Pressure-dependent properties of absorption- and emission-band shapes of impurities in solids

1975 ◽  
Vol 12 (2) ◽  
pp. 594-599 ◽  
Author(s):  
C. Stuart Kelley
Keyword(s):  
Emission Band ◽  
Absorption And Emission

Synthesis, Oxidation and Photophysical Properties of Novel Derivatives of Acyclic Aromatic Amines

2007 ◽  
Vol 72 (9) ◽  
pp. 1255-1268 ◽  
Author(s):  
Csaba Kósa ◽  
Jaroslav Mosnáček ◽  
Adela Bílešová ◽  
Peter Kasák ◽  
Juraj Kronek ◽  
...  
Keyword(s):  
Quantum Yield ◽  
Emission Band ◽  
Photophysical Properties ◽  
Emission Spectra ◽  
Polymer Matrices ◽  
Photochemical Oxidation ◽  
Methoxy Derivative ◽  
Polar Solution ◽  
Absorption And Emission ◽  
Wavelength Absorption

Conjugated acyclic arylamine derivatives, N-(4-methylphenyl)-N-(2-methyl-1-phenylpropyl)amine and N-(4-methoxyphenyl)-N-(2-methyl-1-phenylpropyl)amine, have been synthesized and characterized. Their photophysical properties have been investigated in polar methanol and non-polar cyclohexane solutions, and in PS and PMMA polymer matrices. The influence of the environment polarity as well as of the substituent in para-position of the aryl on the absorption, emission spectra and the fluorescence quantum yield has been studied. In the absorption and emission spectra, the observed absorption and emission band maxima were red shifted and the observed quantum yield was higher in the polar solution in comparison with the non-polar solution or polymer matrices. The distance of short- and long-wavelength absorption maxima in the methoxy derivative was larger and the emission band was red shifted in comparison with the methyl derivative. Chemical and photochemical oxidation of the prepared amines gives unstable nitroxides. High intramolecular quenching was observed in polymer matrix after photochemical oxidation of the amines.

Polar Dyes in Solution:  A Joint Experimental and Theoretical Study of Absorption and Emission Band Shapes

2002 ◽  
Vol 106 (26) ◽  
pp. 6286-6294 ◽  
Author(s):  
Barbara Boldrini ◽  
Enrico Cavalli ◽  
Anna Painelli ◽  
Francesca Terenziani
Keyword(s):  
Emission Band ◽  
Theoretical Study ◽  
Absorption And Emission

Some Results of the Spectroscopic Study of Four Close Binary Systems of Early Spectral Types

1965 ◽  
Vol 5 ◽  
pp. 120-130
Author(s):  
T. S. Galkina
Keyword(s):  
Spectroscopic Study ◽  
Spectral Type ◽  
Spectroscopic Investigation ◽  
Binary Systems ◽  
Quantitative Information ◽  
Close Binary ◽  
Physical Parameters ◽  
Absorption And Emission ◽  
Close Binary Systems ◽  
Quantitative Estimates

It is necessary to have quantitative estimates of the intensity of lines (both absorption and emission) to obtain the physical parameters of the atmosphere of components.Some years ago at the Crimean observatory we began the spectroscopic investigation of close binary systems of the early spectral type with components WR, Of, O, B to try and obtain more quantitative information from the study of the spectra of the components.

Polarimetric Observations of Red Variables: A Study of Gas and Particle Interactions

1979 ◽  
Vol 46 ◽  
pp. 386-408 ◽  
Author(s):  
G. V. Coyne ◽  
I. S. McLean
Keyword(s):  
Wavelength Dependence ◽  
Stellar Atmosphere ◽  
Molecular Absorption ◽  
Absorption Bands ◽  
Absorption And Emission ◽  
Mira Variables ◽  
Stellar Photosphere ◽  
Regular Variable ◽  
Red Supergiants ◽  
Balmer Lines

AbstractIn recent years the wavelength, dependence of the polarization in a number of Mira variables, semi-regular variables and red supergiants has been measured with resolutions between 0.3 and 300 A over the range 3300 to 11000 A. Variations are seen across molecular absorption bands, especially TiO bands, and across atomic absorption and emission lines, especially the Balmer lines. In most cases one can ignore or it is possible to eliminate the effects due to interstellar polarization, so that one can study the polarization mechanisms operating in the stellar atmosphere and environment. The stars Omicron Ceti. (Mira), V CVn (semi-regular variable) and Mu Cephei (M2 la), in addition to other stars similar to them, will be discussed in some detail.Models to explain the observed polarization consider that the continuum flux is polarized either by electron, molecular and/or grain scattering or by temperature variations and/or geometrical asymmetries over the stellar photosphere. This polarized radiation is affected by atomic and molecular absorption and emission processes at various geometric depths in the stellar atmosphere and envelope. High resolution spectropolarimetry promises, therefore, to be a power-rul tool for studying stratification effects in these stars.

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