Comparison of experimental and predicted axial pressure variation for semi-infinite metallic targets

Billingsley, James P.

doi:10.2514/6.1969-361

Cited by 2 publications

(2 citation statements)

References 8 publications

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“…An important consideration is the late‐stage equivalence principle [ Huang and Chou , ; Billingsley , ; Dienes and Walsh , ]. Developed from blast wave theory, a similarity concept or “late‐stage equivalence” indicates that at some point in time (or space), the details of the projectile will no longer influence the terminal effects of the impact; in this regard, the impact is equivalent to a point source of energy and momentum [ Taylor , ; Sedov , ; Sakurai , ].…”

Section: Scaling Of Transient and Final Crater Sizementioning

confidence: 99%

Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

et al. 2017

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We use numerical modeling to investigate the combined effects of impact velocity and acoustic fluidization on lunar craters in the simple‐to‐complex transition regime. To investigate the full scope of the problem, we employed the two widely adopted Block‐Model of acoustic fluidization scaling assumptions (scaling block size by impactor size and scaling by coupling parameter) and compared their outcomes. Impactor size and velocity were varied, such that large/slow and small/fast impactors would produce craters of the same diameter within a suite of simulations, ranging in diameter from 10 to 26 km, which straddles the simple‐to‐complex crater transition on the Moon. Our study suggests that the transition from simple to complex structures is highly sensitive to the choice of the time decay and viscosity constants in the Block‐Model of acoustic fluidization. Moreover, the combination of impactor size and velocity plays a greater role than previously thought in the morphology of craters in the simple‐to‐complex size range. We propose that scaling of block size by impactor size is an appropriate choice for modeling simple‐to‐complex craters on planetary surfaces, including both varying and constant impact velocities, as the modeling results are more consistent with the observed morphology of lunar craters. This scaling suggests that the simple‐to‐complex transition occurs at a larger crater size, if higher impact velocities are considered, and is consistent with the observation that the simple‐to‐complex transition occurs at larger sizes on Mercury than Mars.

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Section: Scaling Of Transient and Final Crater Sizementioning

confidence: 99%

Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

et al. 2017

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“…However, ir has been pointed out repeatedly that quantities at the shock front ate very insensitive to details of the model, and can be approximated fairly well by any number of approximations. A recent illustration of this fact is presented in a paper by BILLI~GSLEY [5], whose results show that the experimental data was incapable of resolving the differences between a wide variety of theoretical treatments, Even in the subset of quasi-similar solutions without viscosity, there are many remaining questions about the effects of the spherical-flow assumption, the neglect of non-similarities due to non-zero projectile size, and the approximations used in defining the equation of state, to mention only a few. These ate critically reviewed in a recent survey paper by RAE [6].…”

Section: Introductionmentioning

confidence: 99%

Determination of flow field behind magnetogasdynamic spherical blast wave under the influence of viscosity

Verma

1974

Acta Physica

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A procedure has been given to determine analytica]ly the flow field behind a spherieal b]ast wave in the case of a viscous compressible f]uid under a spherica]]y symmetric magnetic field. l. IntroductionThe propagation of strong shock waves in a half space, due to surfaee explosion or impact, has becn treatcd in many lcvr of approximation. In one of these an attempt is made to account for the material strength by including a Newtonian viscosity term. This approximation seems to have been originated by S. W. YuA~ and various co-workers [1]--[4], who have further approximated the solution of the resulting equations by seeking a variety of quasisimilar solutions. In all of these solutions the viseosity coefficient is taken to be at most a function of time, but independent of space coordinates. In addition, the flow field in the half space is represented as though it were one half of a spherically symmetric flow. The predictions of this theory, for certain quantities on the symmetry axis at the shock front, ate then compared with experiment, and it is usually claimed that the agreement constitutes a validation of the model used. However, ir has been pointed out repeatedly that quantities at the shock front ate very insensitive to details of the model, and can be approximated fairly well by any number of approximations. A recent illustration of this fact is presented in a paper by BILLI~GSLEY [5], whose results show that the experimental data was incapable of resolving the differences between a wide variety of theoretical treatments, Even in the subset of quasi-similar solutions without viscosity, there are many remaining questions about the effects of the spherical-flow assumption, the neglect of non-similarities due to non-zero projectile size, and the approximations used in defining the equation of state, to mention only a few. These ate critically reviewed in a recent survey paper by RAE [6]. When a spherically symmetric magnetic field is added to this formulation along with a Newtonian viscosity term, the present paper proposes to study the composite effect of all the approximations.

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Comparison of experimental and predicted axial pressure variation for semi-infinite metallic targets

Cited by 2 publications

References 8 publications

Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

Determination of flow field behind magnetogasdynamic spherical blast wave under the influence of viscosity

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