Gone with the wind: the impact of wind mass transfer on the orbital evolution of AGB binary systems

Saladino, M. I.; Pols, O. R.; Helm, Edwin van der; Pelupessy, Inti; Zwart, Simon Portegies

doi:10.1051/0004-6361/201832967

Cited by 55 publications

(76 citation statements)

References 67 publications

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“…Further, Mastrodemos & Morris (1998) pointed out the importance of the wind velocity at the location of the companion as having a crucial effect on the resulting morphology of the wind and accretion processes. Two decades later, Saladino et al (2018;El Mellah et al (2020) described their simulations in function of the ratio of the terminal velocity to the orbital velocity of the companion and could thereby classify the morphology of their models based on several input values.…”

Section: Morphology Classificationmentioning

confidence: 99%

“…A recurring parameter of interest determining the global shape of the outflows is the velocity, more precisely the proportion of the orbital velocity of the companion and AGB star to the wind velocity (e.g. Theuns & Jorissen 1993;Saladino et al 2018;El Mellah et al 2020). In this paper, we analyse the wind morphology of a limited set of 3D SPH models, in which we vary three key parameters.…”

Section: Introductionmentioning

confidence: 99%

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SPH modelling of companion-perturbed AGB outflows including a new morphology classification scheme

Maes

Homan

Malfait

et al. 2021

A&A

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Context. Evolved low-and intermediate-mass stars are known to lose a significant amount of mass by a stellar wind, which controls the remainder of their stellar lifetime. High angular-resolution observations show that the winds of these cool stars typically exhibit mid-to small-scale density perturbations such as spirals and arcs, believed to be caused by the gravitational interaction with a (sub-)stellar companion. Aims. We aim to explore the effects of the wind-companion interaction on the 3D density and velocity distribution of the wind, as a function of three key parameters: wind velocity, binary separation and companion mass. For the first time, we compare the impact on the outflow of a planetary companion to that of a stellar companion. We intend to devise a morphology classification scheme based on a singular parameter. Methods. We run a small grid of high-resolution polytropic models with the smoothed particle hydrodynamics (SPH) numerical code Phantom to examine the 3D density structure of the AGB outflow in the orbital and meridional plane and around the poles. By constructing a basic toy model of the gravitational acceleration due to the companion, we analyse the terminal velocity reached by the outflow in the simulations. Results. We find that models with a stellar companion, large binary separation and high wind speed obtain a wind morphology in the orbital plane consisting of a single spiral structure, of which the two edges diverge due to a velocity dispersion caused by the gravitational slingshot mechanism. In the meridional plane the spiral manifests itself as concentric arcs, reaching all latitudes. When lowering the wind velocity and/or the binary separation, the morphology becomes more complex: in the orbital plane a double spiral arises, which is irregular for the closest systems, and the wind material gets focussed towards the orbital plane, with the formation of an equatorial density enhancement (EDE) as a consequence. Lowering the companion mass from a stellar to a planetary mass, reduces the formation of density perturbations significantly. Conclusions. With this grid of models we cover the prominent morphology changes in a companion-perturbed AGB outflow: slow winds with a close, massive binary companion show a more complex morphology. Additionally, we prove that massive planets are able to significantly impact the density structure of an AGB wind. We find that the interaction with a companion affects the terminal velocity of the wind, which can be explained by the gravitational slingshot mechanism. We distinguish between two types of wind focussing to the orbital plane resulting from distinct mechanisms: global flattening of the outflow as a result of the AGB star's orbital motion and the formation of an EDE as a consequence of the companion's gravitational pull. We investigate different morphology classification schemes and uncover that the ratio of the gravitational potential energy density of the companion to the kinetic energy density of the AGB outflow yields a robust classificatio...

