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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/83994

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/83994
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 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
url 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)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
1396-1408
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
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instname_str Universidad Nacional de La Plata
instacron_str UNLP
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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