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Artykuły w czasopismach na temat „Shock”

Autor: Grafiati

Data publikacji: 4 czerwca 2021

Data aktualizacji: 25 lipca 2025

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1

Pope, M. H., and D. B. Melrose. "Diffusive Shock Acceleration by Multiple Shock Fronts with Differing Properties." Publications of the Astronomical Society of Australia 11, no. 2 (1994): 175–79. http://dx.doi.org/10.1017/s1323358000019858.

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AbstractThe effect of diffusive shock acceleration on a distribution of particles is explored for multiple shocks, taking into account adiabatic expansion between the shocks. Specifically, the spectral index is calculated numerically for two cases: a sequence of identical shocks, and a sequence of pairs of shocks with alternating shock strength. How these two cases evolve to the asymptotic limit is examined, and it is shown that the evolution of the paired-shock case can be described by a sequence of identical shocks with shock strength equal to the mean of the two.

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2

Kevlahan, N. K. R. "The propagation of weak shocks in non-uniform flows." Journal of Fluid Mechanics 327 (November 25, 1996): 161–97. http://dx.doi.org/10.1017/s0022112096008506.

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A new theory of the propagation of weak shocks into non-uniform, two-dimensional flows is introduced. The theory is based on a description of shock propagation in terms of a manifold equation together with compatibility conditions for shock strength and its normal derivatives behind the shock. This approach was developed by Ravindran & Prasad (1993) for shocks of arbitrary strength propagating into a medium at rest and is extended here to non-uniform media and restricted to moderately weak shocks. The theory is tested against known analytical solutions for cylindrical and plane shocks, and

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3

Garcia, S. L., N. L. Garcia, L. R. Oliveira, V. L. C. C. Rodrigues, and M. L. S. Mello. "Experimentally induced heat- and cold-shock tolerance in adult Panstrongylus megistus (Burmeister) (Hemiptera, Reduviidae)." Brazilian Journal of Biology 63, no. 3 (2003): 449–55. http://dx.doi.org/10.1590/s1519-69842003000300010.

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The survival rate of domestic male and female adult Panstrongylus megistus was studied after sequential heat and cold shocks in order to investigate shock tolerance compared to that previously reported for nymphs. Sequential shocks were such that a milder shock (0°C, 5°C, 35°C, or 40°C for 1 h) preceded a severe one (0°C or 40°C for 12 h), separated by intervals of 8, 18, 24, and 72 h at 28°C (control temperature). The preliminary thermal shock induced tolerance to the more severe one, although tolerance intensity depended on the initial shock temperature and the interval between treatments. D

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4

Wu, C. C., M. Dryer, and S. T. Wu. "Slow shock interactions in the heliosphere using an adaptive grid MHD model." Annales Geophysicae 23, no. 3 (2005): 1013–23. http://dx.doi.org/10.5194/angeo-23-1013-2005.

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Abstract. A one-dimensional (1-D), time-dependent, adaptive-grid MHD model with solar wind structure has been used in the past to study the interaction of shocks. In the present study, we wish to study some fundamental processes that may be associated with slow shock genesis and their possible interactions with other discontinuities. This adaptive-grid model, suitable for appropriate spatial and temporal numerical simulations, is used for this purpose because its finer grid sizes in the vicinity of the steep gradients at shocks make it possible to delineate the physical parameters on both side

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5

Shrestha, Bishwas L., David J. McComas, Eric J. Zirnstein, et al. "High-resolution Observations of Pickup-ion-mediated Shocks to 60 au." Astrophysical Journal 984, no. 1 (2025): 11. https://doi.org/10.3847/1538-4357/adc0a1.

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Abstract This study provides a detailed analysis of 14 distant interplanetary shocks observed by the Solar Wind Around Pluto instrument on board New Horizons. These shocks were observed with a pickup ion data cadence of approximately 30 minutes, covering a heliocentric distance range of ∼52–60 au. All the shocks observed within this distance range are fast forward shocks, and the shock compression ratios vary between ∼1.2 and 1.9. The shock transition scales are generally narrow, and the SW density compressions are more pronounced compared to the previous study of seven shocks by D. J. McComas

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6

Bai, Jianming, Yun Chen, Chun Yuan, and Xiaoling Yin. "Limit Theorems for Local Cumulative Shock Models with Cluster Shock Structure." Mathematical Problems in Engineering 2015 (2015): 1–10. http://dx.doi.org/10.1155/2015/828979.

