Infrared spectroscopy of Mira variables. III - R Leonis, the atomic lines

1979 ◽  
Vol 234 ◽  
pp. 548 ◽  
Author(s):  
K. H. Hinkle ◽  
T. G. Barnes
Keyword(s):  
Infrared Spectroscopy ◽  
Mira Variables ◽  
Atomic Lines

High Resolution Infrared Spectroscopy and the Nature of Mira Variability

1979 ◽  
Vol 46 ◽  
pp. 264-272
Author(s):  
Donald N. B. Hall ◽  
Kenneth H. Hinkle ◽  
Stephen T. Ridgway
Keyword(s):  
Infrared Spectroscopy ◽  
High Resolution ◽  
Absorption Line ◽  
Optical Variability ◽  
Mira Variables ◽  
Visible Spectra ◽  
Optical Wavelengths

High resolution visible spectra of Mira variables are extremely complex and despite major observing programs both by Merrill and his colleagues and more recently Wallerstein, the relation between the emission and absorption line velocities measured at optical wavelengths and either the nature of the optical variability or the observed microwave features remains elusive.

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.

Millimetre-wave and infrared spectroscopy of Br13 CN: anharmonic force field of cyanogen bromide from spectroscopic data and ab initio calculations

1997 ◽  
Vol 90 (3) ◽  
pp. 495-497
Author(s):  
CLAUDIO ESPOSTI ◽  
FILIPPO TAMASSIA ◽  
CRISTINA PUZZARINI ◽  
RICCARDO TARRONI ◽  
ZDENEK ZELINGER
Keyword(s):  
Infrared Spectroscopy ◽  
Force Field ◽  
Ab Initio Calculations ◽  
Ab Initio ◽  
Spectroscopic Data ◽  
Cyanogen Bromide ◽  
Millimetre Wave ◽  
Anharmonic Force

A long-term chemical and infrared spectroscopy study on a soil amended with municipal sewage sludge

Agronomie ◽  
2001 ◽  
Vol 21 (2) ◽  
pp. 169-178 ◽  
Author(s):  
Giovanni Gigliotti ◽  
Pier Lodovico Giusquiani ◽  
Daniela Businelli
Keyword(s):  
Infrared Spectroscopy ◽  
Sewage Sludge ◽  
Municipal Sewage ◽  
Municipal Sewage Sludge ◽  
Spectroscopy Study
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