The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)

Autores: Skopal, A.; Shugarov, S. Y.; Munari, U.; Masetti, N.; Marchesini, Ezequiel Joaquín; Komzík, R. M.; Kundra, E.; Shagatova, N.; Tarasova, T. N.; Buil, C.; Boussin, C.; Shenavrin, V. I.; Hambsch, F. J.; Dallaporta, S.; Frigolé, Cecilia Andrea; Gardey, Juan Cruz; Zubareva, A.; Dubovský, P. A.; Kroll, P.
Año de publicación: 2020
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: Context. The star V426 Sge (HBHA 1704-05), originally classified as an emission-line object and a semi-regular variable, brightened at the beginning of August 2018, showing signatures of a symbiotic star outburst. Aims. We aim to confirm the nature of V426 Sge as a classical symbiotic star, determine the photometric ephemeris of the light minima, and suggest the path from its 1968 symbiotic nova outburst to the following 2018 Z And-type outburst. Methods. We re-constructed an historical light curve (LC) of V426 Sge from approximately the year 1900, and used original low- (R ∼ 500-1500; 330-880 nm) and high-resolution (R ∼ 11 000-34 000; 360-760 nm) spectroscopy complemented with Swift-XRT and UVOT, optical UBVRCIC and near-infrared JHKL photometry obtained during the 2018 outburst and the following quiescence. Results. The historical LC reveals no symbiotic-like activity from ∼1900 to 1967. In 1968, V426 Sge experienced a symbiotic nova outburst that ceased around 1990. From approximately 1972, a wave-like orbitally related variation with a period of 493.4 ± 0.7 days developed in the LC. This was interrupted by a Z And-type outburst from the beginning of August 2018 to the middle of February 2019. At the maximum of the 2018 outburst, the burning white dwarf (WD) increased its temperature to ? 2 × 105 K, generated a luminosity of ∼7 × 1037 (d/3.3 kpc)2 erg s-1 and blew a wind at the rate of ∼3 × 10-6 M yr-1. Our spectral energy distribution models from the current quiescent phase reveal that the donor is a normal M4-5 III giant characterised with Teff ∼ 3400 K, RG ∼ 106 (d/3.3 kpc) R and LG ∼ 1350 (d/3.3 kpc)2 L and the accretor is a low-mass ∼0.5 M WD. Conclusions. During the transition from the symbiotic nova outburst to the quiescent phase, a pronounced sinusoidal variation along the orbit develops in the LC of most symbiotic novae. The following eventual outburst is of Z And-type, when the accretion by the WD temporarily exceeds the upper limit of the stable burning. At this point the system becomes a classical symbiotic star.
Fil: Skopal, A.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
Fil: Shugarov, S. Y.. Lomonosov Moscow State University; Rusia. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
Fil: Munari, U.. Osservatorio Astronomico Di Padova; Italia
Fil: Masetti, N.. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica, Bologna; Italia. Universidad Andrés Bello; Chile
Fil: Marchesini, Ezequiel Joaquín. Università di Torino; Italia. 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: Komzík, R. M.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
Fil: Kundra, E.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
Fil: Shagatova, N.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
Fil: Tarasova, T. N.. Crimean Astrophysical Observatory Ras; Rusia
Fil: Buil, C.. Castanet Tolosan Observatory; Francia
Fil: Boussin, C.. Observatoire de L'eridan Et de la Chevelure de Bérénice; Francia
Fil: Shenavrin, V. I.. Lomonosov Moscow State University; Rusia
Fil: Hambsch, F. J.. Istituto Nazionale di Astrofisica; Italia
Fil: Dallaporta, S.. Istituto Nazionale di Astrofisica; Italia
Fil: Frigolé, Cecilia Andrea. Istituto Nazionale di Astrofisica; Italia
Fil: Gardey, Juan Cruz. Observatoire de la Tourbière; Francia
Fil: Zubareva, A.. Institute Of Astronomy Of The Russian Academy Of Sciences; Rusia. Lomonosov Moscow State University; Rusia
Fil: Dubovský, P. A.. Vihorlat Observatory; Eslovaquia
Fil: Kroll, P.. Sonneberg Observatory; Alemania
Materia: BINARIES: SYMBIOTIC
CATACLYSMIC VARIABLES
NOVAE
STARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)
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:11336/145944

Acceder

id	CONICETDig_13147979d589c8a919bc269b4b5c3896
oai_identifier_str	oai:ri.conicet.gov.ar:11336/145944
network_acronym_str	CONICETDig
repository_id_str	3498
network_name_str	CONICET Digital (CONICET)