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This paper considers a more general shock model with insurance and financial risk background, in which the system is subject to two types of shocks called primary shocks and secondary shocks. Each primary shock causes a series of secondary shocks according to some cluster pattern. In reliability applications, a primary shock can represent an issue of insurance policies of an insurer company, and the secondary shocks then denote the relevant insurance claims generated by the policy. We focus on the local cumulative shock process where only a certain number of the most recent primary and seconda

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7

Watari, S., and T. Detman. "In situ local shock speed and transit shock speed." Annales Geophysicae 16, no. 4 (1998): 370–75. http://dx.doi.org/10.1007/s00585-998-0370-9.

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Abstract. A useful index for estimating the transit speeds was derived by analyzing interplanetary shock observations. This index is the ratio of the in situ local shock speed and the transit speed; it is 0.6–0.9 for most observed shocks. The local shock speed and the transit speed calculated for the results of the magnetohydrodynamic simulation show good agreement with the observations. The relation expressed by the index is well explained by a simplified propagation model assuming a blast wave. For several shocks the ratio is approximately 1.2, implying that these shocks accelerated during p

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8

Hollenbach, David. "The Physics of Molecular Shocks in YSO Outflows." Symposium - International Astronomical Union 182 (1997): 181–98. http://dx.doi.org/10.1017/s0074180900061647.

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Shock waves light up the jets, winds and outflows around YSOs and diagnose the physical conditions and processes resident in these regions. This paper discusses the differences between the jet/wind shock and the ambient shock, between C shocks and J shocks, and between the shocks produced by pure jets and by collimated wide angle winds. Basic shock physics is briefly reviewed, with a special focus on the temperature structure in shocks and the Wardle instability of C shocks. Application is made to the origin of shocked H2 emission and to H2O masers.

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9

Cha, Ji Hwan, and Maxim Finkelstein. "On New Classes of Extreme Shock Models and Some Generalizations." Journal of Applied Probability 48, no. 1 (2011): 258–70. http://dx.doi.org/10.1239/jap/1300198148.

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In extreme shock models, only the impact of the current, possibly fatal shock is usually taken into account, whereas in cumulative shock models, the impact of the preceding shocks is accumulated as well. A shock model which combines these two types is called a ‘combined shock model’. In this paper we study new classes of extreme shock models and, based on the obtained results and model interpretations, we extend these results to several specific combined shock models. For systems subject to nonhomogeneous Poisson processes of shocks, we derive the corresponding survival probabilities and discu

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10

Cha, Ji Hwan, and Maxim Finkelstein. "On New Classes of Extreme Shock Models and Some Generalizations." Journal of Applied Probability 48, no. 01 (2011): 258–70. http://dx.doi.org/10.1017/s0021900200007750.

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In extreme shock models, only the impact of the current, possibly fatal shock is usually taken into account, whereas in cumulative shock models, the impact of the preceding shocks is accumulated as well. A shock model which combines these two types is called a ‘combined shock model’. In this paper we study new classes of extreme shock models and, based on the obtained results and model interpretations, we extend these results to several specific combined shock models. For systems subject to nonhomogeneous Poisson processes of shocks, we derive the corresponding survival probabilities and discu

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11

HORNUNG, H. G., and D. W. SCHWENDEMAN. "Oblique shock reflection from an axis of symmetry: shock dynamics and relation to the Guderley singularity." Journal of Fluid Mechanics 438 (July 5, 2001): 231–45. http://dx.doi.org/10.1017/s0022112001004360.

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Oblique shock reflection from an axis of symmetry is studied using Whitham's theory of geometrical shock dynamics, and the results are compared with previous numerical simulations of the phenomenon by Hornung (2000). The shock shapes (for strong and weak shocks), and the location of the shock-shock (for strong shocks), are in good agreement with the numerical results, though the detail of the shock reflection structure is, of course, not resolved by shock dynamics. A guess at a mathematical form of the shock shape based on an analogy with the Guderley singularity in cylindrical shock implosion

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12

Tsurutani, B. T., L. Shan, G. S. Lakhina, et al. "Comment on “Non-interacting coronal mass ejections and solar energetic particles near the quadrature configuration of solar terrestrial relations observatory”: CME shocks are fast magnetosonic shocks and not intermediate Alfvén shocks." Astronomy & Astrophysics 656 (December 2021): A152. http://dx.doi.org/10.1051/0004-6361/202141029.

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Aims. The expression for the shock Mach number used by Ravishankar and Michalek (2020, A&A, 638, A42) is incorrect. We wish to provide a correct expression so they can redo their analyses. Methods. Coronal mass ejection (CME) shocks are fast magnetosonic shocks and not intermediate Alfvén shocks. We give the steps for calculating the shock normal, shock velocity, and, thus, the shock Mach number. We also mention that the shock properties, such as being quasi-perpendicular or quasi-parallel, are another important parameter for the shock acceleration of energetic particles. Results. We have

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13

Maleckar, M. M., M. C. Woods, V. Y. Sidorov, et al. "Polarity reversal lowers activation time during diastolic field stimulation of the rabbit ventricles: insights into mechanisms." American Journal of Physiology-Heart and Circulatory Physiology 295, no. 4 (2008): H1626—H1633. http://dx.doi.org/10.1152/ajpheart.00706.2008.

