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Journal articles on the topic 'Instabilities'

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Author: Grafiati

Published: 4 June 2021

Last updated: 31 August 2024

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1

Cruz, Akaxia, and Matthew McQuinn. "Astrophysical plasma instabilities induced by long-range interacting dark matter." Journal of Cosmology and Astroparticle Physics 2023, no. 04 (April 1, 2023): 028. http://dx.doi.org/10.1088/1475-7516/2023/04/028.

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Abstract If dark matter is millicharged or darkly charged, collective plasma processes may dominate momentum exchange over direct particle collisions. In particular, plasma streaming instabilities can couple the momentum of the dark matter to counter-streaming baryons or other dark matter and result in the counter-streaming fluids coming to rest with each other, just as happens for baryonic collisionless shocks in astrophysical systems. While electrostatic plasma instabilites (such as the two-stream) are highly suppressed by Landau damping when dark matter is millicharged, in the cosmological situations of interest, electromagnetic instabilities such as the Weibel can couple the momenta, assuming that the linear instability saturates in the manner typically found for baryonic plasmas. We find that the streaming of dark matter in the pre-Recombination universe is affected more strongly by direct collisions than collective processes, validating previous constraints. However, when considering unmagnetized instabilities the properties of the Bullet Cluster merger and other merging cluster systems (which show dark matter streaming through itself) are likely to be substantially altered if [qχ /mχ ] ≳ 10-4, where [qχ /mχ ] is the charge-to-mass ratio of the dark matter relative to that of the proton. When a magnetic field is added consistent with cluster observations, the Weibel and Firehose instabilities result in sufficiently fast growth to reach saturation for [qχ /mχ ] ≳ 10-12–10-11. The Weibel growth rates are even faster in the case of a dark-U(1) charge (because “hot” electrons do not damp the instability), potentially ruling out [qχ /mχ ] ≳ 10-14 in the Bullet Cluster system, in agreement with [1]. The strongest previous limits on millicharged dark matter (mDM) arise from considering the spin-down of galactic disks [2]. We show that plasma instabilities or tangled background magnetic fields could lead to diffusive propagation of the dark matter, weakening these spin-down limits. Thus, plasma instabilities may place some of the most stringent constraints over much of the millicharged, and our results corroborate previous extremely stringent potential constraints on the dark-charged parameter space.

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2

Pier, John. "Narrative instabilities." Frontiers of Narrative Studies 6, no. 2 (January 12, 2020): 148–56. http://dx.doi.org/10.1515/fns-2020-0011.

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Abstract Taking Nabokov’s Pale Fire as its tutor text, this chapter seeks to demonstrate that narrative functions as a complex or dynamic system. Due to the novel’s nonlinear and multiply configured format, a series of dissipative structures is provoked whereby states near equilibrium, on reaching states far from equilibrium under the weight of multiple causality, putting the system “beyond the threshold of stability” and “at the edge of chaos,” perpetually self-organize. Taking a cue from nonequilibrium thermodynamics, instabilities, it is argued, are inherent to narrative discourse. This calls into question the pertinence of the logic of linearity (“event A causes event B”) as well as the scope of such postulates as the isomorphic relation between sequence and narrative as a whole, a postulate that frames narrative as a closed system following the principle of conservation of energy in classical mechanics. As the poem “Pale Fire” in Nabokov’s novel advances linearly, it is constantly disrupted by the “Commentary” which is related to the poem only tangentially, each text fragmenting the other and self-organizing into new meanings. The effect is to render salient in narrative discourse the complexity science principles (in addition to those mentioned above) of irreversibility (the “arrow of time”) vs. reversibility, sensitivity to initial conditions, negative vs. positive feedback and the symmetry-breaking effects of bifurcation. The manifestation of these principles in Nabokov’s novel raises fundamental questions about the structuring of narrative, but also about the conceptual framework through which narrative at large might be approached.

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3

Mikhailov, Anatolii L., Nikolai V. Nevmerzhitskii, and Viktor A. Raevskii. "Hydrodynamic instabilities." Physics-Uspekhi 54, no. 4 (April 30, 2011): 392–97. http://dx.doi.org/10.3367/ufne.0181.201104i.0410.

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4

Heavens, O. S. "Optical Instabilities." Optica Acta: International Journal of Optics 33, no. 9 (September 1986): 1095. http://dx.doi.org/10.1080/716099711.

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5

Soderholm, Sidney Case. "Aerosol Instabilities." Applied Industrial Hygiene 3, no. 2 (February 1988): 35–40. http://dx.doi.org/10.1080/08828032.1988.10388506.

