Hydrodynamic simulations of the recurrent nova T Coronae Borealis: Nucleosynthesis predictions
Context. Recurrent novae are, by definition, novae observed in outburst more than once or identified by the presence of vast supershells, ejected in previous eruptions, surrounding the system. These systems are characterized by remarkably short recurrence times between outbursts, typically ranging f...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/439538 |
| Acceso en línea: | https://hdl.handle.net/2117/439538 https://dx.doi.org/10.1051/0004-6361/202553762 |
| Access Level: | acceso abierto |
| Palabra clave: | Hydrodynamics Nuclear reactions Nucleosynthesis Abundances Binaries close Novae cataclysmic variables Àrees temàtiques de la UPC::Enginyeria civil::Geologia::Hidrologia |
| Sumario: | Context. Recurrent novae are, by definition, novae observed in outburst more than once or identified by the presence of vast supershells, ejected in previous eruptions, surrounding the system. These systems are characterized by remarkably short recurrence times between outbursts, typically ranging from 1 to about 100yr. Such short recurrence times require very high mass-accretion rates, white dwarf masses approaching the Chandrasekhar limit, and very high initial white dwarf luminosities. Aims. T Coronae Borealis (T CrB) is one of the eleven known recurrent novae in our Galaxy. It was observed in outburst in 1866 and 1946, with additional likely eruptions recorded in 1217 and 1787. Given its predicted recurrence period of approximately 80yr, the next outburst is anticipated to occur imminently, thus motivating a thorough examination of the main characteristics of this system. Methods. We present 11 new hydrodynamic models of the explosion of T CrB for di erent combinations of parameters (i.e., the mass, composition, and initial luminosity of the white dwarf, the metallicity of the accreted matter, and the mass-transfer rate). We also report on 8 additional hydrodynamic models that include mixing at the interface between the accreted envelope and the outermost layers of the underlying white dwarf, and 3 models for 1.20Mwhite dwarfs. Results. We show that mass-accretion rates of ¿ Macc 10 8 10 7 Myr 1 are required to trigger an outburst after 80yr of accretion of solar-composition material onto white dwarfs with masses MWD 130 138M and initial luminosities LWD 001 1L . For lower white dwarf luminosities, less massive white dwarfs, or reduced metallicity in the accreted material, higher mass-accretion rates are required to drive an explosion within this timescale. A decrease in metallicity or initial white dwarf luminosity leads to higher accumulated masses and ignition pressures, resulting in more violent outbursts. These outbursts exhibit higher peak temperatures, higher ejected masses, and greater kinetic energies. Models computed for di erent white dwarf masses but identical initial luminosities reveal significant di erences in the elemental abundances of a wide range of species, including Ne, Na, Mg, Al, Si, P, S, Ar, K, Ca, and Sc. These compositional di erences o er a potential diagnostic tool for constraining the parameter space and discriminating between the various T CrB models reported in this study. |
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