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To fully characterize the mechanisms of defibrillation, it is necessary to understand the response, within the three-dimensional (3D) volume of the ventricles, to shocks given in diastole. Studies that have examined diastolic responses conducted measurements on the epicardium or on a transmural surface of the left ventricular (LV) wall only. The goal of this study was to use optical imaging experiments and 3D bidomain simulations, including a model of optical mapping, to ascertain the shock-induced virtual electrode and activation patterns throughout the rabbit ventricles following diastolic s

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14

Knisley, S. B., W. M. Smith, and R. E. Ideker. "Prolongation and shortening of action potentials by electrical shocks in frog ventricular muscle." American Journal of Physiology-Heart and Circulatory Physiology 266, no. 6 (1994): H2348—H2358. http://dx.doi.org/10.1152/ajpheart.1994.266.6.h2348.

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Effects of electrical shocks on myocardium are important for defibrillation. We measured effects of shocks (5 ms, 1–40 V/cm) in isolated frog ventricular strips. We recorded contraction strength and intracellular action potential (AP) with a shock-voltage cancellation technique to allow recordings immediately after shocks. Shocks of > or = 5 V/cm produced a dose- and latency-dependent prolongation of the AP ongoing during the shock. Stronger shocks of 28–40 V/cm decreased the duration, maximum diastolic potential, amplitude, and maximum rate of rise of the phase zero depolarization of paced

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15

Baek, Jungho, and Ji-Yong Seo. "A Study on Unobserved Structural Innovations of Oil Price: Evidence from Global Stock, Bond, Foreign Exchange, and Energy Markets." Review of Pacific Basin Financial Markets and Policies 18, no. 01 (2015): 1550004. http://dx.doi.org/10.1142/s0219091515500046.

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This study examines the effects of oil shocks by their respective causes and of volatility spillover including leverage effects. Previous studies did not analyze oil factor by categorizing it into three components (supply shock, demand shock, and market shock) as determinants of rate of return in stock markets, a key issue in finance. Results show that oil shocks determine returns in the global stock market, bond market, foreign exchange market, and energy market, and that their effects vary by types of markets, levels of oil prices, and types of oil shocks. Second, the leverage effect of oil

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16

Spiteri, Shaun. "Shock Absorber Applications." European Journal of Engineering Research and Science 4, no. 1 (2019): 37–41. http://dx.doi.org/10.24018/ejers.2019.4.1.1005.

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Shock Absorbers are a part of everyday life and have many different applications and uses. They are used for bridges, highways, buildings and cars to absorb the impact from the bumps, earthquakes and high winds. Different applications require different types of shocks and different materials. A rubber shock absorber cannot be used on a vehicle while a cylindrical shock absorber cannot be used on a highway. All the situations require a specific shape and type of shocks to be used for the required tasks.

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17

Spiteri, Shaun. "Shock Absorber Applications." European Journal of Engineering and Technology Research 4, no. 1 (2019): 37–41. http://dx.doi.org/10.24018/ejeng.2019.4.1.1005.

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Shock Absorbers are a part of everyday life and have many different applications and uses. They are used for bridges, highways, buildings and cars to absorb the impact from the bumps, earthquakes and high winds. Different applications require different types of shocks and different materials. A rubber shock absorber cannot be used on a vehicle while a cylindrical shock absorber cannot be used on a highway. All the situations require a specific shape and type of shocks to be used for the required tasks.

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18

Zhang, Congyao, Eugene Churazov, William R. Forman, and Natalia Lyskova. "Runaway merger shocks in galaxy cluster outskirts and radio relics." Monthly Notices of the Royal Astronomical Society 488, no. 4 (2019): 5259–66. http://dx.doi.org/10.1093/mnras/stz2135.

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ABSTRACT Moderately strong shocks arise naturally when two subclusters merge. For instance, when a smaller subcluster falls into the gravitational potential of a more massive cluster, a bow shock is formed and moves together with the subcluster. After pericentre passage, however, the subcluster is decelerated by the gravity of the main cluster, while the shock continues moving away from the cluster centre. These shocks are considered as promising candidates for powering radio relics found in many clusters. The aim of this paper is to explore the fate of such shocks when they travel to the clus

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19

James, T. A., S. Viti, J. Holdship, and I. Jiménez-Serra. "Tracing shock type with chemical diagnostics." Astronomy & Astrophysics 634 (January 29, 2020): A17. http://dx.doi.org/10.1051/0004-6361/201936536.

