AGB winds in interacting binary stars

Bermúdez-Bustamante, Luis C.; Garcı́a-Segura, Guillermo; Steffen, W.; Sabin, L.

doi:10.1093/mnras/staa403

Cited by 26 publications

(17 citation statements)

References 78 publications

(95 reference statements)

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“…Phenomena arising from post-CE binaries include Type Ia supernovae (Iben & Tutukov 1984;Ruiter et al 2009;Toonen et al 2012), and also classical novae (Livio et al 1990), X-ray binaries (Kalogera & Webbink 1998;Taam & Ricker 2010), white-dwarf mergers (Pakmor et al 2010;Ruiter et al 2013), and gravitational wave sources (Belczynski et al 2002). Moreover, the CE phase is thought to be responsible for the shapes of some planetary nebulae (de Kool 1990;Nordhaus et al 2007;Hillwig et al 2016;Bermúdez-Bustamante et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Common-envelope evolution with an asymptotic giant branch star

Sand

Ohlmann

Schneider

et al. 2020

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Common-envelope phases are decisive for the evolution of many binary systems. Cases with asymptotic giant branch (AGB) primary stars are of particular interest because they are thought to be progenitors of various astrophysical transients. In three-dimensional hydrodynamic simulations with the moving-mesh code AREPO, we study the common-envelope evolution of a 1.0 M⊙ early-AGB star with companions of different masses. Although the stellar envelope of an AGB star is less tightly bound than that of a red giant, we find that the release of orbital energy of the core binary is insufficient to eject more than about twenty percent of the envelope mass. Ionization energy that is released in the expanding envelope, however, can lead to complete envelope ejection. Because recombination proceeds largely at high optical depths in our simulations, it is likely that this effect indeed plays a significant role in the considered systems. The efficiency of mass loss and the final orbital separation of the core binary system depend on the mass ratio between the companion and the primary star. Our results suggest a linear relation between the ratio of final to initial orbital separation and this parameter.

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Section: Introductionmentioning

confidence: 99%

Common-envelope evolution with an asymptotic giant branch star

Sand

Ohlmann

Schneider

et al. 2020

A&A

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“…Mass flowing towards the companion leaves the system via the L 2 Lagrangian point, thereby creating a spiral arm (Frankowski & Jorissen 2007;Chen et al 2017). However, if the companion is massive enough, the spiral arm might remain bound and wrap around the binary, creating a ring as it intersects itself (Shu et al 1979;Pejcha et al 2016;MacLeod et al 2018;Bermúdez-Bustamante et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Disc-binary interactions in depleted post-AGB binaries

Oomen

Pols

Winckel

et al. 2020

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Binary post-asymptotic giant branch (post-AGB) stars have orbital periods in the range of 100−2500 days in eccentric orbits. They are surrounded by circumbinary dusty discs. They are the immediate result of unconstrained binary interaction processes. Their observed orbital properties do not correspond to model predictions: Neither the periods nor the high eccentricities are expected. Indeed, many orbits are eccentric despite the strong tidal interaction when the primary had giant dimensions on the red giant branch and AGB. Our goal is to investigate if interactions between a binary and its circumbinary disc during the post-AGB phase can result in their eccentric orbits, while simultaneously explaining the chemical anomaly known as depletion. For this paper, we selected three binaries (EP Lyr, RU Cen, HD 46703) with well-constrained orbits, luminosities, and chemical abundances. We used the MESA code to evolve post-AGB models, while including the accretion of metal-poor gas. This allows us to constrain the evolution of the stars and study the impact of circumbinary discs on the orbital properties of the models. We investigate the effect of torques produced by gas inside the binary cavity and the effect of Lindblad resonances on the orbit, while also including the tidal interaction following the equilibrium tide model. We find that none of our models are able to explain the high orbital eccentricities of the binaries in our sample. The accretion torque does not significantly impact the binary orbit, while Lindblad resonances can pump the eccentricity up to only e ≈ 0.2. At higher eccentricities, the tidal interaction becomes too strong, so the high observed eccentricities cannot be reproduced. However, even if we assume tides to be ineffective, the eccentricities in our models do not exceed ≈0.25. Finally, the orbit of RU Cen is too wide to reproduce with disc-binary interactions by starting from a circular orbit. We conclude that either our knowledge of disc-binary interactions is still incomplete, or the binaries must have left their phase of strong interaction in an eccentric orbit.

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“…When in a binary system, the mass loss of the AGB star can be concentrated on the orbital plane of the system, with the bulk Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. of the mass being ejected via the L2 Lagrangian point (Hubová & Pejcha 2019, Bermúdez-Bustamante et al 2020. The focused mass loss of the star can then become a circumbinary disk (Shu et al 1979, Pejcha et al 2016, MacLeod et al 2018.…”

Section: Introductionmentioning

confidence: 99%

Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

Bollen

Kamath

Marco

et al. 2020

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Aims. In this study we determine the morphology and mass-loss rate of jets emanating from the companion in post-asymptotic giant branch (post-AGB) binary stars with a circumbinary disc. In doing so we also determine the mass-accretion rates onto the companion, and investigate the source feeding the circum-companion accretion disc. Methods. We perform a spatio-kinematic modelling of the jet of two well-sampled post-AGB binaries, BD+46°442 and IRAS 19135+3937, by fitting the orbital phased time series of Hα spectra. Once the jet geometry, velocity, and scaled density structure are computed, we carry out radiative transfer modelling of the jet for the first four Balmer lines to determine the jet densities, thus allowing us to compute the jet mass-loss rates and mass-accretion rates. We distinguish the origin of the accretion by comparing the computed mass-accretion rates with theoretically estimated mass-loss rates, both from the post-AGB star and from the circumbinary disc. Results. The spatio-kinematic model of the jet reproduces the observed absorption feature in the Hα lines. The jets have an inner region with extremely low density in both objects. The jet model for BD+46°442 is tilted by 15° with respect to the orbital axis of the binary system. IRAS 19135+3937 has a smaller tilt of 6°. Using our radiative transfer model, we find the full 3D density structure of both jets. By combining these results, we can compute the mass-loss rates of the jets, which are of the order of 10−7 − 10−5 M⊙ yr−1. From this we estimate mass-accretion rates onto the companion of 10−6 − 10−4 M⊙ yr−1. Conclusions. Based on the mass-accretion rates found for these two objects, we conclude that the circumbinary disc is most likely the source feeding the circum-companion accretion disc. This is in agreement with the observed depletion patterns in post-AGB binaries, which is caused by re-accretion of gas from the circumbinary disc that is under-abundant in refractory elements. The high accretion rates from the circumbinary disc imply that the lifetime of the disc will be short. Mass transfer from the post-AGB star cannot be excluded in these systems, but it is unlikely to provide a sufficient mass-transfer rate to sustain the observed jet mass-loss rates.

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AGB winds in interacting binary stars

Cited by 26 publications

References 78 publications

Common-envelope evolution with an asymptotic giant branch star

Common-envelope evolution with an asymptotic giant branch star

Disc-binary interactions in depleted post-AGB binaries

Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

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