Journal
ASTRONOMY & ASTROPHYSICS
Volume 563, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201322421
Keywords
techniques: high angular resolution; stars: individual: HR 5171 A; binaries: close; circumstellar matter; stars: massive; stars: mass-loss
Categories
Funding
- National Research Foundation of South Africa
- GEMINI-CONICYT [32090006]
- CONICYT-FONDECYT [N 3120037]
- CONICYT Capital Humano Avanzado project [N 7912010046]
- centro de astrofisica de Valparaiso
- Fondecyt [N1130849]
- FNRS
- Prodex Integral/XMM
- Science and Technology Facilities Council [ST/J003018/1, ST/I001557/1] Funding Source: researchfish
- STFC [ST/J003018/1, ST/I001557/1] Funding Source: UKRI
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Context. Only a few stars are caught in the very brief and often crucial stages when they quickly traverse the Hertzsprung-Russell diagram, and none has yet been spatially resolved in the mass transfer phase. Aims. We initiated long-term optical interferometry monitoring of the diameters of massive and unstable yellow hypergiants (YHG) with the goal of detecting both the long-term evolution of their radius and shorter term formation of a possible pseudo-photosphere related to proposed large mass-loss events. Methods. We observed HR 5171 A with AMBER/VLTI. We also examined archival photometric data in the visual and near-IR spanning more than 60 years, as well as sparse spectroscopic data. Results. HR 5171 A exhibits a complex appearance. Our AMBER data reveal a surprisingly large star for a YHG R-* = 1315 +/- 260 R-circle dot (or similar to 6.1 AU) at the distance of 3.6 +/- 0.5 kpc. The source is surrounded by an extended nebulosity, and these data also show a large level of asymmetry in the brightness distribution of the system, which we attribute to a newly discovered companion star located in front of the primary star. The companion's signature is also detected in the visual photometry, which indicates an orbital period of P-orb = 1304 +/- 6 d. Modeling the light curve with the NIGHTFALL program provides clear evidence that the system is a contact or possibly over-contact eclipsing binary. A total current system mass of 39(-22)(+40) M-circle dot and a high mass ratio q >= 10 is inferred for the system. Conclusions. The low-mass companion of HR 5171 A is very close to the primary star that is embedded within its dense wind. Tight constraints on the inclination and v sin i of the primary are lacking, which prevents us from determining its influence precisely on the mass-loss phenomenon, but the system is probably experiencing a wind Roche-Lobe overflow. Depending on the amount of angular momentum that can be transferred to the stellar envelope, HR 5171 A may become a fast-rotating B[e]/luminous blue variable/Wolf-Rayet star. In any case, HR 5171 A highlights the possible importance of binaries for interpreting the unstable YHGs and for massive star evolution in general.
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