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Neutral equilibrium

Definitions

  • Webster's Revised Unabridged Dictionary
    • Neutral equilibrium (Mech) the kind of equilibrium of a body so placed that when moved slighty it neither tends to return to its former position not depart more widely from it, as a perfect sphere or cylinder on a horizontal plane.
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Usage

In literature:

In virtue of this property, the equilibrium of the column might be termed neutral or statical equilibrium.
"The Energy System of Matter" by James Weir
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In science:

Stable quark matter should be a color singlet as a whole and neutral in the electric charge under β equilibrium.
Analytical and numerical evaluation of the Debye and Meissner masses in dense neutral three-flavor quark matter
The particle are in the neutral equilibrium state and are at rest at arbitrary R. 2.3.
Some peculiarities of motion of neutral and charged test particles in the field of a spherically symmetric charged object in General Relativity
Until now the condition of local charge neutrality in the neutron star configuration of equilibrium has been adopted mainly for mathematical simplicity (see Sec. 4.2).
Fundamental physics from black holes, neutron stars and gamma-ray bursts
A good starting point is the study of the equilibrium of a neutron star imposing global but not local charge neutrality.
Fundamental physics from black holes, neutron stars and gamma-ray bursts
If the ionization is due to photons, an abundance of neutral gas in photoionization equilibrium should still be present.
THE GUNN-PETERSON EFFECT FROM UNDERDENSE REGIONS IN A PHOTOIONIZED INTERGALACTIC MEDIUM
While the neutrinos remain in flavor equilibrium (due to neutral current interactions) throughtout most of their random walk out of the dense neutron star core, as they reach the neutrino sphere (the radius of last scattering) at ∼ 1012 g/cm3, some differences arise.
Symposium Summary and Outlook: Twenty Years of Meson Factory Physics
Hot DM refers to low-mass neutral particles that were still in thermal equilibrium after the most recent phase transition in the hot early universe, the QCD confinement transition, which took place at TQCD ≈ 102 MeV.
Dark Matter and Structure Formation in the Universe
To condense the properties of the predicted EoS in a few concise numbers let us consider pure quark stars with locally charge-neutral deconfined matter in β equilibrium.
Strange quark matter: mapping QCD lattice results to finite baryon density by a quasi-particle model
The necessary distinction of thermal and nonthermal photons would certainly benefit from an X-ray instrument with high spectral resolution, because Kα lines from neutral to low-ionized Fe, Co or Ni are not expected from thermal plasmas at ionization equilibrium.
Delayed X- and Gamma-Ray Line Emission from Solar Flare Radioactivity
Its photoionization equilibrium in the expanding IGM establishes a tight correlation between neutral and total hydrogen density and numerical simulations have confirmed the existence of this correlatio n.
Recovering the topology of the IGM at z~2
The loss of equilibrium in the system stretches the closed magnetic field such that a neutral point or a current sheet forms between the boundary surface and the flux rope.
Numerical Experiments of Wave-Like Phenomena Caused by the Disruption of an Unstable Magnetic Configuration
Every (asymptotically or neutrally) stable fix point of the replicator equation is a Nash equilibrium.
Cooperation, Norms, and Revolutions: A Unified Game-Theoretical Approach
We impose β -equilibrium and charge neutrality with neutrino trapping at finite temperature.
The pasta phase and its consequences on neutrino opacities
Neutral sodium is a minority species in the atmospheres of late-type stars, and line formation in local thermodynamic equilibrium (LTE) is often a poor assumption, in particular for strong lines.
Non-LTE calculations for neutral Na in late-type stars using improved atomic data
Several elements other than Fe provide both neutral and ionized lines and so offer a check on the condition of ionization equilibrium of Fe.
Comprehensive abundance analysis of red giants in the open clusters NGC 752, NGC 1817, NGC 2360 and NGC 2506
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