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6

Mikhailov, Anatolii L., Nikolai V. Nevmerzhitskii, and Viktor A. Raevskii. "Hydrodynamic instabilities." Uspekhi Fizicheskih Nauk 181, no. 4 (2011): 410. http://dx.doi.org/10.3367/ufnr.0181.201104i.0410.

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7

Scharfman, Barry E., and Alexandra H. Techet. "Bag instabilities." Physics of Fluids 24, no. 9 (September 2012): 091112. http://dx.doi.org/10.1063/1.4748933.

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8

Aukrust, T., and E. H. Hauge. "Wetting instabilities." Physical Review A 36, no. 8 (October 1, 1987): 4097–98. http://dx.doi.org/10.1103/physreva.36.4097.

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9

Furman, A. S. "Photovoltaic instabilities." Ferroelectrics 83, no. 1 (January 1988): 41–53. http://dx.doi.org/10.1080/00150198808235448.

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10

Einaudi, G. "CORONAL INSTABILITIES." Highlights of Astronomy 8 (1989): 529–33. http://dx.doi.org/10.1017/s1539299600008236.

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AbstractThe interest in the stability of coronal structures derives from their observed lifetime (much longer than the relevant hydromagnetic timescale) coupled with their active behavior. This fact implies that these structures must be globally stable with respect to fast and destructive instabilities and, at the same time, must allow some local, non-disrupting, dissipative process to take place. In highly magnetized media as solar and stellar coronae a large number of plasma instabilities can occur. The present review will concentrate on those governed by the magnetohydrodynamic (MHD) equations with the inclusion of the effects of finite resistivity and viscosity and the use of an energy equation where radiation, mechanical heating and thermal conduction are considered.

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11

Malkin, A. Ya. "Surface instabilities." Colloid Journal 70, no. 6 (November 28, 2008): 673–89. http://dx.doi.org/10.1134/s1061933x0806001x.

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12

Young, Gerald W., and Stephen H. Davis. "Rivulet instabilities." Journal of Fluid Mechanics 176, no. -1 (March 1987): 1. http://dx.doi.org/10.1017/s0022112087000557.

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13

Hanna, D. C. "Optical instabilities." Optics & Laser Technology 18, no. 5 (October 1986): 274–75. http://dx.doi.org/10.1016/0030-3992(86)90095-2.

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14

Davis, S. H. "Thermocapillary Instabilities." Annual Review of Fluid Mechanics 19, no. 1 (January 1987): 403–35. http://dx.doi.org/10.1146/annurev.fl.19.010187.002155.

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15

Dey, Subhasish, and Sk Zeeshan Ali. "Fluvial instabilities." Physics of Fluids 32, no. 6 (June 1, 2020): 061301. http://dx.doi.org/10.1063/5.0010038.

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16

Lebovitz, Norman R., and Ellen Zweibel. "Magnetoelliptic Instabilities." Astrophysical Journal 609, no. 1 (July 2004): 301–12. http://dx.doi.org/10.1086/420972.

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17

Falle, S. A. E. G. "Shock instabilities." Astrophysics and Space Science 233, no. 1-2 (November 1995): 239–49. http://dx.doi.org/10.1007/bf00627355.

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18

Angeletti, Thomas, Juliette Galonnier, and Manon Him-Aquilli. "Semantic instabilities." Tracés, no. 43 (December 30, 2022): 7–32. http://dx.doi.org/10.4000/traces.14131.

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19

Trig, C. "Instabilities in theoretical chemistry. II. Mixing of different instabilities." Journal of Polymer Science Part C: Polymer Symposia 29, no. 1 (March 7, 2007): 119–32. http://dx.doi.org/10.1002/polc.5070290115.

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20

Viet Hoa, Le, Nguyen Tuan Anh, Nguyen Chinh Cuong, and Dang Thi Minh Hue. "HYDRODYNAMIC INSTABILITIES OF TWO-COMPONENT BOSE-EINSTEIN CONDENSATES." Journal of Science, Natural Science 60, no. 7 (2015): 121–28. http://dx.doi.org/10.18173/2354-1059.2015-0041.

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21

Reshetnyak, M. Yu. "Instabilities in dynamos." Doklady Physics 55, no. 8 (August 2010): 394–98. http://dx.doi.org/10.1134/s1028335810080070.

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22

Bonch-Bruevich, V. L. "Instabilities in Semiconductors." Physica Scripta T19B (January 1, 1987): 491–97. http://dx.doi.org/10.1088/0031-8949/1987/t19b/028.