spelling	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)Skopal, A.Shugarov, S. Y.Munari, U.Masetti, N.Marchesini, Ezequiel JoaquínKomzík, R. M.Kundra, E.Shagatova, N.Tarasova, T. N.Buil, C.Boussin, C.Shenavrin, V. I.Hambsch, F. J.Dallaporta, S.Frigolé, Cecilia AndreaGardey, Juan CruzZubareva, A.Dubovský, P. A.Kroll, P.BINARIES: SYMBIOTICCATACLYSMIC VARIABLESNOVAESTARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The star V426 Sge (HBHA 1704-05), originally classified as an emission-line object and a semi-regular variable, brightened at the beginning of August 2018, showing signatures of a symbiotic star outburst. Aims. We aim to confirm the nature of V426 Sge as a classical symbiotic star, determine the photometric ephemeris of the light minima, and suggest the path from its 1968 symbiotic nova outburst to the following 2018 Z And-type outburst. Methods. We re-constructed an historical light curve (LC) of V426 Sge from approximately the year 1900, and used original low- (R ∼ 500-1500; 330-880 nm) and high-resolution (R ∼ 11 000-34 000; 360-760 nm) spectroscopy complemented with Swift-XRT and UVOT, optical UBVRCIC and near-infrared JHKL photometry obtained during the 2018 outburst and the following quiescence. Results. The historical LC reveals no symbiotic-like activity from ∼1900 to 1967. In 1968, V426 Sge experienced a symbiotic nova outburst that ceased around 1990. From approximately 1972, a wave-like orbitally related variation with a period of 493.4 ± 0.7 days developed in the LC. This was interrupted by a Z And-type outburst from the beginning of August 2018 to the middle of February 2019. At the maximum of the 2018 outburst, the burning white dwarf (WD) increased its temperature to ? 2 × 105 K, generated a luminosity of ∼7 × 1037 (d/3.3 kpc)2 erg s-1 and blew a wind at the rate of ∼3 × 10-6 M yr-1. Our spectral energy distribution models from the current quiescent phase reveal that the donor is a normal M4-5 III giant characterised with Teff ∼ 3400 K, RG ∼ 106 (d/3.3 kpc) R and LG ∼ 1350 (d/3.3 kpc)2 L and the accretor is a low-mass ∼0.5 M WD. Conclusions. During the transition from the symbiotic nova outburst to the quiescent phase, a pronounced sinusoidal variation along the orbit develops in the LC of most symbiotic novae. The following eventual outburst is of Z And-type, when the accretion by the WD temporarily exceeds the upper limit of the stable burning. At this point the system becomes a classical symbiotic star.Fil: Skopal, A.. Astronomical Institute Slovak Academy Of Sciences; EslovaquiaFil: Shugarov, S. Y.. Lomonosov Moscow State University; Rusia. Astronomical Institute Slovak Academy Of Sciences; EslovaquiaFil: Munari, U.. Osservatorio Astronomico Di Padova; ItaliaFil: Masetti, N.. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica, Bologna; Italia. Universidad Andrés Bello; ChileFil: Marchesini, Ezequiel Joaquín. Università di Torino; Italia. 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: Komzík, R. M.. Astronomical Institute Slovak Academy Of Sciences; EslovaquiaFil: Kundra, E.. Astronomical Institute Slovak Academy Of Sciences; EslovaquiaFil: Shagatova, N.. Astronomical Institute Slovak Academy Of Sciences; EslovaquiaFil: Tarasova, T. N.. Crimean Astrophysical Observatory Ras; RusiaFil: Buil, C.. Castanet Tolosan Observatory; FranciaFil: Boussin, C.. Observatoire de L'eridan Et de la Chevelure de Bérénice; FranciaFil: Shenavrin, V. I.. Lomonosov Moscow State University; RusiaFil: Hambsch, F. J.. Istituto Nazionale di Astrofisica; ItaliaFil: Dallaporta, S.. Istituto Nazionale di Astrofisica; ItaliaFil: Frigolé, Cecilia Andrea. Istituto Nazionale di Astrofisica; ItaliaFil: Gardey, Juan Cruz. Observatoire de la Tourbière; FranciaFil: Zubareva, A.. Institute Of Astronomy Of The Russian Academy Of Sciences; Rusia. Lomonosov Moscow State University; RusiaFil: Dubovský, P. A.. Vihorlat Observatory; EslovaquiaFil: Kroll, P.. Sonneberg Observatory; AlemaniaEDP Sciences2020-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/145944Skopal, A.; Shugarov, S. Y.; Munari, U.; Masetti, N.; Marchesini, Ezequiel Joaquín; et al.; The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05); EDP Sciences; Astronomy and Astrophysics; 636; A77; 4-2020; 1-180004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201937199info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2020/04/aa37199-19/aa37199-19.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:32:40Zoai:ri.conicet.gov.ar:11336/145944instacron: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 09:32:40.833CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
title	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
spellingShingle	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05) Skopal, A. BINARIES: SYMBIOTIC CATACLYSMIC VARIABLES NOVAE STARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)
title_short	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
title_full	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
title_fullStr	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
title_full_unstemmed	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
title_sort	The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
dc.creator.none.fl_str_mv	Skopal, A. Shugarov, S. Y. Munari, U. Masetti, N. Marchesini, Ezequiel Joaquín Komzík, R. M. Kundra, E. Shagatova, N. Tarasova, T. N. Buil, C. Boussin, C. Shenavrin, V. I. Hambsch, F. J. Dallaporta, S. Frigolé, Cecilia Andrea Gardey, Juan Cruz Zubareva, A. Dubovský, P. A. Kroll, P.
