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Title: Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions

Abstract

Classical novae are thermonuclear explosions that take place in the envelopes of accreting white dwarfs in binary systems. The material piles up under degenerate conditions, driving a thermonuclear runaway. The energy released by the suite of nuclear processes operating at the envelope heats the material up to peak temperatures of ~(1-4) × 10 8 K. During these events, about 10 -3-10 -7 M , enriched in CNO and, sometimes, other intermediate-mass elements (e.g., Ne, Na, Mg, Al) are ejected into the interstellar medium. To account for the gross observational properties of classical novae (in particular, the high concentrations of metals spectroscopically inferred in the ejecta), models require mixing between the (solar-like) material transferred from the secondary and the outermost layers (CO- or ONe-rich) of the underlying white dwarf. Recent multidimensional simulations have demonstrated that Kelvin-Helmholtz instabilities can naturally produce self-enrichment of the accreted envelope with material from the underlying white dwarf at levels that agree with observations. However, the feasibility of this mechanism has been explored in the framework of CO white dwarfs, while mixing with different substrates still needs to be properly addressed. We performed three-dimensional simulations of mixing at the core-envelope interface during nova outbursts with the multidimensionalmore » code FLASH, for two types of substrates: CO- and ONe-rich. We also show that the presence of an ONe-rich substrate, as in “neon novae”, yields higher metallicity enhancements in the ejecta than CO-rich substrates (i.e., non-neon novae). Finally, a number of requirements and constraints for such 3D simulations (e.g., minimum resolution, size of the computational domain) are also outlined.« less

Authors:
 [1];  [2];  [3];  [4]
  1. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
  2. Polytechnic Univ. of Catalonia, Barcelona (Spain). Dept. of Physics; Inst. of Space Studies of Catalonia, Barcelona (Spain)
  3. Inst. of Space Studies of Catalonia, Barcelona (Spain); Polytechnic Univ. of Catalonia, Castelldefels (Spain). Dept. of Physics
  4. Univ. of Pisa (Italy). Dept. of Physics
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Sponsoring Org.:
USDOE
OSTI Identifier:
1329738
Grant/Contract Number:  
AC05-00OR22725
Resource Type:
Accepted Manuscript
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 595; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; novae; cataclysmic variables; nuclear reactions; nucleosynthesis; abundances; convection; hydrodynamics; instabilities; turbulence

Citation Formats

Casanova, Jordi, José, Jordi, García-Berro, Enrique, and Shore, Steven N. Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions. United States: N. p., 2016. Web. doi:10.1051/0004-6361/201628707.
Casanova, Jordi, José, Jordi, García-Berro, Enrique, & Shore, Steven N. Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions. United States. doi:10.1051/0004-6361/201628707.
Casanova, Jordi, José, Jordi, García-Berro, Enrique, and Shore, Steven N. Tue . "Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions". United States. doi:10.1051/0004-6361/201628707. https://www.osti.gov/servlets/purl/1329738.
@article{osti_1329738,
title = {Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions},
author = {Casanova, Jordi and José, Jordi and García-Berro, Enrique and Shore, Steven N.},
abstractNote = {Classical novae are thermonuclear explosions that take place in the envelopes of accreting white dwarfs in binary systems. The material piles up under degenerate conditions, driving a thermonuclear runaway. The energy released by the suite of nuclear processes operating at the envelope heats the material up to peak temperatures of ~(1-4) × 108 K. During these events, about 10-3-10-7 M⊙, enriched in CNO and, sometimes, other intermediate-mass elements (e.g., Ne, Na, Mg, Al) are ejected into the interstellar medium. To account for the gross observational properties of classical novae (in particular, the high concentrations of metals spectroscopically inferred in the ejecta), models require mixing between the (solar-like) material transferred from the secondary and the outermost layers (CO- or ONe-rich) of the underlying white dwarf. Recent multidimensional simulations have demonstrated that Kelvin-Helmholtz instabilities can naturally produce self-enrichment of the accreted envelope with material from the underlying white dwarf at levels that agree with observations. However, the feasibility of this mechanism has been explored in the framework of CO white dwarfs, while mixing with different substrates still needs to be properly addressed. We performed three-dimensional simulations of mixing at the core-envelope interface during nova outbursts with the multidimensional code FLASH, for two types of substrates: CO- and ONe-rich. We also show that the presence of an ONe-rich substrate, as in “neon novae”, yields higher metallicity enhancements in the ejecta than CO-rich substrates (i.e., non-neon novae). Finally, a number of requirements and constraints for such 3D simulations (e.g., minimum resolution, size of the computational domain) are also outlined.},
doi = {10.1051/0004-6361/201628707},
journal = {Astronomy and Astrophysics},
number = ,
volume = 595,
place = {United States},
year = {2016},
month = {10}
}

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