Entering the Wind Roche Lobe Overflow realm in Symbiotic Systems

Abstract

We present a suite of dynamical simulations designed to explore the orbital and accretion properties of compact (2$-$7 AU) symbiotic systems, focusing on wind accretion, drag forces, and tidal interactions. Using three levels of physical complexity, we model systems of accreting white dwarfs (WDs) with masses of 0.7, 1.0, and 1.2 M${}_{\odot }$ orbiting evolving Solar-like stars with 1, 2, and 3 M${}_{\odot }$. We show that systems alternate between standard wind accretion and Wind Roche Lobe Overflow (WRLO) regimes during periods of high mass-loss rate experienced by the donor star (the peak of red giant phase and/or thermal pulses). For some configurations, the standard wind accretion has mass accretion efficiencies similar to those obtained by WRLO regime. Tidal forces play a key role in compact systems, leading to orbital shrinkage and enhanced accretion efficiency. We find that systems with high-mass WDs ($\ge 1$ M${}_{\odot }$) and massive donors (2$-$3 M${}_{\odot }$) are the only ones to reach the Chandrasekhar limit. Interestingly, the majority of our simulations reach the Roche lobe overflow condition that is not further simulated given the need of more complex hydrodynamical simulations. Our analysis shows that increasing physical realism, by including drag and tides, systematically leads to more compact final orbital configurations. Comparison with compact known symbiotic systems seems to suggest that they are very likely experiencing orbital decay produced by tidal forces.

arXiv comment14 pages; 9 figures; 2 tables; accepted in MNRAS

References in corpus (24)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
• REBOUND: An open-source multi-purpose N-body code for collisional dynamics
• Common Envelope Evolution: Where we stand and how we can move forward
• IAS15: A fast, adaptive, high-order integrator for gravitational dynamics, accurate to machine precision over a billion orbits
• X-ray Emissions from Accreting White Dwarfs: a Review
• REBOUNDx: A Library for Adding Conservative and Dissipative Forces to Otherwise Symplectic N-body Integrations
• Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-Novae Supersoft Source
• Distant future of the Sun and Earth revisited
• Wind Roche-lobe overflow: Application to carbon-enhanced metal-poor stars
• On the Orbits of Low-mass Companions to White Dwarfs and the Fates of the Known Exoplanets
• Orbital properties of binary post-AGB stars
• Determination of the Interior Structure of Transiting Planets in Multiple-Planet Systems
• Binary stars in the Galactic thick disc
• Orbital eccentricities of binary systems with a former AGB star
• Interacting Binaries with Eccentric Orbits II. Secular Orbital Evolution Due To Non-Conservative Mass Transfer
• Rotation Period Evolution in Low-Mass Binary Stars: The Impact of Tidal Torques and Magnetic Braking
• Symplectic integrators in the shearing sheet
• Wind Roche Lobe Overflow as a way to make type Ia supernova from the widest symbiotic systems
• Dynamical Measurements of the Interior Structure of Exoplanets
• Wind mass transfer in S-type symbiotic binaries I. Focusing by the wind compression model
• T CrB: overview of the accretion history, Roche-lobe filling, orbital solution, and radiative modeling
• Testing tidal theory using Gaia binaries: the red giant branch
• Outflow dynamics of dust-driven wind models and implications for cool envelopes of PNe