Parametric Studies with an Arc Electrode Mass Loss Model*

2010 ◽  
Author(s):  
Joseph Sheeley
Keyword(s):  
Mass Loss ◽  
Loss Model ◽  
Electrode Mass ◽  
Parametric Studies

Laser-induced tissue ablation described by linear mass loss model

2000 ◽  
Author(s):  
Dan C. Dumitras ◽  
Consuela-Elena Matei ◽  
Doru C. A. Dutu
Keyword(s):  
Mass Loss ◽  
Tissue Ablation ◽  
Linear Mass ◽  
Loss Model

scholarly journals Chemical Separation vs Rotation in a and F-Stars

1993 ◽  
Vol 138 ◽  
pp. 474-489
Author(s):  
Paul Charbonneau
Keyword(s):  
Mass Loss ◽  
Convection Zone ◽  
Chemical Separation ◽  
Chemical Abundances ◽  
Loss Model ◽  
Peculiar Stars ◽  
Thermally Driven ◽  
Chemically Peculiar Stars ◽  
F Stars ◽  
Diffusion Mass

AbstractThe role played by rotationally-induced mixing in the diffusion-based models for non-magnetic chemically peculiar stars is investigated. This paper focuses on one specific rotationally controlled mixing mechanism, namely thermally-driven meridional circulation. Its effects on the time evolution of chemical abundances are illustrated by means of three specific examples. The first two concern the diffusion model for FmAm stars, where it is shown that while circulation has a determining influence on the settling of Helium, it has no significant effect on the diffusion of heavier metals once the He superficial convection zone has disappeared. The third example is concerned with the diffusion/mass loss model for λBootis stars. It is shown that the inclusion of circulation prevents the appearance of generalized underabundances at any epoch of the evolution, indicating that the diffusion/mass loss model for these objects must be abandoned.

scholarly journals Diffusion Models for Magnetic Ap Stars

1993 ◽  
Vol 138 ◽  
pp. 458-472
Author(s):  
J. Babel
Keyword(s):  
Mass Loss ◽  
Diffusion Theory ◽  
Transport Processes ◽  
Line Profiles ◽  
Loss Model ◽  
Spectrum Synthesis ◽  
On Line ◽  
Ap Stars ◽  
Diffusion Mass ◽  
Made In

AbstractProgress made in spectroscopy and in the diffusion theory permits now to make severe comparisons, based on line profiles, between theory and observation.We first review transport processes which are present in the atmospheric layers of Ap stars and discuss their relative importance. We then show that mass loss could play a key role for the creation of abundance maps. A mass loss model is proposed for 53 Cam and is compared, by spectrum synthesis, with visible and IUE high resolutions observations. The model accounts well for the line profiles of several elements with an exception for Ti. Furthermore, the abundance stratification predicted by this model gives close agreement with the large variation of the abundances of Cr and Fe found between the visible and UV domains. The diffusion-mass loss model finally permits to give a simple interpretation of the peculiar Ca II K lines observed in many Ap SrCrEu stars and in particular in 53 Cam, β CrB and HD 191742.

scholarly journals A Diffusion Mass-Loss Model for the Ap Star 53 Cam

1993 ◽  
Vol 137 ◽  
pp. 275-277
Author(s):  
J. Babel
Keyword(s):  
Mass Loss ◽  
Time Variation ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Spectral Features ◽  
Loss Model ◽  
A Value ◽  
Upper Limits ◽  
Ap Stars ◽  
Diffusion Mass

AbstractThe mechanism and properties of mass loss are poorly known for Ap stars. Present upper limits on the mass loss rate are of 10−10 M⊙yr−1, a value which does not permit any element separation. Abundance maps could be a very powerful tool to constrain the mass loss rate and the wind geometry of Ap stars, as surface abundances are sensitive to rates as small as 10−15 M⊙yr−1. We here propose a diffusion-mass loss model for 53 Cam and compute abundance distributions in the photosphere of 53 Cam. The mass loss geometry is determined from the Ca II K line profile and its time variation. We obtain that the diffusion-mass loss model explains many spectral features of 53 Cam, both in the UV and visible domains.

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