The orbital period of the recurrent nova V2487 Oph revealed
We present the first reliable determination of the orbital period of the recurrent nova V2487 Oph (Nova Oph 1998). We derived a value of 0.753 ± 0.016 d (18.1 ± 0.4 h) from the radial velocity curve of the intense He¿II ¿4686 emission line as detected in time-series X-shooter spectra. The orbital pe...
| Autores: | , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/397433 |
| Acceso en línea: | https://hdl.handle.net/2117/397433 https://dx.doi.org/10.1093/mnras/stad3124 |
| Access Level: | acceso abierto |
| Palabra clave: | Stars Accretion Accretion discs Binaries: close Stars: individual: V2487 Oph (Nova Ophiuchi 1998) Novae Cataclysmic variables Estels Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
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The orbital period of the recurrent nova V2487 Oph revealedRodríguez Gil, PabloCorral Santana, Jesus M.Elias Rosa, NancyGänsicke, Boris T.Hernanz, MargaritaSala Cladellas, Glòria|||0000-0001-6211-8299StarsAccretionAccretion discsBinaries: closeStars: individual: V2487 Oph (Nova Ophiuchi 1998)NovaeCataclysmic variablesEstelsÀrees temàtiques de la UPC::Física::Astronomia i astrofísicaWe present the first reliable determination of the orbital period of the recurrent nova V2487 Oph (Nova Oph 1998). We derived a value of 0.753 ± 0.016 d (18.1 ± 0.4 h) from the radial velocity curve of the intense He¿II ¿4686 emission line as detected in time-series X-shooter spectra. The orbital period is significantly shorter than earlier claims, but it makes V2487 Oph one of the longest period cataclysmic variables known. The spectrum of V2487 Oph is prolific in broad Balmer absorptions that resemble a white dwarf spectrum. However, we show that they come from the accretion disc viewed at low inclination. Although highly speculative, the analysis of the radial velocity curves provides a binary mass ratio q ˜ 0.16 and a donor star mass M2 ˜ 0.21 M¿, assuming the reported white dwarf mass M1 = 1.35 M¿. A subgiant M-type star is tentatively suggested as the donor star. We were lucky to inadvertently take some of the spectra when V2487 Oph was in a flare state. During the flare, we detected high-velocity emission in the Balmer and He¿II ¿4686 lines exceeding -2000 km s-1 at close to orbital phase 0.4. Receding emission up to 1200 km s-1 at about phase 0.3 is also observed. The similarities with the magnetic cataclysmic variables may point to magnetic accretion on to the white dwarf during the repeating flares.Peer ReviewedOxford University Press20232023-10-1220232023-11-30journal articlehttp://purl.org/coar/resource_type/c_6501VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/2117/397433https://dx.doi.org/10.1093/mnras/stad3124reponame:UPCommons. Portal del coneixement obert de la UPCinstname:Universitat Politècnica de Catalunya (UPC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution-NonCommercial-NoDerivatives 4.0 Internationalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:upcommons.upc.edu:2117/3974332026-05-27T15:37:01Z |
| dc.title.none.fl_str_mv |
The orbital period of the recurrent nova V2487 Oph revealed |
| title |
The orbital period of the recurrent nova V2487 Oph revealed |
| spellingShingle |
The orbital period of the recurrent nova V2487 Oph revealed Rodríguez Gil, Pablo Stars Accretion Accretion discs Binaries: close Stars: individual: V2487 Oph (Nova Ophiuchi 1998) Novae Cataclysmic variables Estels Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| title_short |
The orbital period of the recurrent nova V2487 Oph revealed |
| title_full |
The orbital period of the recurrent nova V2487 Oph revealed |
| title_fullStr |
The orbital period of the recurrent nova V2487 Oph revealed |
| title_full_unstemmed |
The orbital period of the recurrent nova V2487 Oph revealed |
| title_sort |
The orbital period of the recurrent nova V2487 Oph revealed |
| dc.creator.none.fl_str_mv |
