3D1D hydro-nucleosynthesis simulations. I. Advective-reactive post-processing method and its application to H ingestion into He-shell flash convection in rapidly accreting white dwarfs

Abstract

We present two mixing models for post-processing of 3D hydrodynamic simulations applied to convective-reactive i-process nucleosynthesis in a rapidly accreting white dwarf (RAWD) with $[Fe/H]=-2.6$, in which H is ingested into a convective He shell. A 1D advective two-stream model adopts physically motivated radial and horizontal mixing coefficients constrained by 3D hydrodynamic simulations. A simpler approach uses diffusion coefficients calculated from the same simulations. All 3D simulations include the energy feedback of the ${}^{12}$C(p,$\gamma$)${}^{13}$N reaction from the H entrainment. Global oscillations of shell H ingestion in two of the RAWD simulations cause bursts of entrainment of H and non-radial hydrodynamic feedback. With the same nuclear network as in the 3D simulations, the 1D advective two-stream model reproduces the rate and location of the H burning within the He shell closely matching the 3D simulation predictions, as well as qualitatively displaying the asymmetry of the $X_{\mathrm{H}}$ profiles between the up- and downstream. With a full i-process network the advective mixing model captures the difference in the n-capture nucleosynthesis in the up- and downstream. For example, ${}^{89}$Kr and ${}^{90}$Kr with half-lives of 3.18 min and 32.3 s differ by a factor 2-10 in the two streams. In this particular application the diffusion approach provides globally the same abundance distribution as the advective two-stream mixing model. The resulting i-process yields are in excellent agreement with observations of the exemplary CEMP-r/s star CS31062-050.

arXiv comment18 pages, 17 figures, 2 tables, accepted for publication in MNRAS

References in corpus (27)

• The chemical composition of the Sun
• Modules for Experiments in Stellar Astrophysics (MESA)
• Turbulent Convection in Stellar Interiors. I. Hydrodynamic Simulation
• Convective-reactive proton-C12 combustion in Sakurai's object (V4334 Sagittarii) and implications for the evolution and yields from the first generations of stars
• NuGrid stellar data set I. Stellar yields from H to Bi for stars with metallicities Z = 0.02 and Z = 0.01
• NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with Mzams = 1 to 25Msun and Z = 0.0001 to 0.02
• The Last Minutes of Oxygen Shell Burning in a Massive Star
• Active Carbon and Oxygen Shell Burning Hydrodynamics
• i-process nucleosynthesis and mass retention efficiency in He-shell flash evolution of rapidly accreting white dwarfs
• Global non-spherical oscillations in 3-D $4\pi$ simulations of the H-ingestion flash
• MESA Models of Classical Nova Outbursts: The Multicycle Evolution and Effects of Convective Boundary Mixing
• One-, Two-, and Three-dimensional Simulations of Oxygen Shell Burning Just Before the Core-Collapse of Massive Stars
• Idealised hydrodynamic simulations of turbulent oxygen-burning shell convection in 4π geometry
• The i-process yields of rapidly-accreting white dwarfs from multicycle He-shell flash stellar evolution models with mixing parameterizations from 3D hydrodynamics simulations
• The s-process in metal-poor stars: Abundances for 22 neutron-capture elements in CS 31062-050
• Large-Scale Mixing in a Violent Oxygen-Neon Shell Merger Prior to a Core-Collapse Supernova
• Application of a Theory and Simulation based Convective Boundary Mixing model for AGB Star Evolution and Nucleosynthesis
• Convective-reactive nucleosynthesis of K, Sc, Cl and p-process isotopes in O-C shell mergers
• 3D hydrodynamic simulations of C ingestion into a convective O shell
• i-Process Contribution of Rapidly Accreting White Dwarfs to the Solar Composition of First-Peak Neutron-Capture Elements
• Properties of Convective Oxygen and Silicon Burning Shells in Supernova Progenitors
• Convective boundary mixing in a post-He core burning massive star model
• The Impact of Hydrodynamic Mixing on Supernova Progenitors
• A phenomenological modification of thermohaline mixing in globular cluster red giants
• Multidimensional hydrodynamic simulations of the hydrogen injection flash
• Impact of Convective Boundary Mixing on the TP-AGB
• Chromium Nucleosynthesis and Silicon-Carbon Shell Mergers in Massive Stars

Cited by in corpus (14)

• Convective H-He Interactions in Massive Population III Stellar Evolution Models
• Horizons: Nuclear Astrophysics in the 2020s and Beyond
• The intermediate neutron capture process. III. The i-process in AGB stars of different masses and metallicities without overshoot
• 3D hydrodynamic simulations of massive main-sequence stars. I. Dynamics and mixing of convection and internal gravity waves
• The impact of (n,$\gamma$) reaction rate uncertainties of unstable isotopes on the i-process nucleosynthesis of the elements from Ba to W
• 3D hydrodynamics simulations of internal gravity waves in red giant branch stars
• Dynamics in a stellar convective layer and at its boundary: Comparison of five 3D hydrodynamics codes
• Presolar grains
• The imprint of convection on Type I X-ray bursts: Pauses in photospheric radius expansion lightcurves
• 3D hydrodynamics simulations of core convection in supermassive main-sequence stars
• Production of radioactive ${}^{22}$Na in core-collapse supernovae: the Ne-E(L) component in presolar grains and its possible consequences on supernova observations
• The $i$-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
• A primer on the formation and evolution of hydrogen deficient Central Stars of Planetary Nebulæ and Related Objects
• Nuclear astrophysics