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Aims. The physical structure of a shock wave may take a form unique to its shock type, implying that the chemistry of each shock type is unique as well. We aim to investigate the different chemistries of J-type and C-type shocks in order to identify unique molecular tracers of both shock types. We apply these diagnostics to the protostellar outflow L1157 to establish whether the B2 clump could host shocks exhibiting type-specific behaviour. Of particular interest is the L1157-B2 clump, which has been shown to exhibit bright emission in S-bearing species and HNCO. Methods. We simulate, using a

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20

Xu, Y. F., S. C. Hu, Y. Cai, and S. N. Luo. "Origins of plastic shock waves in single-crystal Cu." Journal of Applied Physics 131, no. 11 (2022): 115901. http://dx.doi.org/10.1063/5.0080757.

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We investigate shock wave propagation in single-crystal Cu with large-scale molecular dynamics simulations. Plastic shock waves propagate via dislocation nucleation or growth. With decreasing particle velocity, a remarkable drop in plastic shock wave velocity relative to the linear shock velocity–particle velocity relation is observed in the elastic–plastic two-wave regime for different loading directions. This reduction can be attributed to the changes in the mechanisms of plastic shock wave generation/propagation, from the dislocation nucleation-dominant mode, to the alternating nucleation a

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21

Wu, X. F., Z. G. Dai, Y. F. Huang, and T. Lu. "Optical Flash and Radio Flare in Wind Environment." Symposium - International Astronomical Union 214 (2003): 343–44. http://dx.doi.org/10.1017/s0074180900194720.

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The interaction of a relativistic fireball with its ambient medium is described through two shocks: a reverse shock that propagates into the fireball, and a forward shock that propagates into the medium. We here study very early afterglows from the reverse and forward shocks in winds. An optical flash arises from both the relativistic reverse and forward shock while a radio flare is produced by the forward shock.

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22

GOODMAN, JEREMY, and ANDREW MACFADYEN. "Ultra-relativistic geometrical shock dynamics and vorticity." Journal of Fluid Mechanics 604 (May 14, 2008): 325–38. http://dx.doi.org/10.1017/s0022112008001249.

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Geometrical shock dynamics, also called CCW theory, yields approximate equations for shock propagation in which only the conditions at the shock appear explicitly; the post-shock flow is presumed approximately uniform and enters implicitly via a Riemann invariant. The non-relativistic theory, formulated by G. B. Whitham and others, matches many experimental results surprisingly well. Motivated by astrophysical applications, we adapt the theory to ultra-relativistic shocks advancing into an ideal fluid whose pressure is negligible ahead of the shock, but is one third of its proper energy densit

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23

Vimercati, Davide, Giulio Gori, and Alberto Guardone. "Non-ideal oblique shock waves." Journal of Fluid Mechanics 847 (May 21, 2018): 266–85. http://dx.doi.org/10.1017/jfm.2018.328.

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From the analysis of the isentropic limit of weak compression shock waves, oblique shock waves in which the post-shock Mach number is larger than the pre-shock Mach number, named non-ideal oblique shocks, are admissible in substances characterized by moderate molecular complexity and in the close proximity to the liquid–vapour saturation curve. Non-ideal oblique shocks of finite amplitude are systematically analysed, clarifying the roles of the pre-shock thermodynamic state and Mach number. The necessary conditions for the occurrence of non-ideal oblique shocks of finite amplitude are singled

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24

Huete, C., J. G. Wouchuk, B. Canaud, and A. L. Velikovich. "Analytical linear theory for the shock and re-shock of isotropic density inhomogeneities." Journal of Fluid Mechanics 700 (April 30, 2012): 214–45. http://dx.doi.org/10.1017/jfm.2012.126.

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AbstractWe present an analytical model that describes the linear interaction of two successive shocks launched into a non-uniform density field. The re-shock problem is important in different fields, inertial confinement fusion among them, where several shocks are needed to compress the non-uniform target. At first, we present a linear theory model that studies the interaction of two successive shocks with a single-mode density perturbation field ahead of the first shock. The second shock is launched after the sonic waves emitted by the first shock wave have vanished. Therefore, in the case co

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25

KEVLAHAN, N. K. R. "The vorticity jump across a shock in a non-uniform flow." Journal of Fluid Mechanics 341 (June 25, 1997): 371–84. http://dx.doi.org/10.1017/s0022112097005752.

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The vorticity jump across an unsteady curved shock propagating into a two-dimensional non-uniform flow is considered in detail. The exact general expression for the vorticity jump across a shock is derived from the gasdynamics equations. This general expression is then simplified by writing it entirely in terms of the Mach number of the shock MS and the local Mach number of the flow ahead of the shock MU.The vorticity jump is very large at places where the curvature of the shock is very large, even in the case of weak shocks. Vortex sheets form behind shock-shocks (associated with kinks in the

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26

Trotta, Domenico, Andrew Dimmock, Heli Hietala, et al. "An Overview of Solar Orbiter Observations of Interplanetary Shocks in Solar Cycle 25." Astrophysical Journal Supplement Series 277, no. 1 (2025): 2. https://doi.org/10.3847/1538-4365/ada4a7.

