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, N.
- 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 ≲ 0.6 M⊙) and low-metallicity (ZZAMS≲ 0.001) remnants about 106–107 yr 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 of MV ∼−5 to −6. Our simulations show that surface abundances after the outburst are characterized by log NH/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.
Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Olano, Carlos Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Jiménez, N.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina - Materia
-
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
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/95076
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oai:ri.conicet.gov.ar:11336/95076 |
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3498 |
network_name_str |
CONICET Digital (CONICET) |
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The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterpartsMiller Bertolami, Marcelo MiguelAlthaus, Leandro GabrielOlano, Carlos AlbertoJiménez, N.STARS: AGB AND POST-AGBSTARS: INDIVIDUAL: CK VULSTARS: INDIVIDUAL: PB8STARS: WOLF-RAYETWHITE DWARFShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We 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 ≲ 0.6 M⊙) and low-metallicity (ZZAMS≲ 0.001) remnants about 106–107 yr 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 of MV ∼−5 to −6. Our simulations show that surface abundances after the outburst are characterized by log NH/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.Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Olano, Carlos Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Jiménez, N.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaWiley Blackwell Publishing, Inc2011-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/95076Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Olano, Carlos Alberto; Jiménez, N.; The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts ; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 415; 2; 8-2011; 1396-14080035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18790.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/415/2/1396/1039915info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:38:57Zoai:ri.conicet.gov.ar:11336/95076instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:38:57.404CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
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 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, N. |
author |
Miller Bertolami, Marcelo Miguel |
author_facet |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Olano, Carlos Alberto Jiménez, N. |
author_role |
author |
author2 |
Althaus, Leandro Gabriel Olano, Carlos Alberto Jiménez, N. |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
STARS: AGB AND POST-AGB STARS: INDIVIDUAL: CK VUL STARS: INDIVIDUAL: PB8 STARS: WOLF-RAYET WHITE DWARFS |
topic |
STARS: AGB AND POST-AGB STARS: INDIVIDUAL: CK VUL STARS: INDIVIDUAL: PB8 STARS: WOLF-RAYET WHITE DWARFS |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
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 ≲ 0.6 M⊙) and low-metallicity (ZZAMS≲ 0.001) remnants about 106–107 yr 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 of MV ∼−5 to −6. Our simulations show that surface abundances after the outburst are characterized by log NH/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. Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Olano, Carlos Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Jiménez, N.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina |
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 ≲ 0.6 M⊙) and low-metallicity (ZZAMS≲ 0.001) remnants about 106–107 yr 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 of MV ∼−5 to −6. Our simulations show that surface abundances after the outburst are characterized by log NH/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 |
2011-08 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion 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://hdl.handle.net/11336/95076 Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Olano, Carlos Alberto; Jiménez, N.; The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts ; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 415; 2; 8-2011; 1396-1408 0035-8711 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/95076 |
identifier_str_mv |
Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Olano, Carlos Alberto; Jiménez, N.; The diffusion-induced nova scenario: CK Vul and PB8 as possible observational counterparts ; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 415; 2; 8-2011; 1396-1408 0035-8711 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18790.x info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/415/2/1396/1039915 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1844614413404864512 |
score |
13.070432 |