Following this adiabatic curve until it intersects line No.
"Scientific American Supplement, No. 799, April 25, 1891" by Various
At the same time the utmost pains are taken to maintain the adiabatic condition of the metal walls.
"Respiration Calorimeters for Studying the Respiratory Exchange and Energy Transformations of Man" by Francis Gano Benedict
The adiabatic lines, representing a fall of temperature of 1 deg.
"Sounding the Ocean of Air" by A. Lawrence Rotch
This is the ratio of the adiabatic elasticity of air to the isothermal elasticity.
"Encyclopaedia Britannica, 11th Edition, Volume 13, Slice 2" by Various
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X Y chains obtained within the continued-fraction approach may be of use for the study of the spin-Peierls instability in these chains in adiabatic limit.
Thermodynamic properties of the periodic nonuniform spin-1/2 isotropic XY chains in a transverse field
Similarly, magnetic ﬁelds may change their conﬁguration and orientation in space (e.g. due to Alfven waves), but if the time for such a change is much longer than the Larmor period the alignment of grains in respect to the ﬁeld lines persists as the consequence of preservation of the adiabatic invariant.
Physics of Grain Alignment
Thus the atmosphere has a nearly adiabatic pro ﬁle when convective.
Rotational Evolution During Type I X-Ray Bursts
For the convective zone, we integrate dT /d y = n(T /y) for a given base temperature Tb (the super-adiabaticity needed to carry the ﬂux in the convective zone is negligible when the convection is so efﬁcient; see Cox & Giuli 1968).
Rotational Evolution During Type I X-Ray Bursts
In addition, we have ttherm ≈ tE , so non-adiabatic effects may be important, reducing the effect of the thermal buoyancy (Sakurai et al. 1971).
Rotational Evolution During Type I X-Ray Bursts
The difference in slope of the convective adiabat between models is due to the differing contribution of radiation pressure.
Rotational Evolution During Type I X-Ray Bursts
In these model universes both the ordinary matter, the adiabatic perfect ﬂuid, and the scalar ﬁeld, are equally important, and one of the main enigmas to be resolved in this context is why the energy density of the additional quintessence matter almost co-incides with the usual matter density today [3, 5].
Exact Inflationary Solutions from a Superpotential
W ′ (φ) here one must assume that the “adiabatic” index of the perfect ﬂuid model describing the scalar ﬁeld is constant .
Exact Inflationary Solutions from a Superpotential
In the case when a set of slow (adiabatic) variables can be chosen, our formalism yields a general form of the macroscopic evolution law (Generalized Langevin Equation) and extends Fluctuation Dissipative Theorem.
Generalized Entropy approach to far-from-equilibrium statistical mechanics
This approach assumes the possibility of choosing a set of relatively slow (adiabatic) variables.
Generalized Entropy approach to far-from-equilibrium statistical mechanics
At the same time, the gas adiabatically re-expands to approximately the same pressure it had before being shocked.
A Moderate Cluster Cooling Flow Model
In all calculations below, we set γ = 5/3 for the adiabatic index of intracluster gas.
A Moderate Cluster Cooling Flow Model
Later Aharonov and Anandan (1987) generalized Berry’s result to any cyclic evolution of the quantum system by giving up the assumption of adiabaticity.
Smooth Loops, Generalized Coherent States and Geometric Phases
In this Letter, we further investigate this result showing that, using the CMB data alone, a purely baryonic adiabatic model of structure formation seems unlikely if the universe is ﬂat (Ω = 1).
CMB Constraints on a Baryonic Dark Matter-Dominated Universe
As is well known, purely baryonic adiabatic models are in severe contradiction with the measured amplitude and shape of galaxy and cluster correlations.
CMB Constraints on a Baryonic Dark Matter-Dominated Universe
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