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Abstract Interplanetary (IP) shocks are fundamental constituents of the heliosphere, where they form as a result of solar activity. We use previously unavailable measurements of IP shocks in the inner heliosphere provided by Solar Orbiter, and present a survey of the first 100 shocks observed in situ at different heliocentric distances during the rising phase of solar cycle 25. The fundamental shock parameters (shock normals, shock normal angles, shock speeds, compression ratios, Mach numbers) have been estimated and studied as a function of heliocentric distance, revealing a rich scenario of

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27

SCHWENDEMAN, DONALD W. "On converging shock waves of spherical and polyhedral form." Journal of Fluid Mechanics 454 (March 10, 2002): 365–86. http://dx.doi.org/10.1017/s0022112001007170.

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The behaviour of converging spherical shock waves is considered using Whitham's theory of geometrical shock dynamics. An analysis of converging shocks whose initial shape takes the form of regular polyhedra is presented. The analysis of this problem is motivated by the earlier work on converging cylindrical shocks discussed in Schwendeman & Whitham (1987). In that paper, exact solutions were reported for converging polygonal shocks in which the initial shape re-forms repeatedly as the shock contracts. For the polyhedral case, the analysis is performed both analytically and numerically for

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28

Sow Mondal, Shanwlee, Aveek Sarkar, Bhargav Vaidya, and Andrea Mignone. "Acceleration of Solar Energetic Particles by the Shock of Interplanetary Coronal Mass Ejection." Astrophysical Journal 923, no. 1 (2021): 80. http://dx.doi.org/10.3847/1538-4357/ac2c7a.

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Abstract Interplanetary coronal mass ejection (ICME) shocks are known to accelerate particles and contribute significantly to solar energetic particle events. We have performed magnetohydrodynamic-particle in cell simulations of ICME shocks to understand the acceleration mechanism. These shocks vary in Alfvénic Mach numbers as well as in magnetic field orientations (parallel and quasi-perpendicular). We find that diffusive shock acceleration plays a significant role in accelerating particles in a parallel ICME shock. In contrast, shock drift acceleration (SDA) plays a pivotal role in a quasi-p

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29

Shrestha, Bishwas L., Eric J. Zirnstein, David J. McComas, et al. "Suprathermal H⁺ Pickup Ion Tails in the Outer Heliosphere." Astrophysical Journal 960, no. 1 (2023): 35. http://dx.doi.org/10.3847/1538-4357/ad08b9.

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Abstract This study provides a detailed analysis of five distant interplanetary shocks observed by the Solar Wind Around Pluto instrument on board New Horizons, which exhibit the signature of a suprathermal H+ pickup ion (PUI) tail in the downstream distribution. These shocks were observed with a PUI data cadence of approximately 24 hr, covering a heliocentric distance range of 23.71–36.75 au. The shock compression ratio varies between approximately 1.4 and 3.2. The H+ PUI density and temperature show a gradual increase across the shock, while the H+ solar wind density shows erratic behavior w

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30

Wu, C. C., S. T. Wu, and M. Dryer. "Generation and evolution of interplanetary slow shocks." Annales Geophysicae 14, no. 4 (1996): 375–82. http://dx.doi.org/10.1007/s00585-996-0375-1.

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Abstract. It is well known that most MHD shocks observed within 1 AU are MHD fast shocks. Only a very limited number of MHD slow shocks are observed within 1 AU. In order to understand why there are only a few MHD slow shocks observed within 1 AU, we use a one-dimensional, time-dependent MHD code with an adaptive grid to study the generation and evolution of interplanetary slow shocks (ISS) in the solar wind. Results show that a negative, nearly square-wave perturbation will generate a pair of slow shocks (a forward and a reverse slow shock). In addition, the forward and the reverse slow shock

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31

Ruggeri, Tommaso, and Shigeru Taniguchi. "A complete classification of sub-shocks in the shock structure of a binary mixture of Eulerian gases with different degrees of freedom." Physics of Fluids 34, no. 6 (2022): 066116. http://dx.doi.org/10.1063/5.0094835.

