Plotted alongside this, although almost indiscernible, is the same solution expect using the nonexpanding spacetime kernel (dashed line), obtained by setting H → 0, a → constant in Eq. (2.5), and the solution based on the adiabatic-Markovian approximation of Eq. (1.2) (dot-dashed line) for the same parameter set.
Warm inflation solution to the eta-problem
Also shown (as two solid lines) is the 68% constraint on the power spectrum after implementing a prior which restricts the range of theories to a 10-parameter space of adiabatic inﬂationary theories (from ).
Statistical Challenges of Cosmic Microwave Background Analysis
The crosses are the SPH results; the solid line gives the analytic solution for an adiabatic shock, and the dashed line for an isothermal shock.
Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
From Fig. 40 it is clear that the temperature peaks at z ≈ 3 and that the gas becomes close to isothermal (adiabatic index γ ≈ 1), but the present constraints are not suﬃcient to distinguish between a sharp rise (as indicated by the dashed line) and a more gradual increase.
The First Cosmic Structures and their Effects
The terms of the right hand side of equation (20) are adiabatic changes along the dipole ﬁeld line, synchrotron losses and cyclotron/synchrotron resonant absorption. A derivation of the above equations (minus the CR loss and resonant absorption terms) is given in the Appendix.
High-Energy Emission From Millisecond Pulsars
An optical lattice is turned on adiabatically, until the system passes the line of instability (See Fig. 11), and then slowly turned off.
Decay of a superfluid currents in a moving system of strongly interacting bosons
Given an equation of state, the line of thought introduces black-hole Cauchy horizon instability criteria in terms of the associated adiabatic index Γ, revealing a connection between this sub ject and the stability theory of relativistic stars.
Strong cosmic censorship: the role of nearly extreme nonrotating black holes
The line ratios are consistent with those expected from radiative shocks with velocity 310 − 390 km s−1 , corresponding to a shock temperature of (1.6 − 2.5) × 106 K. A fraction of the coronal emission may, however, originate in higher velocity adiabatic shocks.
Coronal emission from the shocked circumstellar ring of SN 1987A
However, in order to explain the slower evolution of the intermediate ionization lines such as [Ne V], [Ar V] and [Fe VII], we do require that some fraction of the [Fe X-XIV] ﬂuxes arise from adiabatic shocks which would not be contributing to the intermediate and low ionization lines.
Coronal emission from the shocked circumstellar ring of SN 1987A
The large range in ionization stage with similar line proﬁles shows that most of the emission is coming from radiative shocks with velocity 310 − 390 km s−1 , although a fraction of the coronal line emission may originate in adiabatic shocks.
Coronal emission from the shocked circumstellar ring of SN 1987A
Plotted alongside this, although almost indiscernible, is the same solution expect using the nonexpanding spacetime kernel (dashed line), obtained by setting H → 0, a → constant in Eq. (59), and the solution based on the adiabatic-Markovian approximation of Eq. (5) (dot-dashed line) for the same parameter set.
Inflation in the warm and cold regimes
Markey & Tayler (1973) and Wright (1973) performed similar adiabatic stability analyses for axisymmetric poloidal ﬁelds and concluded its general instability if at least some of its ﬁeld lines are closed within the star.
Turning Points in the Evolution of Isolated Neutron Stars' Magnetic Fields
The dotted line there denotes the adiabatic curve of the magnetization.
Quantum response to time-dependent external fields
The lines represent the predicted dependencies ˙m ∝ (∆Φ)γg /(γg −1) where the variability of γg = 4/3 is the adiabatic index.
Foundations of Black Hole Accretion Disk Theory
The wind velocities are almost identical in the quasi-adiabatic models A and B (solid and dotted lines, respectively).
The Steady State Wind Model for Young Stellar Clusters with an Exponential Stellar Density Distribution
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