Hydrodynamic simulations of the recurrent nova T Coronae Borealis: Nucleosynthesis predictions

TL;DR

This study uses hydrodynamic simulations to explore the characteristics and nucleosynthesis of recurrent nova T Coronae Borealis, predicting its next outburst and analyzing how various parameters influence explosion properties and elemental abundances.

Contribution

The paper presents new hydrodynamic models of T CrB's nova outbursts, detailing how different parameters affect explosion timing, energy, and elemental yields, aiding in understanding and predicting its eruptions.

Findings

Mass-accretion rates of 10^-8 to 10^-7 Msun/yr trigger outbursts after 80 years.

Lower white dwarf luminosity or metallicity requires higher accretion rates for explosions.

Elemental abundances vary significantly with white dwarf mass, providing diagnostic tools.

Abstract

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 80 yr, the next outburst is anticipated to occur imminently, thus motivating a thorough examination of the main characteristics of this system. We present new hydrodynamic models of the explosion of T CrB for different 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 show that mass-accretion rates between 10-8 - 10-7 Msun yr-1 are required to trigger an outburst after 80 yr of accretion of solar-composition material onto white dwarfs with masses about 1.30 - 1.38 Msun. 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 different white dwarf masses but identical initial luminosities reveal significant differences 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 differences offer a potential diagnostic tool for constraining the parameter space and discriminating between the various T CrB models reported in this study.