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The shock structure in a binary mixture of polyatomic Eulerian gases with different degrees of freedom of a molecule is studied based on the multi-temperature model of rational extended thermodynamics. Since the system of field equations is hyperbolic, the shock-structure solution is not always regular, and discontinuous parts (sub-shocks) can be formed. For given values of the mass ratio and the specific heat of the constituents, we identify the possible sub-shocks as the Mach number M0 of the shock wave and the equilibrium concentration c0 of the constituents change. In the plane ( c0, M0),

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32

Bulat, Pavel, Konstantin Volkov, and Igor Volobuev. "Interaction between Shock Waves Travelling in the Same Direction." Fluids 6, no. 9 (2021): 315. http://dx.doi.org/10.3390/fluids6090315.

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In this paper, we study the intersection (interaction) between several steady shocks traveling in the same direction. The interaction between overtaking shocks may be regular or irregular. In the case of regular reflection, the intersection of overtaking shocks leads to the formation of a resulting shock, contact discontinuity, and some reflected discontinuities. The type of discontinuity depends on the parameters of incoming shocks. At the irregular reflection, a Mach shock forms between incoming overtaking shocks. Reflected discontinuities come from the points of intersection of the Mach ste

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33

de Voil, Cedric. "Snack Shack or Snack Shock?" Nutrition and Health 16, no. 3 (2002): 249–50. http://dx.doi.org/10.1177/026010600201600310.

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Snow, B., and A. Hillier. "Intermediate shock sub-structures within a slow-mode shock occurring in partially ionised plasma." Astronomy & Astrophysics 626 (June 2019): A46. http://dx.doi.org/10.1051/0004-6361/201935326.

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Context. Slow-mode shocks are important in understanding fast magnetic reconnection, jet formation and heating in the solar atmosphere, and other astrophysical systems. The atmospheric conditions in the solar chromosphere allow both ionised and neutral particles to exist and interact. Under such conditions, fine sub-structures exist within slow-mode shocks due to the decoupling and recoupling of the plasma and neutral species. Aims. We study numerically the fine sub-structure within slow-mode shocks in a partially ionised plasma, in particular, analysing the formation of an intermediate transi

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35

Rahn, Daniela, and Enzo Weber. "PATTERNS OF UNEMPLOYMENT DYNAMICS IN GERMANY." Macroeconomic Dynamics 23, no. 1 (2017): 322–57. http://dx.doi.org/10.1017/s1365100516001358.

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Using a structural vector autoregressive (SVAR) model, this paper provides deeper insight into unemployment dynamics in Germany. We identify a technology shock and two policy shocks that play a central role in business cycle research. Accordingly, we enrich the discussion on the sources of unemployment dynamics by considering demand-side impulses. The worker reallocation process varies substantially with the identified shocks. The job-finding rate plays a larger role after a technology shock and a monetary policy shock, whereas the separation rate appears to be the dominant margin after a fisc

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MITROVIĆ, DARKO, and MARKO NEDELJKOV. "DELTA SHOCK WAVES AS A LIMIT OF SHOCK WAVES." Journal of Hyperbolic Differential Equations 04, no. 04 (2007): 629–53. http://dx.doi.org/10.1142/s021989160700129x.

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We discus the existence of delta shock waves obtained as a limit of two shock waves. For that purpose we perturb a prototype of weakly hyperbolic 2 × 2 system (sometimes called the "generalized pressureless gas dynamics model") by an additional term (called the "generalized vanishing pressure"). The obtained perturbed system is strictly hyperbolic and its Riemann problem is solvable. Since it is genuinely nonlinear, its solution consists of shocks and rarefaction waves combination. As perturbation parameter vanishes, the solution converges in the space of distribution. Specially, a solution co

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AL-Taee, Anwaar F., and Jamella H. Rasheed. "Expression of Heat Shock Protein HSP90 in Genomic-DNA of Chickpea (Cicer arietinum L.) Callus by Heat Shock Treatment." Academic Journal of Research and Scientific Publishing 3, no. 33 (2022): 121–39. http://dx.doi.org/10.52132/ajrsp.e.2022.33.6.

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This study was able to detect of the expression activity of heat shock proteins HSP90 and heat transcription factors HSFs for the first time in callus cultures of chickpea, Cicer arietinum L., that exposed to abiotic shocks, grown on MS medium supplemented with 1.0 mg L-1 naphthalene acetic acid (NAA) and 2.0 mg L-1 benzyl adenine (BA). Heat shock proteins HSPs were constructed for increase of withstand long-term physical shocks, and production of resistant to heat chickpeas plants, this shock was enhancement of tolerance of chickpea callus to abiotic stresses (high - temperatures). Results en

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Bret, Antoine, and Asaf Pe’er. "On the Width of a Collisionless Shock and the Index of the Cosmic Rays It Accelerates." Astrophysical Journal 968, no. 2 (2024): 100. http://dx.doi.org/10.3847/1538-4357/ad4bde.