Rodríguez Gil, Pablo Corral Santana, Jesus M. Elias Rosa, Nancy Gänsicke, Boris T. Hernanz, Margarita Sala Cladellas, Glòria|||0000-0001-6211-8299 |
| author |
Rodríguez Gil, Pablo |
| author_facet |
Rodríguez Gil, Pablo Corral Santana, Jesus M. Elias Rosa, Nancy Gänsicke, Boris T. Hernanz, Margarita Sala Cladellas, Glòria|||0000-0001-6211-8299 |
| author_role |
author |
| author2 |
Corral Santana, Jesus M. Elias Rosa, Nancy Gänsicke, Boris T. Hernanz, Margarita Sala Cladellas, Glòria|||0000-0001-6211-8299 |
| author2_role |
author author author author author |
| dc.subject.none.fl_str_mv |
Stars Accretion Accretion discs Binaries: close Stars: individual: V2487 Oph (Nova Ophiuchi 1998) Novae Cataclysmic variables Estels Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| topic |
Stars Accretion Accretion discs Binaries: close Stars: individual: V2487 Oph (Nova Ophiuchi 1998) Novae Cataclysmic variables Estels Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| description |
We present the first reliable determination of the orbital period of the recurrent nova V2487 Oph (Nova Oph 1998). We derived a value of 0.753 ± 0.016 d (18.1 ± 0.4 h) from the radial velocity curve of the intense He¿II ¿4686 emission line as detected in time-series X-shooter spectra. The orbital period is significantly shorter than earlier claims, but it makes V2487 Oph one of the longest period cataclysmic variables known. The spectrum of V2487 Oph is prolific in broad Balmer absorptions that resemble a white dwarf spectrum. However, we show that they come from the accretion disc viewed at low inclination. Although highly speculative, the analysis of the radial velocity curves provides a binary mass ratio q ˜ 0.16 and a donor star mass M2 ˜ 0.21 M¿, assuming the reported white dwarf mass M1 = 1.35 M¿. A subgiant M-type star is tentatively suggested as the donor star. We were lucky to inadvertently take some of the spectra when V2487 Oph was in a flare state. During the flare, we detected high-velocity emission in the Balmer and He¿II ¿4686 lines exceeding -2000 km s-1 at close to orbital phase 0.4. Receding emission up to 1200 km s-1 at about phase 0.3 is also observed. The similarities with the magnetic cataclysmic variables may point to magnetic accretion on to the white dwarf during the repeating flares. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023 2023-10-12 2023 2023-11-30 |
| dc.type.none.fl_str_mv |
journal article http://purl.org/coar/resource_type/c_6501 VoR http://purl.org/coar/version/c_970fb48d4fbd8a85 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
| format |
article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/2117/397433 https://dx.doi.org/10.1093/mnras/stad3124 |
| url |
https://hdl.handle.net/2117/397433 https://dx.doi.org/10.1093/mnras/stad3124 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 Attribution-NonCommercial-NoDerivatives 4.0 International http://creativecommons.org/licenses/by-nc-nd/4.0/ |
| dc.rights.openaire.fl_str_mv |
info:eu-repo/semantics/openAccess |
| rights_invalid_str_mv |
open access http://purl.org/coar/access_right/c_abf2 Attribution-NonCommercial-NoDerivatives 4.0 International http://creativecommons.org/licenses/by-nc-nd/4.0/ |
| eu_rights_str_mv |
openAccess |
| dc.format.none.fl_str_mv |
application/pdf |
| dc.publisher.none.fl_str_mv |
Oxford University Press |
| publisher.none.fl_str_mv |
Oxford University Press |
| dc.source.none.fl_str_mv |
reponame:UPCommons. Portal del coneixement obert de la UPC instname:Universitat Politècnica de Catalunya (UPC) |
| instname_str |
Universitat Politècnica de Catalunya (UPC) |
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UPCommons. Portal del coneixement obert de la UPC |
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UPCommons. Portal del coneixement obert de la UPC |
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1869405198189854720 |
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