scholarly journals On the Asymmetry of Solar Acoustic Line Profiles

1998 ◽  
Vol 496 (1) ◽  
pp. 527-537 ◽  
Author(s):  
Mark P. Rast ◽  
Thomas J. Bogdan
Keyword(s):  
Line Profiles ◽  
The Asymmetry

Experimental Characterization Of The Asymmetry And The Dip Form Of The H[sub β]-Line Profiles In Microwave-Produced Plasmas At Atmospheric Pressure

2008 ◽  
Author(s):  
J. M. Palomares ◽  
J. Torres ◽  
M. A. Gigosos ◽  
J. J. A. M. van der Mullen ◽  
A. Gamero ◽  
...  
Keyword(s):  
Atmospheric Pressure ◽  
Line Profiles ◽  
Experimental Characterization ◽  
The Asymmetry

Variations of the asymmetry of disk-integrated solar line profiles

Solar Physics ◽  
1985 ◽  
Vol 97 (1) ◽  
pp. 1-7 ◽  
Author(s):  
David H. Bruning ◽  
Barry LaBonte
Keyword(s):  
Line Profiles ◽  
The Asymmetry

scholarly journals Asymmetry of metallic spectral lines in Cepheids

1993 ◽  
Vol 139 ◽  
pp. 375-375
Author(s):  
Michael Albrow ◽  
P.L. Cottrel
Keyword(s):  
High Resolution ◽  
Radial Velocity ◽  
Velocity Curve ◽  
Radial Velocities ◽  
Spectral Lines ◽  
Line Profiles ◽  
Radial Velocity Curve ◽  
Spectroscopic Observations ◽  
The Asymmetry

AbstractA program of high resolution spectroscopic observations of Cepheids has been carried out at Mt John University Observatory for several years. Radial velocities and asymmetries have been measured for selected metallic lines using the method of Wallerstein et al (1992).The line profiles show the largest asymmetry at phases of maximum inward velocity. The asymmetry at phases of maximum outward velocity is smaller and sometimes in the same direction as for the inward velocity maxima. Enhanced asymmetry is also noticed at phases where the bump appears on the radial velocity curve.To date our models are unable to predict such behaviour. It is important that a satisfactory explaination for these observations be found so that the accuracy of Baade-Wesselink radius solutions for such stars can be assessed.

Structuring, Motions and Shapes of Corona Emission Line Profiles

1994 ◽  
Vol 144 ◽  
pp. 421-426
Author(s):  
N. F. Tyagun
Keyword(s):  
Emission Line ◽  
Filling Factor ◽  
Direct Relationship ◽  
Coronal Plasma ◽  
Line Of Sight ◽  
Line Profiles ◽  
The Difference ◽  
Yellow Line ◽  
Red Line

AbstractThe interrelationship of half-widths and intensities for the red, green and yellow lines is considered. This is a direct relationship for the green and yellow line and an inverse one for the red line. The difference in the relationships of half-widths and intensities for different lines appears to be due to substantially dissimilar structuring and to a set of line-of-sight motions in ”hot“ and ”cold“ corona regions.When diagnosing the coronal plasma, one cannot neglect the filling factor - each line has such a factor of its own.

Effects of Ambipolar Diffusion on Prominence Thread Models

1994 ◽  
Vol 144 ◽  
pp. 315-321 ◽  
Author(s):  
M. G. Rovira ◽  
J. M. Fontenla ◽  
J.-C. Vial ◽  
P. Gouttebroze
Keyword(s):  
Energy Balance ◽  
Transition Region ◽  
Ambipolar Diffusion ◽  
Line Profiles ◽  
Balance Equations ◽  
Model Calculations ◽  
Partial Frequency ◽  
Frequency Redistribution ◽  
Partial Frequency Redistribution ◽  
Theoretical Structure

AbstractWe have improved previous model calculations of the prominence-corona transition region including the effect of the ambipolar diffusion in the statistical equilibrium and energy balance equations. We show its influence on the different parameters that characterize the resulting prominence theoretical structure. We take into account the effect of the partial frequency redistribution (PRD) in the line profiles and total intensities calculations.

The Interpretation of Line Profiles

1977 ◽  
Vol 36 ◽  
pp. 191-215
Author(s):  
G.B. Rybicki
Keyword(s):  
Magnetic Fields ◽  
Atomic Physics ◽  
Velocity Fields ◽  
Spectral Lines ◽  
Inhomogeneous Structure ◽  
The Sun ◽  
Line Profiles ◽  
Physical Phenomena

Observations of the shapes and intensities of spectral lines provide a bounty of information about the outer layers of the sun. In order to utilize this information, however, one is faced with a seemingly monumental task. The sun’s chromosphere and corona are extremely complex, and the underlying physical phenomena are far from being understood. Velocity fields, magnetic fields, Inhomogeneous structure, hydromagnetic phenomena – these are some of the complications that must be faced. Other uncertainties involve the atomic physics upon which all of the deductions depend.

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