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For inherently unstable aircraft, see Relaxed stability. A ball on the top of a hill is an unstable situation. In numerous fields of study, the component of instability within a system is generally characterized by some of the outputs or internal states growing without bounds. Not all systems that are not stable are unstable; systems can also be marginally stable or exhibit limit cycle behavior. In control theory, a system is unstable (or as sometimes referred to as instable) if any of the roots of its characteristic equation has real part greater than zero. This is equivalent to any of the eigenvalues of the state matrix having real part greater than zero. In structural engineering, a structure can become unstable when excessive load is applied. Beyond a certain threshold, structural deflections magnify stresses, which in turn increases deflections. This can take the form of buckling or crippling. The general field of study is called structural stability. Atmospheric instability is a major component of all weather systems on Earth. Contents 1 Fluid instabilities 2 Plasma instabilities 3 Instabilities of stellar systems 4 See also 5 Notes 6 External links Fluid instabilities Hydrodynamics simulation of the Rayleigh–Taylor instability [1] Unstable flow structure generated from the collision of two impinging jets. Fluid instabilities occur in liquids, gases and plasmas, and are often characterized by the shape that form; they are studied in fluid dynamics and magnetohydrodynamics. Fluid instabilities include: Ballooning mode instability (some analogy to the Rayleigh–Taylor instability); found in the magnetosphere Atmospheric instability Hydrodynamic instability or dynamic instability (atmospheric dynamics) Inertial instability; baroclinic instability; symmetric instability, conditional symmetric or convective symmetric instability; barotropic instability; Helmholtz or shearing instability; rotational instability Hydrostatic instability or static instability/vertical instability (parcel instability), thermodynamic instability (atmospheric thermodynamics) Conditional or static instability, buoyant instability, latent instability, nonlocal static instability, conditional-symmetric instability; convective, potential, or thermal instability, convective instability of the first and second kind; absolute or mechanical instability Bénard instability Drift mirror instability Kelvin–Helmholtz instability (similar, but different from the diocotron instability in plasmas) Rayleigh–Taylor instability Plateau-Rayleigh instability (similar to the Rayleigh–Taylor instability) Richtmyer-Meshkov instability (similar to the Rayleigh–Taylor instability) Plasma instabilities Main article: Plasma_stability#Plasma_instabilities Plasma instabilities can be divided into two general groups (1) hydrodynamic instabilities (2) kinetic instabilities. Plasma instabilities are also categorised into different modes - see this paragraph in plasma stability. Instabilities of stellar systems Galaxies and star clusters can be unstable, if small perturbations in the gravitational potential cause changes in the density that reinforce the original perturbation. Such instabilities usually require that the motions of stars be highly correlated, so that the perturbation is not "smeared out" by random motions. After the instability has run its course, the system is typically "hotter" (the motions are more random) or rounder than before. Instabilities in stellar systems include: Bar instability of rapidly-rotating disks Jeans instability Firehose instability[2] Gravothermal instability Radial-orbit instability Various instabilities in cold rotating disks See also Plasma stability Notes ^ Shengtai Li, Hui Li "Parallel AMR Code for Compressible MHD or HD Equations" (Los Alamos National Laboratory) [1] ^ Merritt, D.; Sellwood, J. (1994), "Bending Instabilities of Stellar Systems", The Astrophysical Journal 425: 551–567, Bibcode 1994ApJ...425..551M, doi:10.1086/174005  External links eFluids Fluid Flow Image Gallery