Aluminium-26 from Massive Binary Stars. I. Nonrotating Models

Brinkman, Hannah and Doherty, Carolyn and Pols, O. R. and Li, E. T. and Coté, Benoit and Lugaro, Maria (2019) Aluminium-26 from Massive Binary Stars. I. Nonrotating Models. ASTROPHYSICAL JOURNAL, 884 (1). ISSN 1538-4357

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Abstract

Aluminium-26 is a short-lived radionuclide with a half-life of 0.72 Myr, which is observed today in the Galaxy via γ-ray spectroscopy and i inferred to have been present in the early solar system via analysis o meteorites. Massive stars are considered the main contributors o 26Al. Although most massive stars are found in binar systems, the effect, however, of binary interactions on th 26Al yields has not been investigated since Braun & Langer. Here we aim to fill this gap. We have used the MESA stella evolution code to compute massive (10 M ☉ ≤ M ≤ 80 ☉) nonrotating single and binary stars of solar metallicit (Z = 0.014). We computed the wind yields for the single stars and fo the binary systems where mass transfer plays a major role. Depending o the initial mass of the primary star and orbital period, th 26Al yield can either increase or decrease in a binar system. For binary systems with primary masses up to ∼35─40 ☉, the yield can increase significantly, especially at th lower mass end, while above ∼45 M ☉ the yield becomes simila to the single-star yield or even decreases. Our preliminary results sho that compared to supernova explosions, the contribution of mass loss i binary systems to the total 26Al abundance produced by stellar population is minor. On the other hand, if massive star mas loss is the origin of 26Al in the early solar system, ou results will have significant implications for the identification of th potential stellar, or stellar population, source. This paper i dedicated to the celebration of the 100th birthday of Margaret Burbidge in recognition of the outstanding contributions she has made to nuclea astrophysics (Burbidge et al. 1957)

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