5.2.8.1 The relative spectral-intensity distribution in stellar spectra

2005 ◽  
pp. 374-380
Author(s):  
E. Lamla
Keyword(s):  
Intensity Distribution ◽  
Spectral Intensity ◽  
Stellar Spectra

Spectral Intensity Distribution of a Time Dependent Gaussian Pulsed Beam From a Circular Aperture in the Near-Field Diffraction

2003 ◽  
Vol 10 (1) ◽  
pp. 19-23 ◽  
Author(s):  
Gwo-Huei Yang ◽  
Hone-Ene Hwang ◽  
Pin Han
Keyword(s):  
Intensity Distribution ◽  
Near Field ◽  
Spectral Intensity ◽  
Time Dependent ◽  
Circular Aperture

Spectral intensity distribution in a hydrogen discharge

1927 ◽  
Vol 204 (2) ◽  
pp. 219-225 ◽  
Author(s):  
E.W. Tschudi
Keyword(s):  
Intensity Distribution ◽  
Spectral Intensity ◽  
Hydrogen Discharge

On the Spectral Intensity Distribution of Donor–Acceptor Pair Recombination in GaP

1974 ◽  
Vol 66 (1) ◽  
pp. 133-143 ◽  
Author(s):  
R. Bindemann ◽  
K. Unger
Keyword(s):  
Intensity Distribution ◽  
Spectral Intensity ◽  
Acceptor Pair ◽  
Donor Acceptor ◽  
Donor Acceptor Pair

Studies of the Afterglow in Mercury Vapor. II. Spectral Intensity Distribution

1941 ◽  
Vol 60 (3) ◽  
pp. 216-224 ◽  
Author(s):  
George E. Moore ◽  
Robert C. Garth
Keyword(s):  
Intensity Distribution ◽  
Mercury Vapor ◽  
Spectral Intensity

scholarly journals The Shape of the Interstellar Reddening Curve

1965 ◽  
Vol 7 ◽  
pp. 27-37
Author(s):  
Anne B. Underhill ◽  
Gordon A. H. Walker
Keyword(s):  
Spectral Type ◽  
Intensity Distribution ◽  
Spectral Intensity ◽  
Type Star ◽  
Early Type ◽  
The Earth ◽  
Early Type Star ◽  
Sensitivity Factors ◽  
Interstellar Material ◽  
The Difference

When the Observed Spectral Intensity Distribution of an early-type star has been freed from the distortions caused by absorption in the Earth's atmosphere and by instrumental sensitivity factors, it is a measure of the true spectral intensity distribution of the star and of the modifications to that distribution caused by the interstellar material between the Earth and the star. Thus, if one knew the true intensity distribution from the star, one could derive the shape of the interstellar reddening curve. In practice it is customary to compare the intensity distributions of pairs of stars of apparently the same spectral type, within the errors of classification, but which suffer different amounts of reddening, and to attribute the difference to interstellar reddening. In this way one can determine the shape of the interstellar reddening curve.

scholarly journals On the Polarization and Anisotropy of Solar X-Radiation During Flares

1971 ◽  
Vol 2 ◽  
pp. 575-579
Author(s):  
G. Elwert ◽  
E. Haug
Keyword(s):  
Angular Distribution ◽  
Thermal Radiation ◽  
Velocity Distribution ◽  
Intensity Distribution ◽  
Solar Flares ◽  
Short Wavelength ◽  
Initial Phase ◽  
Spectral Intensity ◽  
Energy Distributions ◽  
Preferred Direction

From the spectral intensity distribution of solar X-radiation one can conclude that there is a non-thermal contribution, which is effective during the initial phase of a flare. It is reasonable to suppose that the electrons producing the non-thermal radiation have a non-isotropic velocity distribution. Indeed, one should assume that the electrons, during their acceleration, obtain a preferred direction and that only afterwards does their velocity distribution become Maxwellian by means of collisions. Hence the short-wavelength continuous X-radiation in the initial phase of a flare, consisting mainly of bremsstrahlung, should be polarized and should have a non-isotropic angular distribution.In papers presented to the IAU-Symposia in Budapest 1967 (Elwert, 1968) and in Leningrad last May, the polarization of X-radiation from electrons of a few keV accelerated in solar flares has been calculated using energy distributions based on the observations of Pounds et al. obtained with the satellites Ariel I and OSO-4.

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