Deteonation of commercial explosives. The detonation characteristics of VA-4 ammonites and “Skal'nyi” ammonite No. 1. Shock wave parameters at the explosives/rock interface

1971 ◽  
Vol 7 (4) ◽  
pp. 408-411
Author(s):  
A. N. Dremin ◽  
K. K. Shvedov ◽  
A. L. Krivchenko ◽  
E. G. Baranov ◽  
V. E. Klapovskii ◽  
...  
Keyword(s):  
Shock Wave ◽  
Wave Parameters ◽  
Rock Interface ◽  
Detonation Characteristics

Conditions needed for generation of type II radio emission in the interplanetary space

2021 ◽  
Author(s):  
Immanuel Christopher Jebaraj ◽  
Athanasios Kouloumvakos ◽  
Jasmina Magdalenic ◽  
Alexis Rouillard ◽  
Vratislav Krupar ◽  
...  
Keyword(s):  
Shock Wave ◽  
Shock Waves ◽  
Radio Emission ◽  
Interplanetary Space ◽  
Region Of Interest ◽  
Type Ii ◽  
Radio Observations ◽  
Wave Parameters ◽  
First Results ◽  
Radio Signature

<p>Eruptive events such as Coronal mass ejections (CMEs) and flares cangenerate shock waves. Tracking shock waves and predicting their arrival at Earth is a subject of numerous space weather studies. Ground-based radio observations allow us to locate shock waves in the low corona while space-based radio observations provide us opportunity to track shock waves in the inner heliosphere. We present a case study of CME/flare event, associated shock wave and its radio signature, i.e. type II radio burst.</p><p>In order to analyze the shock wave parameters, we employed a robust paradigm. We reconstructed the shock wave in 3D using multi-viewpoint observations and modelled the evolution of its parameters using a 3D MHD background coronal model produced by the MAS (Magnetohydrodynamics Around a Sphere).</p><p>To map regions on the shock wave surface, possibly associated with the electron acceleration, we combined 3D shock modelling results with the 3D source positions of the type II burst obtained using the radio triangulation technique. We localize the region of interest on the shock surface and examine the shock wave parameters to understand the relationship between the shock wave and the radio event. We analyzed the evolution of the upstream plasma characteristics and shock wave parameters during the full duration of the type II radio emission. First results indicate that shock wave geometry and its relationship with shock strength play an important role in the acceleration of electrons responsible for the generation of type II radio bursts.</p>

Experiments on the relation of shock wave parameters to stone disintegration

1998 ◽  
Vol 103 (5) ◽  
pp. 3072-3072 ◽  
Author(s):  
Thomas Dreyer ◽  
Rainer E. Riedlinger ◽  
Eckard Steiger
Keyword(s):  
Shock Wave ◽  
Wave Parameters

Shock-wave parameters in the explosive expansion of effervescing liquid

1991 ◽  
Vol 27 (4) ◽  
pp. 438-442 ◽  
Author(s):  
S. P. Medvedev ◽  
A. N. Polenov ◽  
B. E. Gel'fand
Keyword(s):  
Shock Wave ◽  
Wave Parameters ◽  
Explosive Expansion

Rankine–Hugoniot-Berechnungen für Nichtgleichgewichts-Plasmen

1966 ◽  
Vol 21 (11) ◽  
pp. 1960-1963
Author(s):  
J. Artmann
Keyword(s):  
Shock Wave ◽  
Shock Waves ◽  
Pressure Ratio ◽  
Density Ratio ◽  
Charged Particles ◽  
Strong Shock ◽  
Ion Temperature ◽  
Saha Equation ◽  
Wave Parameters ◽  
Strong Shock Waves

In optically thin plasmas produced by strong shock waves the SAHA equation is no longer valid to describe the conditions directly behind the shock wave. Photoionisation may be neglected in the balance of production and recombination of charged particles. For the case of nonequilibrium a calculation assuming various ratios of electron to ion temperature (ϑ= TeT) shows that the shock wave parameters are described sufficiently well by the Korona-equation. Temperature, density ratio and electron density are increased with increasing ϑ whereas the pressure ratio is independent of the kind of equilibrium and ϑ.

New craters on Mars: Air shock wave traces

2020 ◽  
Author(s):  
Boris Ivanov ◽  
Gwen Barnes ◽  
Ingrid Daubar ◽  
Colin Dundas ◽  
Alfred McEwen ◽  
...  
Keyword(s):  
Shock Wave ◽  
Spherical Wave ◽  
Impact Craters ◽  
Analysis Program ◽  
Martian Surface ◽  
Impact Cratering ◽  
Near Surface ◽  
Origin And Evolution ◽  
Wave Parameters ◽  
Wave Passage

<p>The idea of visualizing shock wave passage along a dusty (sooty) surface was first proposed and tested by Ernst Mach. High resolution HiRISE images of new impact craters on dusty areas of Mars gave in many cases revealed dark “fresh” halos around craters. In ~7% of cases they have low albedo/color contrasting curved strips near craters referred to as “parabolas” and “scimitars”. We analyze these albedo details as the possible surface footprints of atmospheric shock waves generated during atmospheric passage and shocks from impact cratering by small meteoroids and their fragments. In this approach “parabolas” are the trace of two colliding air shocks propagated from a pair of neighboring craters formed after a meteoroid fragmented during the atmosphere passage. The mechanism of the “scimitar’s” formation is more enigmatic and tentatively could be related to the interaction of the ballistic cone wave and a spherical wave from the point of impact. The study of images is accompanied by numerical modeling of impact of small projectiles at the atmosphere/rock boundary. This modeling constrains the minimum efficiency of an impact to generate the air shock wave in the rarified Martian atmosphere below of 0.1% of the kinetic energy for non-volatile targets. Targets with near surface volatiles could amplificated the air blast (if volatiles are presented in the shocked zone). The study is intended to estimate the air-shock wave parameters along the visible surface traces around impact craters. By constraining shock wave parameters opens new possibilities for investigating the mechanical properties of the Martian surface.<br>The work is supported by RAS program 12 “Universe Origin and Evolution from Earth-based Observations and Space Missions” (BAI), and a grant from the NASA Mars Data Analysis Program, number 80NSSC18K1368.</p>

Calculation of the shock wave parameters from the detonation of combustible gas mixtures of variable composition

1985 ◽  
Vol 21 (3) ◽  
pp. 355-360 ◽  
Author(s):  
B. E. Gel'fand ◽  
S. A. Gubin ◽  
V. N. Mikhalkin ◽  
V. A. Shargatov
Keyword(s):  
Shock Wave ◽  
Gas Mixtures ◽  
Variable Composition ◽  
Combustible Gas ◽  
Wave Parameters

Optimal shock wave parameters for supersonic inlets

1996 ◽  
Vol 12 (1) ◽  
pp. 202-205 ◽  
Author(s):  
Pavel Safarik ◽  
Arnold Polak
Keyword(s):  
Shock Wave ◽  
Wave Parameters
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