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

A. Skopal, S. Y. Shugarov, U. Munari, N. Masetti, E. Marchesini, R. M. Komzík, E. Kundra, N. Shagatova, T. N. Tarasova, C. Buil, C. Boussin, V. I. Shenavrin, F. J. Hambsch, S. Dallaporta, A. Frigo, O. Garde, A. Zubareva, P. A. Dubovský, P. Kroll

Research output: Contribution to journalArticlepeer-review

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.

Original languageEnglish
Article number201937199
JournalAstronomy and Astrophysics
Volume636
DOIs
Publication statusPublished - 1 Apr 2020

Keywords

  • Binaries: symbiotic
  • Cataclysmic variables
  • Novae
  • Stars: individual: V426 Sagittae (HBHA 1704-05)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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