Detection of selected solar-stimulated fluorophores with a Fraunhofer line radiometer

2008 ◽  
Vol 2 (1) ◽  
pp. 023504
Author(s):  
Robert L. Fischer
Keyword(s):  
Fraunhofer Line

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

SHIELDS: A battlespace Fraunhofer line discriminator for real-time aerosol cloud analysis

2007 ◽  
Author(s):  
S. Watchorn ◽  
J. Noto ◽  
J. Anderson ◽  
C. S. Sioris ◽  
M. A. Migliozzi
Keyword(s):  
Real Time ◽  
Fraunhofer Line ◽  
Aerosol Cloud ◽  
Cloud Analysis

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 X.—On the Spectrum of Nova Persei and the Structure of its Bands, as photographed at Glasgow

1906 ◽  
Vol 41 (2) ◽  
pp. 251-290
Author(s):  
L. Becker
Keyword(s):  
Wave Length ◽  
Line Spectrum ◽  
Fraunhofer Line ◽  
Hydrogen Lines

The spectrum of the new star in Perseus, which Dr Anderson, of Edinburgh, discovered 1901 February 21, was photographed at the Glasgow Observatory from 1901 March 3 till 1903 January. From the early photographs one gains the impression that the spectrum consists of a number of bright bands of different lengths, fading towards the ends, and overlapping each other, thus producing a series of maxima and minima of brightness. Near wave-length 5000 the intensity rapidly falls off towards the less refrangible side, and the bands appear detached. The middle of each of the three most intense maxima approximately coincide with the hydrogen lines Hβ, Hγ, Hδ, and on two photo-plates, March 18 to 20 and March 25, each of the bands is crossed by a sharp Fraunhofer line. On the photo-plates taken after 1901 August 1 the bands are all detached; some, including the two bands whose middles approximately coincide with the principal nebular lines, have almost the same lengths, and suggest a line spectrum in which the lines have been broadened into bands, others are considerably longer and have pronounced maxima.

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