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3 edition of Deflagration to detonation transition in thermonuclear supernovae found in the catalog.

Deflagration to detonation transition in thermonuclear supernovae

Deflagration to detonation transition in thermonuclear supernovae

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  • 22 Currently reading

Published by Naval Research Laboratory, [National Aeronautics and Space Administration, National Technical Information Service, distributor in Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Turbulent mixing.,
  • Supernovae.,
  • Detonation.,
  • Degeneration.

  • Edition Notes

    StatementA.M. Khokhlov, E.S. Oran, J.C. Wheeler.
    SeriesNASA contractor report -- NASA CR-204441.
    ContributionsOran, Elaine S., Wheeler, J. Craig., Naval Research Laboratory (U.S.), United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL15505754M

    In a deflagration, the combustion or; these explosions create a high-pressure shock wave that causes; may also cause a deflagration-to-detonation transition To validate this model, NRL performed numerical simulations of flame acceleration and deflagration-to-detonation transition (DDT) in channels with obstacles. Deflagration and Detonation Deflagration: • Subsonic, typically 1 m/s and 7 to 10 bar starting at ambient pressure Detonation: • Supersonic • High pressure shock front ahead of the reaction zone (i.e. flame) • Adiabatic compression – gas autoignites • Average pressure 15 to 19 bar (lean), 25 to 30 bar (stoichiometric) • Typical peak pressure up to 50 bar (but see later)File Size: KB.

    to a deflagration-to-detonation transition in Type Ia supernovae (SNe Ia). We thus proceed under the assumption that the ion3,wedescribethehydro-dynamic and nucleosynthetic evolution of these He detonations under the assumption of one-dimensional (1D) spherical sym-metry. Fig. 1: Images from a two-dimensional thermonuclear supernova simulation from a neutronized-core progenitor. The left panel shows the development of fluid instabilities during the deflagration phase, the center panel shows the configuration just prior to the first detonation, and the right panel shows the configuration with two distinct detonations.

    Abstract Type Ia supernovae (SNe Ia) originate from the thermonuclear explosions of carbon-oxygen (C-O) white dwarfs (WDs). The single-degenerate scenario is a well-explored model of SNe Ia where unstable thermonuclear burning initiates in an accreting, Chandrasekhar-mass WD and forms an advancing flame. Numerical Analysis of the Deflagration to Detonation Transition in Primary Explosives21 characteristics C+ in the compression wave are straight lines (Figure 1). The point of intersection of the characteristics on which the difference in pressure is a few kbar, was assumed as the beginning of the formation of the shock wave of.


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Deflagration to detonation transition in thermonuclear supernovae Download PDF EPUB FB2

DEFLAGRATION TO DETONATION TRANSITION IN THERMONUCLEAR SUPERNOVAE A.M. Khokhlov Laboratory for Computational Physics and Fluid Dynamics, CodeNaval Research Laboratory, Washington, DC E.S.

Oran Laboratory for Computational Physics and Fluid Dynamics, CodeNaval Research Laboratory, Washington, DC J.C. Wheeler. We derive the criteria for deflagration to detonation transition (DDT) in a Type Ia supernova.

The theory is based on two major assumptions: (1) detonation is triggered via the Zeldovich gradient mechanism inside a region of mixed fuel and products, and (2) the mixed region is produced by a turbulent mixing of fuel and products either inside an active deflagration front or during the.

Get this from a library. Deflagration to detonation transition in thermonuclear supernovae. [A M Khokhlov; Elaine S Oran; J Craig Wheeler; Naval Research Laboratory (U.S.); United States. National Aeronautics and Space Administration.].

Detonating Failed Deflagration Model of Thermonuclear Supernovae I. Explosion Dynamics Article in The Astrophysical Journal March Author: Tomasz Plewa.

Carbon detonation or Carbon deflagration is the violent reignition of thermonuclear fusion in a white dwarf star that was previously slowly cooling.

It involves a runaway thermonuclear process which spreads through the white dwarf in a matter of seconds, producing a Type Ia supernova which releases an immense amount of energy as the star is blown apart.

The carbon. The thermonuclear deflagration releases enough energy to produce a healthy explosion. The turbulent flame, however, leaves large amounts of unburnt and partially burnt material near the star center, whereas observations imply these materials only in outer layers.

This disagreement could be resolved if the deflagration triggers a detonation. Thermonuclear instability in a WD core is thought to start off as a subsonic, turbulent deflagration wave or "burning" wave but then may, at some point, transition into a supernova blast or.

