In 1981, the idea of a superwind that ends the life of cool giant stars was proposed1. Extreme oxygen-rich giants, OH/IR stars, develop superwinds with the highest mass-loss rates known so far, up to a few 10−4 solar masses (M⊙) per year2,3,4,5,6,7,8,9,10,11,12, informing our understanding of the maximum mass-loss rate achieved during the asymptotic giant branch (AGB) phase. A conundrum arises whereby the observationally determined duration of the superwind phase is too short for these stars to lose enough mass to become white dwarfs2,3,4,6,8,9,10. Here we report on the detection of spiral structures around two cornerstone extreme OH/IR stars, OH 26.5 + 0.6 and OH 30.1 − 0.7, thereby identifying them as wide binary systems. Hydrodynamic simulations show that the companion’s gravitational attraction creates an equatorial density enhancement mimicking a short, extreme superwind phase, thereby solving the decades-old conundrum. This discovery restricts the maximum mass-loss rate of AGB stars to around the single-scattering radiation pressure limit of a few 10−5 M⊙ yr−1. This has crucial implications for nucleosynthetic yields, planet survival and the wind-driving mechanism.
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Figures 1–3, and Supplementary Figs. 1 and 2 were made using CASA35. Supplementary Fig. 3 was made using a simple Python script that can be distributed upon request. Supplementary Fig. 4 is based on ballistic trajectory calculations by one of the authors46 solving the equation of motion using a classical fourth-order Runge–Kutta scheme. The code is available for collaboration with I.E.M. upon reasonable request.
The ALMA data from proposals 2015.1.00054.S, 2016.1.00005.S and 2016.2.00088.S can be retrieved from the ALMA data archive at http://almascience.eso.org/aq/. The data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request.
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This paper uses the ALMA data ADS/JAO.ALMA2015.1.00054.S, 2016.1.00005.S and 2016.2.00088.S. ALMA is a partnership of ESO (representing its member states), NSF (United States) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This paper makes use of the CASA data reduction package: https://casa.nrao.edu. CASA is developed by an international consortium of scientists based at the National Radio Astronomical Observatory (NRAO), the European Southern Observatory (ESO), the National Astronomical Observatory of Japan (NAOJ), the CSIRO Australia Telescope National Facility (CSIRO/ATNF) and the Netherlands Institute for Radio Astronomy (ASTRON) under the guidance of NRAO. L.D., T.D., W.H. and M.V.d.S. acknowledge support from the ERC consolidator grant 646758 AEROSOL. T.D. acknowledges support from the Fund of Scientific Research Flanders (FWO). D.A.G.-H. acknowledges support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA-2017-88254-P. We acknowledge the help of C. Gottlieb (Harvard University) for his editorial advice on the manuscript.
The authors declare no competing interests.
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Supplementary text, Supplementary references, Supplementary Figures 1–4, Supplementary Video 1 caption, Supplementary Video 2 caption.
Animated 12CO J = 3–2 channel map of star OH 26.5 + 0.6.
Animated 12CO J = 2–1 channel map of star OH 30.1-0.7.
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Decin, L., Homan, W., Danilovich, T. et al. Reduction of the maximum mass-loss rate of OH/IR stars due to unnoticed binary interaction. Nat Astron 3, 408–415 (2019). https://doi.org/10.1038/s41550-019-0703-5