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23

Osborne, Ian S. "Taming laser instabilities." Science 361, no. 6408 (September 20, 2018): 1211.5–1212. http://dx.doi.org/10.1126/science.361.6408.1211-e.

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24

Inan, Umran S. "Waves and instabilities." Reviews of Geophysics 25, no. 3 (1987): 588. http://dx.doi.org/10.1029/rg025i003p00588.

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25

Rajvaidya, P., and K. C. Almeroth. "Multicast routing instabilities." IEEE Internet Computing 8, no. 5 (September 2004): 42–49. http://dx.doi.org/10.1109/mic.2004.48.

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26

Alderton, Gemma. "Dissecting the instabilities." Nature Reviews Cancer 7, no. 3 (March 2007): 159. http://dx.doi.org/10.1038/nrc2095.

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27

Tang, W. M., F. Romanelli, and S. Briguglio. "Resistive electrostatic instabilities." Physics of Fluids 31, no. 10 (1988): 2951. http://dx.doi.org/10.1063/1.866952.

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28

Keskar, Nitin R., James R. Chelikowsky, and Renata M. Wentzcovitch. "Mechanical instabilities inAlPO4." Physical Review B 50, no. 13 (October 1, 1994): 9072–78. http://dx.doi.org/10.1103/physrevb.50.9072.

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29

Mathoulin, C., Ph Saffar, and S. Roukoz. "Luno-triquetral instabilities." Annales de Chirurgie de la Main et du Membre Supérieur 9, no. 2 (January 1990): 146. http://dx.doi.org/10.1016/s0753-9053(05)80494-6.

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30

HALLER, MERRICK C., and R. A. DALRYMPLE. "Rip current instabilities." Journal of Fluid Mechanics 433 (April 25, 2001): 161–92. http://dx.doi.org/10.1017/s0022112000003414.

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A laboratory experiment involving rip currents generated on a barred beach with periodic rip channels indicates that rip currents contain energetic low-frequency oscillations in the presence of steady wave forcing. An analytic model for the time-averaged flow in a rip current is presented and its linear stability characteristics are investigated to evaluate whether the rip current oscillations can be explained by a jet instability mechanism. The instability model considers spatially growing disturbances in an offshore directed, shallow water jet. The effects of variable cross-shore bathymetry, non-parallel flow, turbulent mixing, and bottom friction are included in the model. Model results show that rip currents are highly unstable and the linear stability model can predict the scales of the observed unsteady motions.

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31

ZEBIB, ABDELFATTAH. "Vibrational thermocapillary instabilities." Journal of Fluid Mechanics 540, no. -1 (September 27, 2005): 353. http://dx.doi.org/10.1017/s0022112005006014.

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32

Bloch, A. M., P. S. Krishnaprasad, J. E. Marsden, and T. S. Ratiu. "Dissipation Induced Instabilities." Annales de l'Institut Henri Poincare (C) Non Linear Analysis 11, no. 1 (January 1994): 37–90. http://dx.doi.org/10.1016/s0294-1449(16)30196-2.

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33

Meyer, F. "Accretion Disk Instabilities." International Astronomical Union Colloquium 89 (1986): 249–67. http://dx.doi.org/10.1017/s0252921100086115.

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In this article we discuss two instabilities of stationary accretion disks which lead to an understanding of observed light variations in accretion disk systems, the dwarf novae and the rapid burster MXB 17030-335. The accretion disks in these systems avoid instability at the cost of stationarity and perform stable cycles in which sudden changes of the accretion flow lead to corresponding, often dramatic, variations of their accretion luminosity.Figure 1 shows a light curve of U Geminorum. It was discovered In 1855 by J.R. Hind and has become a prototype of the dwarf novae. In these systems an extended time of quiescence of up to several weeks Is followed by a short outburst of a few days during which the luminosity rises by a factor of 30 to 100. The dwarf novae belong to the cataclysmic variables. They are all close binaries In which a white dwarf primary is orbited by a Roche lobe-filling low mass secondary. Through the inner Lagrangian point mass flows over from the secondary and forms a luminious accretion disk around the white dwarf. In the case of the dwarf novae this disk has temperatures below about 10000K in Its outer region. It will be discussed how partial lonizatlon and convection then affect the vertical structure of the disk such that the stationary flow becomes unstable.Fig. 1. Light curve of the dwarf nova U Geminorum. Abszissa in days С [2])

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34

King, A. R. "Accretion Disc Instabilities." Symposium - International Astronomical Union 151 (1992): 195–203. http://dx.doi.org/10.1017/s0074180900122193.