Deflagration is subsonic combustion propagating through heat transfer; hot burning material heats the next layer of cold material and ignites it. Most "fires" found in daily life, from flames to explosions such as that of black powder, are deflagrations.

This differs from detonation, which propagates supersonically through shock waves, decomposing a substance. The authors derive the criteria for deflagration to detonation transition (DDT) in a Type Ia supernova.

The theory is based on the two major assumptions: (i) detonation is triggered via the Zeldovich gradient mechanism inside a region of mixed fuel and products, (ii) the mixed region is produced by a turbulent mixing of fuel and products either inside an active deflagration front or.

The thermonuclear explosion of a Chandrasekhar mass white dwarf is an important class of supernovae which can attribute to various subclasses of Type Ia supernovae and accretion induced collapse. Type Ia supernovae are not only essential as their roles of standard candle in the discovery of dark energy, but also robust sources of iron-peak elements for the galactic.

The talk, "Deflagration-to-detonation Transition in Unconfined Media," is at p.m. on Sunday, Nov. 20, in Room Explore further Argonne supercomputer to simulate extreme physics of.

All theoretical and observational topics relevant to the understanding of the thermonuclear (Type Ia) supernova phenomenon are thoroughly and consistently reviewed by a panel including the foremost experts in the field.

The book covers all aspects, ranging from the observations of SNe Ia at all stages and all wavelengths to the 2D and 3D modelling of thermonuclear flames in. Deflagration to detonation experiments in granular HMX In this paper the authors report on continuing work involving a series of deflagration-to-detonation transition Abstract.

Thermonuclear explosions of Type Ia supernovae (SNIa) involve turbulent deflagrations, detonations, and possibly a deflagration-to-detonation transition.

This paper summarizes a year theoretical and numerical effort to understand the deflagration-to-detonation transition (DDT). To simulate DDT from first principles, it is necessary to resolve the relevant scales ranging from the size of the system to the flame thickness, a range that can cover up to 12 orders of magnitude in real by: Abstract The thermonuclear explosion of a Chandrasekhar mass white dwarf is an important class of supernovae which can attribute to various subclasses of Type Ia supernovae and accretion induced collapse.

Type Ia supernovae are not only essential as their roles of standard candle in the discovery of dark energy, but also robust sources of iron. Then simulations of the deflagration stage of a Type Ia thermonuclear supernovae are performed to evaluate whether a deflagration alone is enough to account for astronomical observations.

The conclusion is that the deflagration model alone is inadequate energetically, so there must be a transition to a : E. Oran. The Deflagration-to-Detonation Transition in Gas-Phase Combustion Thermonuclear Supernovae (Type Ia) - Universal Standard Candles behind shocks, transition to detonation, and the evolution of a full detonation including detonation cell structure.

Reactive Structure. completeness. The key feature of this model is that the deflagration-to-detonation transition is delayed. This delay allows the deflagration flame to produce enough inter-mediate mass elements before the detonation takes over [69].

The initial stellar setup has a central density of ρ ≈ 3× g=cm3, a mass of M ¼ M Sun, a radius ofCited by: 8. ON THE TRANSITION FROM DEFLAGRATION TO DETONATION S. BRINKLEY, We are concerned with the transition of a defla- gration wave (combustion wave), propagating in an explosive gas mixture at a rate of a few m per sec, to a detonation wave, propagating at a rate of a few km per by: the key outstanding open challenges in the theory of thermonuclear supernovae is the question of the nature of a spontaneous deflagration-to-detonation transition (sDDT) in unconfined systems.

In our previous work [10], we identified a new mechanism of sDDT. Fast deflagrations, deflagration to detonation transition (DDT) and direct detonation initiation in hydrogen-air mixtures Andrzej Teodorczyk Warsaw University of Technology.

First European Summer School on Hydrogen Safety, Belfast, August by Andrzej Teodorczyk 2 Outline • Flame acceleration in tubes and channels File Size: 6MB.The predicted transition density from this criterion remains below gcm3 after accounting for intermittency using our intermittency models.

Subject headinggs: stars: interiors — supernovae: general — turbulence 1. INTRODUCTION A successful model for Type Ia supernova (SN Ia) explosions is required to produce a deflagration to detonation.

Khokhlov AM, Oran E, Wheeler JC () Deflagration-to-detonation transition in thermonuclear supernovae. ApJ – CrossRef ADS Google Scholar Kobayashi C, Nakasato N () Chemodynamical simulations of the milky way galaxy.