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Abstract Despite being studied for many years, the structure of collisionless shocks is still not fully determined. Such shocks are known to be accelerators of cosmic rays (CRs), which, in turn, modify the shock structure. The shock width λ is known to be connected to the CR spectral index a. Here, we use an instability analysis to derive the shock width in the presence of CRs. We obtain an analytical expression connecting the shock width to the CR index and to the fraction of upstream particles that are accelerated. We find that when this fraction becomes larger than ∼30%, a new instability b

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Zhang, Congyao, Eugene Churazov, Klaus Dolag, William R. Forman, and Irina Zhuravleva. "Encounters of merger and accretion shocks in galaxy clusters and their effects on intracluster medium." Monthly Notices of the Royal Astronomical Society 494, no. 3 (2020): 4539–47. http://dx.doi.org/10.1093/mnras/staa1013.

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ABSTRACT Several types/classes of shocks naturally arise during formation and evolution of galaxy clusters. One such class is represented by accretion shocks, associated with deceleration of infalling baryons. Such shocks, characterized by a very high Mach number, are present even in 1D models of cluster evolution. Another class is composed of ‘runaway merger shocks’, which appear when a merger shock, driven by a sufficiently massive infalling subcluster, propagates away from the main-cluster centre. We argue that, when the merger shock overtakes the accretion shock, a new long-living shock is

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Cha, Ji Hwan, and Maxim Finkelstein. "On a Terminating Shock Process with Independent Wear Increments." Journal of Applied Probability 46, no. 2 (2009): 353–62. http://dx.doi.org/10.1239/jap/1245676092.

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In extreme shock models, only the impact of the current, possibly fatal shock is usually taken into account, whereas in cumulative shock models, the impact of the preceding shocks is accumulated as well. In this paper we combine an extreme shock model with a specific cumulative shock model. It is shown that the proposed setting can also be interpreted as a generalization of the well-known Brown–Proschan model that describes repair actions for repairable systems. For a system subject to a specific process of shocks, we derive the survival probability and the corresponding failure rate function.

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Cha, Ji Hwan, and Maxim Finkelstein. "On a Terminating Shock Process with Independent Wear Increments." Journal of Applied Probability 46, no. 02 (2009): 353–62. http://dx.doi.org/10.1017/s0021900200005507.

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In extreme shock models, only the impact of the current, possibly fatal shock is usually taken into account, whereas in cumulative shock models, the impact of the preceding shocks is accumulated as well. In this paper we combine an extreme shock model with a specific cumulative shock model. It is shown that the proposed setting can also be interpreted as a generalization of the well-known Brown–Proschan model that describes repair actions for repairable systems. For a system subject to a specific process of shocks, we derive the survival probability and the corresponding failure rate function.

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Gedalin, M., and E. Griv. "Collisionless electrons in a thin high Mach number shock: dependence on angle and <font face="Symbol" ><b><i>b</i></b></font>." Annales Geophysicae 17, no. 10 (1999): 1251–59. http://dx.doi.org/10.1007/s00585-999-1251-6.

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Abstract. It is widely believed that electron dynamics in the shock front is essentially collisionless and determined by the quasistationary magnetic and electric fields in the shock. In thick shocks the electron motion is adiabatic: the magnetic moment is conserved throughout the shock and v2^ ∝ B. In very thin shocks with large cross-shock potential (the last feature is typical for shocks with strong electron heating), electrons may become demagnetized (the magnetic moment is no longer conserved) and their motion may become nonadiabatic. We consider the case of substantial demagnetization in

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Chakrabarti, Sandip K. "A Systematic Study of the Standing Shocks in Astrophysical Flows near a Compact Object." Publications of the Astronomical Society of Japan 41, no. 6 (1990): 1145–72. https://doi.org/10.1093/pasj/41.6.1145.

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Abstract We have systematically studied both standing dissipative and non-dissipative shocks and isentropic compression waves in thin, rotating, adiabatic astrophysical flows, such as the accretion or winds near black holes and neutron stars. The flow is assumed to be in transverse equilibrium and the dissipation is allowed only at the shocks. We classify the whole parameter space spanned by the accretion rate (M˙), the energy (E), and the angular momentum (λ) according to whether a shock solution can exist or not. Apart from conserving the baryon flux and the net momentum flux, flows at these

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Wang, Liyao, Li Yang, and Lianjie Yue. "Study on the influence of expansion waves on the reflection type of shock wave in double-wedge configurations." Journal of Physics: Conference Series 2882, no. 1 (2024): 012025. http://dx.doi.org/10.1088/1742-6596/2882/1/012025.

