Natalia Vladimirova | University of New Mexico (original) (raw)
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Papers by Natalia Vladimirova
Physical review, Jun 16, 2003
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NUMERICAL ANALYSIS AND APPLIED MATHEMATICS ICNAAM 2011: International Conference on Numerical Analysis and Applied Mathematics, 2011
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Physical Review Letters, Oct 16, 2018
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Optics Letters, Jun 3, 2010
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AIP Conference Proceedings, 2009
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Philosophical Transactions of the Royal Society A, Jan 17, 2022
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Astrophysical Journal Supplement Series, Dec 1, 2002
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Nonlinearity, Oct 18, 2013
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Fluids, May 13, 2021
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Jetp Letters, Oct 30, 2018
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American Astronomical Society Meeting Abstracts #208, Jun 1, 2006
ABSTRACT The enormous (1012) range in the spatial scales encountered in the thermonuclear deflagr... more ABSTRACT The enormous (1012) range in the spatial scales encountered in the thermonuclear deflagration stage of a Type Ia supernova mandates the use of a model to describe burning on unresolved scales. A realistic model must accurately describe (1) the nuclear energy that is released, (2) the timescale on which it is released, and (3) compositional changes occurring in the flame. Building on the thick flame model of Khokhlov (1995), we have developed a three-stage burning model (involving carbon fusion, burning to Si-group, and finally relaxation to NSE). In this poster, we present details of and simulations with this new three-stage burning model. We utilize self-heating network calculations of nuclear burning to quantify the energies that are released and the timescales on which the energies are released. We use tabulated results from a nuclear statistical equilibrium (NSE) code for describing the state of the evolving ash in NSE and addressing the effects of neutronization. The reaction network includes up-to-date thermonuclear reaction rates, weak interaction rates, effects of electron screening, and nuclear partition functions, and has been shown to be consistent with the NSE method. We have initiated a study with the improved energetics exploring the effect of the initial conditions on the deflagration phase. In particular, we present the results of two-dimensional simulations in which we vary the off-set distance of a single ignition spot from the center of the white dwarf.This work was supported by the U.S. Department of Energy under grant No. B523820 to the Center for Astrophysics Flashes and by the National Science Foundation under grant PHY 02-16783 to the Joint Institute for Nuclear Astrophysics and grant AST-0507456.
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arXiv (Cornell University), Aug 22, 2012
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arXiv (Cornell University), May 7, 2004
We present the first high-resolution three-dimensional simulations of the deflagration phase of T... more We present the first high-resolution three-dimensional simulations of the deflagration phase of Type Ia supernovae that treat the entire massive white dwarf. We report the results of simulations in which ignition of the nuclear burning occurs slightly off-center. The subsequent evolution of the nuclear burning is surprisingly asymmetric with a growing bubble of hot ash rapidly rising to the stellar surface. Upon reaching the surface, the mass of burned material is approx0.075Msun\approx 0.075 M_\sunapprox0.075Msun and the kinetic energy is 4.3times10494.3 \times 10^{49}4.3times1049 ergs. The velocity of the top of the rising bubble approaches 8000 km s$^{-1}$. The amount of the asymmetry found in the model offers a natural explanation for the observed diversity in Type Ia supernovae. Our study strongly disfavors the classic central-ignition pure deflagration scenario by showing that the result is highly sensitive to details of the initial conditions.
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Optics Letters, Jun 4, 2014
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Combustion Theory and Modelling, Sep 1, 2003
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Physics of Plasmas, Jul 1, 2014
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Optics Express, Nov 20, 2015
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Physical Review E
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arXiv (Cornell University), Sep 13, 2022
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Physical review, Jun 16, 2003
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NUMERICAL ANALYSIS AND APPLIED MATHEMATICS ICNAAM 2011: International Conference on Numerical Analysis and Applied Mathematics, 2011
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Physical Review Letters, Oct 16, 2018
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Optics Letters, Jun 3, 2010
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AIP Conference Proceedings, 2009
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Philosophical Transactions of the Royal Society A, Jan 17, 2022
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Astrophysical Journal Supplement Series, Dec 1, 2002
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Nonlinearity, Oct 18, 2013
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Fluids, May 13, 2021
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Jetp Letters, Oct 30, 2018
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American Astronomical Society Meeting Abstracts #208, Jun 1, 2006
ABSTRACT The enormous (1012) range in the spatial scales encountered in the thermonuclear deflagr... more ABSTRACT The enormous (1012) range in the spatial scales encountered in the thermonuclear deflagration stage of a Type Ia supernova mandates the use of a model to describe burning on unresolved scales. A realistic model must accurately describe (1) the nuclear energy that is released, (2) the timescale on which it is released, and (3) compositional changes occurring in the flame. Building on the thick flame model of Khokhlov (1995), we have developed a three-stage burning model (involving carbon fusion, burning to Si-group, and finally relaxation to NSE). In this poster, we present details of and simulations with this new three-stage burning model. We utilize self-heating network calculations of nuclear burning to quantify the energies that are released and the timescales on which the energies are released. We use tabulated results from a nuclear statistical equilibrium (NSE) code for describing the state of the evolving ash in NSE and addressing the effects of neutronization. The reaction network includes up-to-date thermonuclear reaction rates, weak interaction rates, effects of electron screening, and nuclear partition functions, and has been shown to be consistent with the NSE method. We have initiated a study with the improved energetics exploring the effect of the initial conditions on the deflagration phase. In particular, we present the results of two-dimensional simulations in which we vary the off-set distance of a single ignition spot from the center of the white dwarf.This work was supported by the U.S. Department of Energy under grant No. B523820 to the Center for Astrophysics Flashes and by the National Science Foundation under grant PHY 02-16783 to the Joint Institute for Nuclear Astrophysics and grant AST-0507456.
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arXiv (Cornell University), Aug 22, 2012
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arXiv (Cornell University), May 7, 2004
We present the first high-resolution three-dimensional simulations of the deflagration phase of T... more We present the first high-resolution three-dimensional simulations of the deflagration phase of Type Ia supernovae that treat the entire massive white dwarf. We report the results of simulations in which ignition of the nuclear burning occurs slightly off-center. The subsequent evolution of the nuclear burning is surprisingly asymmetric with a growing bubble of hot ash rapidly rising to the stellar surface. Upon reaching the surface, the mass of burned material is approx0.075Msun\approx 0.075 M_\sunapprox0.075Msun and the kinetic energy is 4.3times10494.3 \times 10^{49}4.3times1049 ergs. The velocity of the top of the rising bubble approaches 8000 km s$^{-1}$. The amount of the asymmetry found in the model offers a natural explanation for the observed diversity in Type Ia supernovae. Our study strongly disfavors the classic central-ignition pure deflagration scenario by showing that the result is highly sensitive to details of the initial conditions.
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Optics Letters, Jun 4, 2014
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Combustion Theory and Modelling, Sep 1, 2003
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Physics of Plasmas, Jul 1, 2014
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Optics Express, Nov 20, 2015
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Physical Review E
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arXiv (Cornell University), Sep 13, 2022
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