author	Skopal, A.
author_facet	Skopal, A. Shugarov, S. Y. Munari, U. Masetti, N. Marchesini, Ezequiel Joaquín Komzík, R. M. Kundra, E. Shagatova, N. Tarasova, T. N. Buil, C. Boussin, C. Shenavrin, V. I. Hambsch, F. J. Dallaporta, S. Frigolé, Cecilia Andrea Gardey, Juan Cruz Zubareva, A. Dubovský, P. A. Kroll, P.
author_role	author
author2	Shugarov, S. Y. Munari, U. Masetti, N. Marchesini, Ezequiel Joaquín Komzík, R. M. Kundra, E. Shagatova, N. Tarasova, T. N. Buil, C. Boussin, C. Shenavrin, V. I. Hambsch, F. J. Dallaporta, S. Frigolé, Cecilia Andrea Gardey, Juan Cruz Zubareva, A. Dubovský, P. A. Kroll, P.
author2_role	author author author author author author author author author author author author author author author author author author
dc.subject.none.fl_str_mv	BINARIES: SYMBIOTIC CATACLYSMIC VARIABLES NOVAE STARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)
topic	BINARIES: SYMBIOTIC CATACLYSMIC VARIABLES NOVAE STARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)
purl_subject.fl_str_mv	https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv	Context. The star V426 Sge (HBHA 1704-05), originally classified as an emission-line object and a semi-regular variable, brightened at the beginning of August 2018, showing signatures of a symbiotic star outburst. Aims. We aim to confirm the nature of V426 Sge as a classical symbiotic star, determine the photometric ephemeris of the light minima, and suggest the path from its 1968 symbiotic nova outburst to the following 2018 Z And-type outburst. Methods. We re-constructed an historical light curve (LC) of V426 Sge from approximately the year 1900, and used original low- (R ∼ 500-1500; 330-880 nm) and high-resolution (R ∼ 11 000-34 000; 360-760 nm) spectroscopy complemented with Swift-XRT and UVOT, optical UBVRCIC and near-infrared JHKL photometry obtained during the 2018 outburst and the following quiescence. Results. The historical LC reveals no symbiotic-like activity from ∼1900 to 1967. In 1968, V426 Sge experienced a symbiotic nova outburst that ceased around 1990. From approximately 1972, a wave-like orbitally related variation with a period of 493.4 ± 0.7 days developed in the LC. This was interrupted by a Z And-type outburst from the beginning of August 2018 to the middle of February 2019. At the maximum of the 2018 outburst, the burning white dwarf (WD) increased its temperature to ? 2 × 105 K, generated a luminosity of ∼7 × 1037 (d/3.3 kpc)2 erg s-1 and blew a wind at the rate of ∼3 × 10-6 M yr-1. Our spectral energy distribution models from the current quiescent phase reveal that the donor is a normal M4-5 III giant characterised with Teff ∼ 3400 K, RG ∼ 106 (d/3.3 kpc) R and LG ∼ 1350 (d/3.3 kpc)2 L and the accretor is a low-mass ∼0.5 M WD. Conclusions. During the transition from the symbiotic nova outburst to the quiescent phase, a pronounced sinusoidal variation along the orbit develops in the LC of most symbiotic novae. The following eventual outburst is of Z And-type, when the accretion by the WD temporarily exceeds the upper limit of the stable burning. At this point the system becomes a classical symbiotic star. Fil: Skopal, A.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia Fil: Shugarov, S. Y.. Lomonosov Moscow State University; Rusia. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia Fil: Munari, U.. Osservatorio Astronomico Di Padova; Italia Fil: Masetti, N.. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica, Bologna; Italia. Universidad Andrés Bello; Chile Fil: Marchesini, Ezequiel Joaquín. Università di Torino; Italia. 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: Komzík, R. M.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia Fil: Kundra, E.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia Fil: Shagatova, N.