Entering the Wind Roche Lobe Overflow realm in Symbiotic Systems
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) wit...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/411372 |
| Acceso en línea: | http://hdl.handle.net/10261/411372 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion, accretion disks Binaries: symbiotic Stars: evolution Stars: low-mass Stars: mass-loss Stars: winds, outflows |
| Sumario: | 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 orbiting evolving Solar-like stars with 1, 2, and 3 M. 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 (M) and massive donors (2-3 M) 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. © 2025 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. |
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