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dc.contributor.author
Skopal, A.
dc.contributor.author
Shugarov, S. Y.
dc.contributor.author
Munari, U.
dc.contributor.author
Masetti, N.
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Marchesini, Ezequiel Joaquín
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Komzík, R. M.
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Kundra, E.
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Shagatova, N.
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Tarasova, T. N.
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Buil, C.
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Boussin, C.
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Shenavrin, V. I.
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Hambsch, F. J.
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Dallaporta, S.
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Frigolé, Cecilia Andrea
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Gardey, Juan Cruz
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Zubareva, A.
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Dubovský, P. A.
dc.contributor.author
Kroll, P.
dc.date.available
2021-11-04T11:56:15Z
dc.date.issued
2020-04
dc.identifier.citation
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
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/145944
dc.description.abstract
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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
BINARIES: SYMBIOTIC
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CATACLYSMIC VARIABLES
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NOVAE
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STARS: INDIVIDUAL: V426 SAGITTAE (HBHA 1704-05)
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2021-09-06T17:46:16Z
dc.journal.volume
636
dc.journal.number
A77
dc.journal.pagination
1-18
dc.journal.pais
Francia
dc.description.fil
Fil: Skopal, A.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
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Fil: Shugarov, S. Y.. Lomonosov Moscow State University; Rusia. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
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Fil: Munari, U.. Osservatorio Astronomico Di Padova; Italia
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Fil: Masetti, N.. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica, Bologna; Italia. Universidad Andrés Bello; Chile
dc.description.fil
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
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Fil: Komzík, R. M.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
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Fil: Kundra, E.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
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Fil: Shagatova, N.. Astronomical Institute Slovak Academy Of Sciences; Eslovaquia
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Fil: Tarasova, T. N.. Crimean Astrophysical Observatory Ras; Rusia
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Fil: Buil, C.. Castanet Tolosan Observatory; Francia
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Fil: Boussin, C.. Observatoire de L'eridan Et de la Chevelure de Bérénice; Francia
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Fil: Shenavrin, V. I.. Lomonosov Moscow State University; Rusia
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Fil: Hambsch, F. J.. Istituto Nazionale di Astrofisica; Italia
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Fil: Dallaporta, S.. Istituto Nazionale di Astrofisica; Italia
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Fil: Frigolé, Cecilia Andrea. Istituto Nazionale di Astrofisica; Italia
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Fil: Gardey, Juan Cruz. Observatoire de la Tourbière; Francia
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Fil: Zubareva, A.. Institute Of Astronomy Of The Russian Academy Of Sciences; Rusia. Lomonosov Moscow State University; Rusia
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Fil: Dubovský, P. A.. Vihorlat Observatory; Eslovaquia
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Fil: Kroll, P.. Sonneberg Observatory; Alemania
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201937199
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info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2020/04/aa37199-19/aa37199-19.html
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