scholarly journals Theoretical Fraunhofer Line Profiles in the Spectrum of the Zodiacal Light

1969 ◽  
Vol 142 (1) ◽  
pp. 45-52 ◽  
Author(s):  
J. F. James
Keyword(s):  
Line Profiles ◽  
Zodiacal Light ◽  
Fraunhofer Line

scholarly journals Zodiacal Light - Scattered Fraunhofer Line Profiles

1996 ◽  
Vol 150 ◽  
pp. 337-340
Author(s):  
David Clarke
Keyword(s):  
Line Shape ◽  
Brightness Variation ◽  
Line Profiles ◽  
Scattering Function ◽  
Zodiacal Light ◽  
Successful Model ◽  
Fraunhofer Line ◽  
Shape Changes

AbstractThe scattering function of Hong's successful model for the brightness variation with elongation, B(ε), of the Zodiacal Light has been used to calculate profiles of Doppler shifted Fraunhofer lines. Substantial line shape changes with ε are predicted with an indication of a bifurcation at ε < 30°, so offering an explanation for reported F corona observations.

scholarly journals Anomalous Fraunhofer Line Profiles

Nature ◽  
1962 ◽  
Vol 193 (4817) ◽  
pp. 762-762 ◽  
Author(s):  
J. F. GRAINGER ◽  
J. RING
Keyword(s):  
Line Profiles ◽  
Fraunhofer Line

scholarly journals Doppler Shifts Measurements of the Zodiacal Light at the Pic Midi Observatory

1985 ◽  
Vol 85 ◽  
pp. 85-88
Author(s):  
R. Robley ◽  
A. Bücher ◽  
S. Koutchmy ◽  
Ph. Lamy
Keyword(s):  
Accurate Determination ◽  
Interplanetary Dust ◽  
Emission Lines ◽  
Line Profiles ◽  
Atmospheric Emission ◽  
Zodiacal Light ◽  
Doppler Shifts ◽  
Channel Plate ◽  
Micro Channel Plate

AbstractAt the Pic-du-Midi Observatory, we have started a program to observe the spectrum of the zodiacal light in the region of the b absorption lines of MgI. We use a 1 meter spectrograph with a holographic grating followed by a focal reducer to obtain a 19 Å/mm dispersion over the micro-channel plate camera. Calibrated spectra obtained with an exposure time of 10 minutes systematically show earth atmospheric emission lines attributed to both NI and OH. The temporal variability of these emissions prevents an accurate determination of the line profiles. Our best processed measurements of Doppler shifts obtained during five nights do not allow to descriminate between circular and hyperbolic orbits of the interplanetary dust.

Fraunhofer line profiles

Solar Physics ◽  
1984 ◽  
Vol 90 (1) ◽  
pp. 195-197 ◽  
Author(s):  
A. Keith Pierce
Keyword(s):  
Line Profiles ◽  
Fraunhofer Line

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.

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