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Abstract This paper investigates how variations in the relative positioning between the expansion fan emitted from the triple point in the shock/shock interference on double-wedge geometries in confined spaces and the incidence point of oblique shocks influence the transition of oblique shock reflection types, and understands the roles of expansion waves in inhibiting MR. Predictive analysis through the shock polar line provides critical values for the transition of oblique shock reflection types under the influence of expansion fan effects. The position where the shock/expansion fan undergoes

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Lee, Kiseok, Wensheng Kang, and Ronald A. Ratti. "OIL PRICE SHOCKS, FIRM UNCERTAINTY, AND INVESTMENT." Macroeconomic Dynamics 15, S3 (2011): 416–36. http://dx.doi.org/10.1017/s1365100511000496.

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This paper seeks to answer the following questions: Do oil price shocks affect firms' investment decisions? Do oil price shocks affect investment decisions differentially depending on firm-specific uncertainty? Over what time horizon do oil price shocks affect high-uncertainty firms? Is the intensity of the oil price shock important, or just its existence? It is found that oil price shocks depress firms' investment decisions, and do so differentially by depressing investment more for more uncertain firms. Oil shocks affect investment for at least the first and second year after the shock. In t

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Melrose, D. B., and M. H. Pope. "Diffusive Shock Acceleration by Multiple Shocks." Publications of the Astronomical Society of Australia 10, no. 3 (1993): 222–24. http://dx.doi.org/10.1017/s1323358000025716.

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AbstractDiffusive shock acceleration produces a power law momentum distribution f(p)α p−b, with b ≥ 4 for a single shock, and b = 4 for a single strong shock. It has been shown that the distribution for acceleration at a sequence of identical shocks is flatter, approaching f(p)α p−3 below a high energy knee, for an arbitrarily large number of shocks. We show how this flatter distribution arises and discuss the range of momenta over which it extends after a finite number of shocks.

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Ocker, Stella Koch, and Maren Cosens. "Probing the Low-velocity Regime of Nonradiative Shocks with Neutron Star Bow Shocks." Astrophysical Journal Letters 975, no. 2 (2024): L31. http://dx.doi.org/10.3847/2041-8213/ad87cf.

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Abstract Nonradiative shocks accelerate particles and heat astrophysical plasmas. While supernova remnants are the most well-studied example, neutron star (NS) bow shocks are also nonradiative and Balmer dominated. NS bow shocks are likely ubiquitous in the interstellar medium due to their large speeds imparted at birth, and they are thought to be a discrete source population contributing to the Galactic cosmic-ray spectrum. To date, nine NS bow shocks have been directly observed in Hα images. Most of these shocks have been characterized using narrowband Hα imaging and slit spectroscopy, which

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Zhang, Congyao, Eugene Churazov, and Irina Zhuravleva. "Pairs of giant shock waves (N-waves) in merging galaxy clusters." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 1038–45. http://dx.doi.org/10.1093/mnras/staa3718.

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ABSTRACT When a subcluster merges with a larger galaxy cluster, a bow shock is driven ahead of the subcluster. At a later merger stage, this bow shock separates from the subcluster, becoming a ‘runaway’ shock that propagates down the steep density gradient through the cluster outskirts and approximately maintains its strength and the Mach number. Such shocks are plausible candidates for producing radio relics in the periphery of clusters. We argue that, during the same merger stage, a secondary shock is formed much closer to the main cluster centre. A close analogue of this structure is known

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Vieu, T., S. Gabici, and V. Tatischeff. "Non-linear particle reacceleration by multiple shocks." Monthly Notices of the Royal Astronomical Society 510, no. 2 (2021): 2529–37. http://dx.doi.org/10.1093/mnras/stab3564.

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ABSTRACT When the pressure of particles accelerated at shock waves is no longer negligible compared to the kinetic pressure of the gas, the linear theory of diffusive shock acceleration breaks down. This is expected in particular when the shock sweeps up pre-existing cosmic rays, or when multiple shocks reaccelerate successively the same particles. To describe these systems, one has to account for the non-linear backreaction of the particles on the magnetohydrodynamic flow. Using an up-to-date semi-analytical model of particle reacceleration at non-linear shocks, we show that the presence of p

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Kruparova, Oksana, Adam Szabo, Lan K. Jian, et al. "Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe." Astrophysical Journal Letters 979, no. 1 (2025): L10. https://doi.org/10.3847/2041-8213/ada558.

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Abstract We present a comprehensive analysis of 66 interplanetary shocks observed by the Parker Solar Probe between 2018 November and 2024 January. Among these, 33 events fulfilled the Rankine–Hugoniot (R-H) conditions, ensuring reliable asymptotic plasma parameter solutions. The remaining 33 events could not be confirmed by the standard R-H approach—potentially including wave-like structures—yet were analyzed via averaging and mixed-data methods to obtain robust shock parameters. Utilizing our ShOck Detection Algorithm database, the shocks are categorized into fast-forward, fast-reverse, slow

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