Hydrodynamical Models of Aerosol Induced Breakdown

1984 ◽  
pp. 761-769
Author(s):  
P. Vigliano ◽  
M. Autric ◽  
J. P. Caressa ◽  
V. Chhim ◽  
G. Inglésakis
Keyword(s):  
Hydrodynamical Models

scholarly journals Hydrodynamical Models of Outflow Collimation in Young Stellar Objects

1996 ◽  
Vol 472 (2) ◽  
pp. 684-702 ◽  
Author(s):  
Adam Frank ◽  
Garrelt Mellema
Keyword(s):  
Young Stellar Objects ◽  
Stellar Objects ◽  
Hydrodynamical Models

The Early Spectra of SN 1987A

1988 ◽  
Vol 7 (4) ◽  
pp. 431-433 ◽  
Author(s):  
R.P. Harkness ◽  
J.C. Wheeler
Keyword(s):  
Hydrodynamical Models ◽  
Sn 1987A

AbstractSpectra computed from hydrodynamical models for SN 1987A at very early times (t < 2 days) are presented and discussed.

scholarly journals Testing Hydrodynamical Models on the Characteristics of a One-Dimensional Submicrometer Structure

VLSI Design ◽  
1998 ◽  
Vol 6 (1-4) ◽  
pp. 155-160
Author(s):  
A. M. Anile ◽  
O. Muscato ◽  
S. Rinaudo ◽  
P. Vergari
Keyword(s):  
High Speed ◽  
Relaxation Times ◽  
Drift Diffusion Model ◽  
Drift Diffusion ◽  
Industrial Environment ◽  
Hydrodynamical Models ◽  
One Dimensional ◽  
Simulation Tools ◽  
Speed Performance ◽  
Output Characteristics

Recent advances in technology leads to increasing high speed performance of submicrometer electron devices by the scaling of both process and geometry. In order to aid the design of these devices it is necessary to utilize powerful numerical simulation tools. In an industrial environment the simulation codes based on the Drift-Diffusion models have been widely used. However the shrinking dimension of the devices causes the Drift-Diffusion based simulators to become less accurate. Then it is necessary to utilize more refined models (including higher order moments of the distribution function) in order to correctly predict the behaviour of these devices. Several hydrodynamical models have been considered as viable simulation tools. It is possible to discriminate among the several hydrodynamical models on the basis of their results on the output characteristics of the electron device which are measurable (I-V curves). We have analyzed two classes of hydrodynamical models: i) HFIELDS hydrodynamical models and HFIELDS drift-diffusion model; ii) self-consistent extended hydrodynamical models with relaxation times determined from Monte Carlo simulations.

Sidetracks Drilling Supported by Hydrodynamical Models of Reservoir

2010 ◽  
Author(s):  
Alexander B. Starostin ◽  
Alexander Basak
Keyword(s):  
Hydrodynamical Models

scholarly journals Accurate Fourier Decomposition of Cepheid Radial Velocity Curves

2000 ◽  
Vol 176 ◽  
pp. 233-234 ◽  
Author(s):  
P. Moskalik ◽  
T. Krzyt ◽  
N. A. Gorynya ◽  
N. N. Samus
Keyword(s):  
Radial Velocity ◽  
Light Curves ◽  
Fourier Decomposition ◽  
Hydrodynamical Models ◽  
Classical Cepheid

AbstractThe shapes of light curves and of radial velocity curves are two main predictions of the hydrodynamical models of Cepheids. Of the two, the velocity curves are more robust numerically and therefore, more suitable for comparison with the observations. In this report, we present accurate Fourier parameters for an extensive set of classical Cepheid velocity curves. Published radiative models reproduce the observations very well, with only small discrepancies present. We estimate the center of the ω2 = 2ω0 resonance to occur at Pr = 9.947 ± 0.051 day

scholarly journals Radiation-hydrodynamical models of X-ray photoevaporation in carbon-depleted circumstellar discs

2019 ◽  
Vol 490 (4) ◽  
pp. 5596-5614 ◽  
Author(s):  
Lisa Wölfer ◽  
Giovanni Picogna ◽  
Barbara Ercolano ◽  
Ewine F van Dishoeck
Keyword(s):  
Mass Loss ◽  
Gas Phase ◽  
Central Star ◽  
X Rays ◽  
Hydrodynamical Models ◽  
X Ray ◽  
Energetic Radiation ◽  
Low Metallicity ◽  
Penetration Depths ◽  
Loss Rates

ABSTRACT The so-called transition discs provide an important tool to probe various mechanisms that might influence the evolution of protoplanetary discs and therefore the formation of planetary systems. One of these mechanisms is photoevaporation due to energetic radiation from the central star, which can in principal explain the occurrence of discs with inner cavities like transition discs. Current models, however, fail to reproduce a subset of the observed transition discs, namely objects with large measured cavities and vigorous accretion. For these objects the presence of (multiple) giant planets is often invoked to explain the observations. In our work, we explore the possibility of X-ray photoevaporation operating in discs with different gas-phase depletion of carbon and show that the influence of photoevaporation can be extended in such low-metallicity discs. As carbon is one of the main contributors to the X-ray opacity, its depletion leads to larger penetration depths of X-rays in the disc and results in higher gas temperatures and stronger photoevaporative winds. We present radiation-hydrodynamical models of discs irradiated by internal X-ray + EUV radiation assuming carbon gas-phase depletions by factors of three, 10, and 100 and derive realistic mass-loss rates and profiles. Our analysis yields robust temperature prescriptions as well as photoevaporative mass-loss rates and profiles which may be able to explain a larger fraction of the observed diversity of transition discs.

scholarly journals Emission-Line Profiles in Planetary Nebulae

1968 ◽  
Vol 34 ◽  
pp. 267-269
Author(s):  
Donald E. Osterbrock
Keyword(s):  
Velocity Distribution ◽  
Emission Line ◽  
Observational Data ◽  
Planetary Nebulae ◽  
Line Profiles ◽  
Measured Velocity ◽  
Hydrodynamical Models ◽  
Internal Velocity ◽  
First Time

This research was undertaken with the idea of measuring as accurately as possible the internal-velocity distribution in planetary nebulae, in order to compare the observational measurements with hydrodynamical models of expanding nebulae. Much of the work was done in collaboration with J. S. Miller and D.W. Weedman. All the observational data were obtained photographically with the Coudé spectrograph of the 100-inch telescope at Mt. Wilson, using an image rotator, a 900 line/mm grating, and an F/5-2 camera, giving a dispersion of about 4 Å/mm in the blue and about 6 Å/mm in the red. The measured velocity resolution is approximately 5–6 km/sec. The data for five nebulae have been published (Osterbrock et al., 1966) while data for three more, NGC 2392, NGC 3242, and IC 418 are discussed here for the first time.

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