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Section: Morphology Classificationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

SPH modelling of companion-perturbed AGB outflows including a new morphology classification scheme

Maes

Homan

Malfait

et al. 2021

A&A

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“…Some supernova progenitors emit copious amount of stellar wind prior to the explosion (Heuvel & Portegies Zwart 2013;Moriya et al 2014). The motion of the progenitor around the centre of mass modulates the wind, increasing the density in the forward direction (relative to the velocity of the progenitor) and reducing it in the backward direction (see also Ishii et al 1993;Saladino et al E-mail: almog.yalin@gmail.com 2018). When the progenitor explodes, the ejecta collide with the ripples in the wind and launch a shock wave.…”

Section: Introductionmentioning

confidence: 99%

The Signature of a Windy Radio Supernova Progenitor in a Binary System

Yalinewich

Zwart

2019

ApJL

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Type II supernova progenitors are expected to emit copious amounts of mass in a dense stellar wind prior to the explosion. When the progenitor is a member of a binary, the orbital motion modulates the density of this wind. When the progenitor explodes, the high-velocity ejecta collides with the modulated wind, which in turn produces a modulated radio signal. In this work we derive general analytic relations between the parameters of the radio signal modulations and binary parameter in the limit of large member mass ratio. We use these relations to infer the semi major axis of SN1979c and a lower bound for the mass of the companion. We further constrain the analytic estimates by numerical simulations using the AMUSE framework. In these calculations we simulate the progenitor binary system including the wind and the gravitational effect of a companion star. The simulation output is compared to the observed radio signal in supernova SN1979C. We find that it must have been a binary with an orbital period of about 2000 yr. If the exploding star evolved from a ∼ 18 M zero-age main-sequence at solar metalicity, we derive a companion mass of 5 to 12 M in an orbit with an eccentricity lower than about 0.8.

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“…We get γ am from the binary simulations by evaluating the average γ am through a spherical shell whose radius is 1.3d and center is at the center of mass of the binary. By setting the sampling radius at 1.3d, we probably underestimate the angular momentum loss from the binary because the escaping gas can still gain angular momentum as it goes beyond 1.3d (Lin 1977;Saladino et al 2018). However, the angular momentum conservation becomes worse in our code as the radius goes large (Chen et al 2018).…”

Section: Orbital Stabilitymentioning

confidence: 99%

“…and v ∞ is velocity of wind at infinity. Saladino et al (2018) multiplied the RHS of Equation 31 by an efficiency parameter α BHL which may vary from 0.8 to 1.5. This parameter is mainly empirical so we do not study which value is more appropriate for which AGB binary model.…”

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confidence: 99%

A 3D Radiation Hydrodynamic AGB Binary Model

Chen

Іванова

Carroll-Nellenback

2020

ApJ

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The origin of the chemically peculiar stars and non-zero eccentricity in evolved close binaries have been long-standing problems in stellar evolution. Answers to these questions may trace back to an intense mass transfer phase. In this work, we use AstroBEAR to solve the 3D radiation-hydrodynamic equations and calculate the mass transfer rate in asymptotic-giant-branch (AGB) binaries that undergo the wind-Roche-lobe-overflow or Bondi-Hoyle-Lyttleton (BHL) accretion. To resolve the dynamics of a circumbinary disk, we implement an azimuthal angle-dependent 3D radiation transfer. We consider optically thin cooling and obtain the number density of the coolants by solving the Saha equation. We use MESA to produce the density and temperature of the boundary condition of the AGB star. Four simulations are carried out to illustrate the transition from the wind-Roche-lobe-overflow to BHL accretion. Both circumbinary disks and spiral structure outflows can appear in the simulations. The resulting mass transfer efficiency in our models is up to a factor of eight times higher than what the standard BHL accretion scenario predicts, and the outflow gains up to 91% of its initial angular momentum when it reaches 1.3 binary separations. Consequently, some AGB binaries may undergo orbit shrinkage, and some will expand. The mass transfer efficiency is closely related to the presence of the circumbinary disks. Circumbinary disks may form when the optical thickness in the equatorial region becomes greater than a critical value. The increase of the optical thickness is due to the deflected wind.

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Gone with the wind: the impact of wind mass transfer on the orbital evolution of AGB binary systems

Cited by 55 publications

References 67 publications

SPH modelling of companion-perturbed AGB outflows including a new morphology classification scheme

SPH modelling of companion-perturbed AGB outflows including a new morphology classification scheme

The Signature of a Windy Radio Supernova Progenitor in a Binary System

A 3D Radiation Hydrodynamic AGB Binary Model

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