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia Fil: Tarasova, T. N.. Crimean Astrophysical Observatory Ras; Rusia Fil: Buil, C.. Castanet Tolosan Observatory; Francia Fil: Boussin, C.. Observatoire de L'eridan Et de la Chevelure de Bérénice; Francia Fil: Shenavrin, V. I.. Lomonosov Moscow State University; Rusia Fil: Hambsch, F. J.. Istituto Nazionale di Astrofisica; Italia Fil: Dallaporta, S.. Istituto Nazionale di Astrofisica; Italia Fil: Frigolé, Cecilia Andrea. Istituto Nazionale di Astrofisica; Italia Fil: Gardey, Juan Cruz. Observatoire de la Tourbière; Francia Fil: Zubareva, A.. Institute Of Astronomy Of The Russian Academy Of Sciences; Rusia. Lomonosov Moscow State University; Rusia Fil: Dubovský, P. A.. Vihorlat Observatory; Eslovaquia Fil: Kroll, P.. Sonneberg Observatory; Alemania
description	Context. The star V426 Sge (HBHA 1704-05), originally classified as an emission-line object and a semi-regular variable, brightened at the beginning of August 2018, showing signatures of a symbiotic star outburst. Aims. We aim to confirm the nature of V426 Sge as a classical symbiotic star, determine the photometric ephemeris of the light minima, and suggest the path from its 1968 symbiotic nova outburst to the following 2018 Z And-type outburst. Methods. We re-constructed an historical light curve (LC) of V426 Sge from approximately the year 1900, and used original low- (R ∼ 500-1500; 330-880 nm) and high-resolution (R ∼ 11 000-34 000; 360-760 nm) spectroscopy complemented with Swift-XRT and UVOT, optical UBVRCIC and near-infrared JHKL photometry obtained during the 2018 outburst and the following quiescence. Results. The historical LC reveals no symbiotic-like activity from ∼1900 to 1967. In 1968, V426 Sge experienced a symbiotic nova outburst that ceased around 1990. From approximately 1972, a wave-like orbitally related variation with a period of 493.4 ± 0.7 days developed in the LC. This was interrupted by a Z And-type outburst from the beginning of August 2018 to the middle of February 2019. At the maximum of the 2018 outburst, the burning white dwarf (WD) increased its temperature to ? 2 × 105 K, generated a luminosity of ∼7 × 1037 (d/3.3 kpc)2 erg s-1 and blew a wind at the rate of ∼3 × 10-6 M yr-1. Our spectral energy distribution models from the current quiescent phase reveal that the donor is a normal M4-5 III giant characterised with Teff ∼ 3400 K, RG ∼ 106 (d/3.3 kpc) R and LG ∼ 1350 (d/3.3 kpc)2 L and the accretor is a low-mass ∼0.5 M WD. Conclusions. During the transition from the symbiotic nova outburst to the quiescent phase, a pronounced sinusoidal variation along the orbit develops in the LC of most symbiotic novae. The following eventual outburst is of Z And-type, when the accretion by the WD temporarily exceeds the upper limit of the stable burning. At this point the system becomes a classical symbiotic star.
publishDate	2020
dc.date.none.fl_str_mv	2020-04
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/11336/145944 Skopal, A.; Shugarov, S. Y.; Munari, U.; Masetti, N.; Marchesini, Ezequiel Joaquín; et al.; The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05); EDP Sciences; Astronomy and Astrophysics; 636; A77; 4-2020; 1-18 0004-6361 CONICET Digital CONICET
url	http://hdl.handle.net/11336/145944
identifier_str_mv	Skopal, A.; Shugarov, S. Y.; Munari, U.; Masetti, N.; Marchesini, Ezequiel Joaquín; et al.; The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05); EDP Sciences; Astronomy and Astrophysics; 636; A77; 4-2020; 1-18 0004-6361 CONICET Digital CONICET
dc.language.none.fl_str_mv	eng
language	eng
dc.relation.none.fl_str_mv	info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201937199 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2020/04/aa37199-19/aa37199-19.html
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
dc.publisher.none.fl_str_mv	EDP Sciences
publisher.none.fl_str_mv	EDP Sciences
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
_version_	1844612998368329728
score	13.070432

The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)

Publicaciones similares