Dynamics of bubbles in supernovae and turbulent vortices

Bychkov, Vitaly; Попов, М. В.; Oparin, A. M.; Stenflo, L.; Чечеткин, В. М.

doi:10.1134/s1063772906040044

Cited by 23 publications

(34 citation statements)

References 26 publications

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“…We took the region of instability to be perfectly spherical at the initial time. However, as it rises, the matter with enhanced entropy (bubble) is stretched along the rotational axis of the star, in accordance with the predictions of the analytical theory [7]. It is shown on Fig.…”

Section: Resultssupporting

confidence: 85%

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Mechanism Of Supernova

Чечеткин¹,

Ruffini²,

Vereshchagin³

2010

AIP Conference Proceedings

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Section: Resultssupporting

confidence: 85%

“…The successive thermonuclear outbursts can essentially result in the establishment of a detonation regime. Later, numerical simulations of thermonuclear supernovae [7] supported this qualitative conclusion. For example, Fig.…”

Section: Resultsmentioning

confidence: 84%

Mechanism Of Supernova

Чечеткин¹,

Ruffini²,

Vereshchagin³

2010

AIP Conference Proceedings

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“…It is necessary to take into account the interactions between particles and their transport in transparent and opaque regions. Early multidimensional models for thermonuclear supernovae were considered in [35,36] (including rotational effects in the envelope during the supernova explosion) and in [37].…”

Section: Introductionmentioning

confidence: 99%

Supernova explosion mechanism taking into account large-scale convection and neutrino transport

Aksenov

Чечеткин

2014

Astron. Rep.

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Two types of supernovae are considered: thermonuclear supernovae, whose explosions are due to thermonuclear energy, and core-collapse supernovae, whose explosions are due to the gravitational energy of collapsing stars released in the form of neutrinos. Numerical models of supernovae are discussed. The main problem in devising supernova explosion mechanisms is producing the energy required to disperse the envelope. In theoretical models, it is necessary to solve multi-dimensional problems involving complex physics (3D gas dynamics, neutrino transport, large-scale convective instability, and other important physical processes). In recent years, the development of large-scale convection during supernova explosions has been reconsidered. Self-consistent problems problems in three-dimensional, gas-dynamical instability have been considered. Two-dimensional gas-dynamical calculations taking into account neutrino absorption in the envelope have been performed. The spherically symmetric collapse and neutrino transport were calculated including all reactions, leading to a new understanding of possible paths for the development of supernova theory. The main emphasis is placed on the neutrino transport and the basis for promising multidimensional models taking into account large-scale convective instability.

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“…An "isentropic" system of gas dynamic equations has been used in a numerical simulation of the dynamics of supernova bubbles [2]. The supernova shock wave, however, has a large amplitude (the Mach number of the shock wave from the supernova can reach tens) and substantially determines the structure of the flow after the shock front.…”

Section: On the Possibility Of Using The Isentropic Equations For Nummentioning

confidence: 99%

“…1. Although the use of such isentropic schemes has continued [2,3], the errors in the law of energy conservation due to the application of entropy conservation at strong discontinuities have not been analyzed. Evidently, an isentropic jump requires removal of energy from the post-shock gas, since the entropy of the gas in a real jump (shock wave) increases, and heat extraction is needed to conserve it.…”

Section: Introductionmentioning

confidence: 99%