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Rarefaction

About: Rarefaction is a research topic. Over the lifetime, 1852 publications have been published within this topic receiving 26943 citations.


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Journal ArticleDOI
TL;DR: In this article, a small volume of an initially uniform plasma is heated with a CO2 laser focused to an intensity of 1.3*1011 W cm-2, and the evolving thermal and rarefaction wave is measured by Thomson scattering.
Abstract: A small volume of an initially uniform plasma is heated with a CO2 laser focused to an intensity of 1.3*1011 W cm-2. The evolving thermal and rarefaction wave is measured by Thomson scattering. Comparison of these measurements with a one-dimensional simulation shows that the heat flux reaches 15% of the free-streaming limit.

5 citations

Proceedings ArticleDOI
05 Jun 2006
TL;DR: In this article, an experimental study has been conducted to examine the interaction of a shock wave and a vortex ring with a cylinder and a sphere using high-speed Schlieren photography.
Abstract: *† ‡ § ** An experimental study has been conducted to examine the interaction of a shock wave and a vortex ring with a cylinder and a sphere. The experiments were carried out using a 30mm internal diameter shock-tube. The driver and driven gas was air. High-speed Schlieren photography was employed to study the development of the flow-field and the resulting interactions with the body configurations. Wall pressure measurements were also carried out to study the flow quantitatively at the apex of the cylindrical surface. Three different driver pressures of 4, 8, and 12 bar were examined under maximum driver length (1477mm); the shock wave Mach number at the exit of the tube was 1.33, 1.52 and 1.67 respectively. Nomenclature a1 = speed of sound (m/s) in region one a2 = speed of sound (m/s) in region two a3 = speed of sound (m/s) in region there a4 = speed of sound (m/s) in region four M1 = incident Mach number M3 = Mach number in region three P1 = static pressure (bar) in region one P2 = static pressure (bar) in region two P3 = static pressure (bar) in region three P4 = static pressure (bar) in region four R = universal gas constant (J/kgK) t = time (ms) count from the rupture of the diaphragm t3 = time (ms) of the reflected rarefaction head meets the rarefaction tail tc = time (ms) when rarefaction head overtakes the contact surface

5 citations

Journal ArticleDOI
TL;DR: In this article, the dynamics of the structure of a liquid layer structure behind a rarefaction wave front is studied numerically using the two-phase Iordansky-Kogarko-van Wijngaarden model and the frozen mass-velocity field model.
Abstract: The dynamics of the structure of a liquid layer structure (with microbubbles of a free gas) behind a rarefaction wave front is studied numerically using the two-phase Iordansky–Kogarko–van Wijngaarden model and the “frozen” mass-velocity field model. An analysis of the initial stage of cavitation by the Iordansky–Kogarko–van Wijngaarden model showed that tensile stresses behind the rarefaction wave front relax quickly and the mass-velocity field in the cavitation zone turns out to be “frozen.” This effect is used to describe the late stage of the development of the cavitation zone. These models were combined to study the formation of cavitating spalls in a free-surface liquid under shock-wave loading.

5 citations

Journal ArticleDOI
TL;DR: In this paper, the authors investigate the propagation of shocks with arbitrary initial strengths in polytropic stellar envelopes using a suite of spherically symmetric hydrodynamic simulations and find that shocks, no matter their initial strengths, evolve toward either the infinitely strong or infinitely weak self-similar solutions at sufficiently late times.
Abstract: Core-collapse supernovae span a wide range of energies, from much less than to much greater than the binding energy of the progenitor star. As a result, the shock wave generated from a supernova explosion can have a wide range of Mach numbers. In this paper, we investigate the propagation of shocks with arbitrary initial strengths in polytropic stellar envelopes using a suite of spherically symmetric hydrodynamic simulations. We interpret these results using the three known self-similar solutions for this problem: the Sedov-Taylor blastwave describes an infinitely strong shock and the self-similar solutions from Coughlin et al. (2018b) (Paper I) and Coughlin et al. (2019) (Paper II) describe a weak and infinitely weak shock (the latter being a rarefaction wave). We find that shocks, no matter their initial strengths, evolve toward either the infinitely strong or infinitely weak self-similar solutions at sufficiently late times. For a given density profile, a single function characterizes the long-term evolution of a shock's radius and strength. However, shocks with strengths near the self-similar solution for a weak shock (from Paper I) evolve extremely slowly with time. Therefore, the self-similar solutions for infinitely strong and infinitely weak shocks are not likely to be realized in low-energy stellar explosions, which will instead retain memory of the shock strength initiated in the stellar interior.

5 citations


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Performance
Metrics
No. of papers in the topic in previous years
YearPapers
20224
2021105
202064
201964
201864
201773