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I give a brief discussion of accretion disc instabilities, concentrating mainly on tidal instabilities caused by the presence of a binary companion. The superhumps observed in superoutbursts of SU UMa dwarf novae probably result from the excitation of a resonance in the accretion disc near the 3:1 commensurability with the binary orbit. This resonance can only appear for mass ratios q = M2/M1 < qerit ≃ 0.25 – 0.33: for larger mass ratios the available resonances are considerably weaker. Application of this picture to other types of binary suggests that the condition q < qerit may be necessary but not sufficient. Further, some cataclysmic systems show phenomena which could be tidal in origin even though the condition evidently fails.

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35

Kwak, C. H., J. Takacs, and L. Solymar. "Spatial subharmonic instabilities." Optics Communications 96, no. 4-6 (February 1993): 278–82. http://dx.doi.org/10.1016/0030-4018(93)90275-a.

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36

Lindner, Anke, and Christian Wagner. "Viscoelastic surface instabilities." Comptes Rendus Physique 10, no. 8 (November 2009): 712–27. http://dx.doi.org/10.1016/j.crhy.2009.10.017.

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37

Juel, Anne, Draga Pihler-Puzović, and Matthias Heil. "Instabilities in Blistering." Annual Review of Fluid Mechanics 50, no. 1 (January 5, 2018): 691–714. http://dx.doi.org/10.1146/annurev-fluid-122316-045106.

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38

Mineshige, S. "Accretion Disk Instabilities." International Astronomical Union Colloquium 134 (1993): 83–103. http://dx.doi.org/10.1017/s0252921100013968.

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AbstractBasic properties of accretion disk instabilities are summarized. We first explain the standard disk model by Shakura and Sunyaev. In this model, the dominant sources of viscosity are assumed to be chaotic magnetic fields and turbulence in gas flow, and the magnitude of viscosity is prescribed by so-called a model. It is then possible to build a particular disk model. In the framework of the standard model, accretion disks are stationary, but when some of the basic assumptions are relaxed, various kinds of instabilities appear. In particular, we focus on the thermal limit-cycle instability caused by partial ionization of hydrogen (and helium). We demonstrate that the disk instability model well accounts for the basic observed features of outbursts of dwarf novae and X-ray nova. We then introduce other kinds of instabilities based on the α viscosity model. They are suspected to produce time variabilities observed on a wide range of timescales in close binaries and active galactic nuclei.

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39

Blum, A., H. Coudane, and D. Molé. "Gleno-humeral instabilities." European Radiology 10, no. 1 (January 10, 2000): 63–82. http://dx.doi.org/10.1007/s003300050008.

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40

Roupas, Zacharias. "Relativistic gravothermal instabilities." Classical and Quantum Gravity 32, no. 13 (June 16, 2015): 135023. http://dx.doi.org/10.1088/0264-9381/32/13/135023.

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41

CHADAM, J., D. HOFF, E. MERINO, P. ORTOLEVA, and A. SEN. "Reactive Infiltration Instabilities." IMA Journal of Applied Mathematics 36, no. 3 (1986): 207–21. http://dx.doi.org/10.1093/imamat/36.3.207.

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42

Mineshige, S. "Accretion disk instabilities." Astrophysics and Space Science 210, no. 1-2 (December 1993): 83–103. http://dx.doi.org/10.1007/bf00657876.

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43

Silva, Camilo F. "Intrinsic thermoacoustic instabilities." Progress in Energy and Combustion Science 95 (March 2023): 101065. http://dx.doi.org/10.1016/j.pecs.2022.101065.

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44

Lott, François, Hennie Kelder, and Hector Teitelbaum. "A transition from Kelvin–Helmholtz instabilities to propagating wave instabilities." Physics of Fluids A: Fluid Dynamics 4, no. 9 (September 1992): 1990–97. http://dx.doi.org/10.1063/1.858368.

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45

Jung, Peter, and Peter Hänggi. "Optical instabilities: new theories for colored-noise-driven laser instabilities." Journal of the Optical Society of America B 5, no. 5 (May 1, 1988): 979. http://dx.doi.org/10.1364/josab.5.000979.

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46

KERR, OLIVER S. "Oscillatory double-diffusive instabilities in a vertical slot." Journal of Fluid Mechanics 426 (January 10, 2001): 347–54. http://dx.doi.org/10.1017/s0022112000002445.

