars: individual: PB8
Stars: Wolf-Rayet
White dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/83994
Ver los metadatos del registro completo
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The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterpartsMiller Bertolami, Marcelo MiguelAlthaus, Leandro GabrielOlano, Carlos AlbertoJiménez, NoeliaCiencias AstronómicasStars: AGB and post-AGBStars: individual: CK VulStars: individual: PB8Stars: Wolf-RayetWhite dwarfsWe propose a scenario for the formation of DA white dwarfs with very thin helium buffers. For these stars we explore the possible occurrence of diffusion-induced CNO-flashes during their early cooling stage. In order to obtain very thin helium buffers, we simulate the formation of low-mass remnants through an asymptotic giant branch (AGB) final/late thermal pulse (AFTP/LTP scenario). Then we calculate the consequent white dwarf cooling evolution by means of a consistent treatment of element diffusion and nuclear burning. Based on physically sound white dwarf models, we find that the range of helium buffer masses for these diffusion-induced novae to occur is significantly smaller than that predicted by the only previous study of this scenario. As a matter of fact, we find that these flashes do occur only in some low-mass (M ≲ 0.6M⊙) and low-metallicity (ZZAMS ≲ 0.001) remnants about 106-107yr after departing from the AGB. For these objects, we expect the luminosity to increase by about 4 orders of magnitude in less than a decade. We also show that diffusion-induced novae should display a very typical eruption light curve, with an increase of about a few magnitudes per year before reaching a maximum ofMV~-5 to -6. Our simulations show that surface abundances after the outburst are characterized by logNH/NHe~-0.15...0.6 and N > C ≳ O by mass fractions. Contrary to previous speculations we show that these events are not recurrent and do not change substantially the final H-content of the cool (DA) white dwarf. Finally, with the aid of model predictions we discuss the possibility that Nova Vul 1670 (CK Vul) and the recently proposed [WN/WC]-central stars of planetary nebulae could be observational counterparts of this diffusion-induced nova scenario. We conclude that, despite discrepancies with observations, the scenario offers one of the best available explanations for CK Vul and, with minor modifications, explains the observed properties of [WN/WC]-central stars of planetary nebulae.Facultad de Ciencias Astronómicas y Geofísicas2011-07-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1396-1408http://sedici.unlp.edu.ar/handle/10915/83994enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18790.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:06Zoai:sedici.unlp.edu.ar:10915/83994Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:06.495SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
title |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
spellingShingle |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts Miller Bertolami, Marcelo Miguel Ciencias Astronómicas Stars: AGB and post-AGB Stars: individual: CK Vul Stars: individual: PB8 Stars: Wolf-Rayet White dwarfs |
title_short |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
title_full |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
title_fullStr |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
title_full_unstemmed |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
title_sort |
The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts |
dc.creator.none.fl_str_mv |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Olano, Carlos Alberto Jiménez, Noelia |
author |
Miller Bertolami, Marcelo Miguel |
author_facet |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Olano, Carlos Alberto Jiménez, Noelia |
author_role |
author |
author2 |
Althaus, Leandro Gabriel Olano, Carlos Alberto Jiménez, Noelia |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Stars: AGB and post-AGB Stars: individual: CK Vul Stars: individual: PB8 Stars: Wolf-Rayet White dwarfs |
topic |
Ciencias Astronómicas Stars: AGB and post-AGB Stars: individual: CK Vul Stars: individual: PB8 Stars: Wolf-Rayet White dwarfs |
dc.description.none.fl_txt_mv |
We propose a scenario for the formation of DA white dwarfs with very thin helium buffers. For these stars we explore the possible occurrence of diffusion-induced CNO-flashes during their early cooling stage. In order to obtain very thin helium buffers, we simulate the formation of low-mass remnants through an asymptotic giant branch (AGB) final/late thermal pulse (AFTP/LTP scenario). Then we calculate the consequent white dwarf cooling evolution by means of a consistent treatment of element diffusion and nuclear burning. Based on physically sound white dwarf models, we find that the range of helium buffer masses for these diffusion-induced novae to occur is significantly smaller than that predicted by the only previous study of this scenario. As a matter of fact, we find that these flashes do occur only in some low-mass (M ≲ 0.6M⊙) and low-metallicity (ZZAMS ≲ 0.001) remnants about 106-107yr after departing from the AGB. For these objects, we expect the luminosity to increase by about 4 orders of magnitude in less than a decade. We also show that diffusion-induced novae should display a very typical eruption light curve, with an increase of about a few magnitudes per year before reaching a maximum ofMV~-5 to -6. Our simulations show that surface abundances after the outburst are characterized by logNH/NHe~-0.15...0.6 and N > C ≳ O by mass fractions. Contrary to previous speculations we show that these events are not recurrent and do not change substantially the final H-content of the cool (DA) white dwarf. Finally, with the aid of model predictions we discuss the possibility that Nova Vul 1670 (CK Vul) and the recently proposed [WN/WC]-central stars of planetary nebulae could be observational counterparts of this diffusion-induced nova scenario. We conclude that, despite discrepancies with observations, the scenario offers one of the best available explanations for CK Vul and, with minor modifications, explains the observed properties of [WN/WC]-central stars of planetary nebulae. Facultad de Ciencias Astronómicas y Geofísicas |
description |
We propose a scenario for the formation of DA white dwarfs with very thin helium buffers. For these stars we explore the possible occurrence of diffusion-induced CNO-flashes during their early cooling stage. In order to obtain very thin helium buffers, we simulate the formation of low-mass remnants through an asymptotic giant branch (AGB) final/late thermal pulse (AFTP/LTP scenario). Then we calculate the consequent white dwarf cooling evolution by means of a consistent treatment of element diffusion and nuclear burning. Based on physically sound white dwarf models, we find that the range of helium buffer masses for these diffusion-induced novae to occur is significantly smaller than that predicted by the only previous study of this scenario. As a matter of fact, we find that these flashes do occur only in some low-mass (M ≲ 0.6M⊙) and low-metallicity (ZZAMS ≲ 0.001) remnants about 106-107yr after departing from the AGB. For these objects, we expect the luminosity to increase by about 4 orders of magnitude in less than a decade. We also show that diffusion-induced novae should display a very typical eruption light curve, with an increase of about a few magnitudes per year before reaching a maximum ofMV~-5 to -6. Our simulations show that surface abundances after the outburst are characterized by logNH/NHe~-0.15...0.6 and N > C ≳ O by mass fractions. Contrary to previous speculations we show that these events are not recurrent and do not change substantially the final H-content of the cool (DA) white dwarf. Finally, with the aid of model predictions we discuss the possibility that Nova Vul 1670 (CK Vul) and the recently proposed [WN/WC]-central stars of planetary nebulae could be observational counterparts of this diffusion-induced nova scenario. We conclude that, despite discrepancies with observations, the scenario offers one of the best available explanations for CK Vul and, with minor modifications, explains the observed properties of [WN/WC]-central stars of planetary nebulae. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-07-04 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://sedici.unlp.edu.ar/handle/10915/83994 |
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http://sedici.unlp.edu.ar/handle/10915/83994 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18790.x |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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openAccess |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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application/pdf 1396-1408 |
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