3D hydrodynamic simulations of white dwarf–main-sequence star collisions – I. Head-on collisions
Recently inaugurated telescopes, such as the MeerKAT radio telescope and the upcoming Rubin Observatory Le gac y Surv e y of Space and Time, will be able to detect millions of transient events in the night sky. Stellar collisions between white dwarfs (WDs) and main-sequence (MS) stars may be detecta...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/371452 |
| Acceso en línea: | http://hdl.handle.net/10261/371452 |
| Access Level: | acceso abierto |
| Palabra clave: | Hydrodynamics Nuclear reactions Nucleosynthesis Stars: mass-loss Globular clusters: general |
| Sumario: | Recently inaugurated telescopes, such as the MeerKAT radio telescope and the upcoming Rubin Observatory Le gac y Surv e y of Space and Time, will be able to detect millions of transient events in the night sky. Stellar collisions between white dwarfs (WDs) and main-sequence (MS) stars may be detectable among such transients. Simulations will play a key role in characterizing these events and selecting targets for follow-up. We present 3D smoothed particle hydrodynamics models of dynamical interactions between a 0 . 6 M WD and 0.3, 0.6, and 1 . 2 M MS stars within globular cluster environments. Utilizing a 34-isotope nuclear network, we investigate the energetics, gas morphologies, and mass-loss properties of these collisions for different stellar mass ratios. Our models predict an o v erabundance of 13 C, 15 N, and 17 O isotopes relative to solar abundances. Moreo v er, we find that the time-scale of the collisions is too short and maximum temperatures too low for any significant hydrogen burning or triple-alpha reactions to occur. This combined with a negligible production of elements heavier than neon may be key signatures in distinguishing these events from other transient events with similar peak bolometric luminosities ( ∼10 38 −10 41 erg s −1 ). |
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