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Recent linear stability analyses of double-diffusive convection in a laterally heated vertical slot containing water have shown that for very weak (or no) vertical salinity gradient the initial instabilities are steady, but as the salinity gradient is increased there is a transition to oscillatory instabilities. For higher Prandtl number fluids the initial instabilities in a slot with no stratification can be oscillatory or wave-like. We show that the oscillatory instabilities in water are linked to these higher Prandtl number oscillatory instabilities. The salinity gradient has a destabilizing effect on these oscillations, making them appear for Prandtl numbers where oscillatory instabilities are not possible in the absence of salinity gradients. We derive an asymptotic description for this mode of instability.

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47

Parker, R. G., and Y. Lin. "Parametric Instability of Axially Moving Media Subjected to Multifrequency Tension and Speed Fluctuations." Journal of Applied Mechanics 68, no. 1 (June 27, 2000): 49–57. http://dx.doi.org/10.1115/1.1343914.

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This work investigates the stability of axially moving media subjected to parametric excitation resulting from tension and translation speed oscillations. Each of these excitation sources has spectral content with multiple frequencies and arbitrary phases. Stability boundaries for primary parametric instabilities, secondary instabilities, and combination instabilities are determined analytically through second-order perturbation. The classical result that primary instability occurs when one of the excitation frequencies is close to twice a natural frequency changes as a result of multiple excitation frequencies. Unusual interactions occur for the practically important case of simultaneous primary and secondary instabilities. While sum type combination instabilities occur, no difference type instabilities are detected. The nonlinear limit cycle amplitude that occurs under primary instability is derived using the method of multiple scales.

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48

Nagalla, Satya Abhihst. "Analysis and Control of Combustion Instabilities in Rocket Engines." International Journal for Research in Applied Science and Engineering Technology 9, no. VIII (August 10, 2021): 223–28. http://dx.doi.org/10.22214/ijraset.2021.37305.

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Sound is the transmission of energy that is produced when two particles or objects undergo collision. It is one of the forms in which energy modulates and travels in a medium. Vibration is a phenomenon in which an object of mass executes a periodic oscillatory displacement when certain energy is transferred to it. Combustion is a chemical reaction in which a lot of molecules collide. Combustion instabilities occur in a reacting flow. It is a physical phenomenon. Combustion instabilities have mostly been studied in a particular flow but they also occur in real life. Real engines often feature specific unstable modes such as azimuthal instabilities in gas turbines or transverse modes in rocket chambers. Eddy simulation has been the major tool to study this type of instabilities so far but recently it has been proved to be insufficient to completely understand the complex nature of these instabilities [3]. These instabilities involve large Reynolds number, high pressure, densities in real engines. Combustion instabilities can occur at any part of the rocket propulsion system like nozzle, combustion chamber, injectors, feed systems and lines. Theory plays an important role in understanding and analysing these instabilities and the amount of damage they can cause to a particular object. In this paper we will look at different types or modes of combustion instabilities and active and passive ways to control them in real situations.

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49

Ruspini, L. C., C. A. Dorao, and M. Fernandino. "ICONE19-43568 MODELING OF DYNAMIC INSTABILITIES IN BOILING SYSTEMS." Proceedings of the International Conference on Nuclear Engineering (ICONE) 2011.19 (2011): _ICONE1943. http://dx.doi.org/10.1299/jsmeicone.2011.19._icone1943_232.

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50

Rudykh, S., K. Bhattacharya, and G. deBotton. "Multiscale instabilities in soft heterogeneous dielectric elastomers." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 470, no. 2162 (February 8, 2014): 20130618. http://dx.doi.org/10.1098/rspa.2013.0618.

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The development of instabilities in soft heterogeneous dielectric elastomers is investigated. Motivated by experiments and possible applications, we use in our analysis the physically relevant referential electric field instead of electric displacement. In terms of this variable, a closed form solution is derived for the class of layered neo-Hookean dielectrics. A criterion for the onset of electromechanical multiscale instabilities for the layered composites with anisotropic phases is formulated. A general condition for the onset of the macroscopic instability in soft multiphase dielectrics is introduced. In the example of the layered dielectrics, the essential influence of the microstructure on the onset of instabilities is revealed. We found that: (i) macroscopic instabilities dominate at moderate volume fractions of the stiffer phase, (ii) interface instabilities appear at small volume fractions of the stiffer phase and (iii) instabilities of a finite scale, comparable to the microstructure size, occur at large volume fractions of the stiffer phase. The latest new type of instabilities does not appear in the purely mechanical case and dominates in the region of large volume fractions of the stiff phase.

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