Temperature Dependence of Optical Absorption Lines from Iron Atoms in a Krypton Matrix

1971 ◽  
Vol 4 (11) ◽  
pp. 3845-3848 ◽  
Author(s):  
H. Micklitz ◽  
P. H. Barrett
Keyword(s):  
Optical Absorption ◽  
Temperature Dependence ◽  
Absorption Lines

Formation Energy of Interstitial Si in Au-Doped Si

1998 ◽  
Vol 510 ◽  
Author(s):  
Masashi Suezawa
Keyword(s):  
High Temperature ◽  
Optical Absorption ◽  
Temperature Dependence ◽  
Absorption Spectra ◽  
Formation Energy ◽  
Hydrogen Atmosphere ◽  
Absorption Lines ◽  
Optical Absorption Spectra ◽  
Vapor Method

AbstractIn this report, we proposed that complexes responsible for optical absorption lines in Si grown in a hydrogen (H) atmsophere were composed of interstitial Si and H atoms and then determined the formation energy of interstitial Si in Au-doped Si from the measurements of optical absorption due to H bound to interstitial Si. In the first experiment, specimens were grown in a hydrogen atmosphere. In the second experiment, Si crystals were doped with Au by a vapor method; namely, specimens were sealed in quartz capsules together with a piece of Au wire and then annealed at high temperature followed by quenching in water. Then the specimens were doped with H by annealing them in hydrogen atmosphere of 1 atm. followed by quenching. We measured optical absorption of those specimens. From the effect of impurity on the optical absorption spectra of Si grown in a hydrogen atmosphere, we concluded that those optical absorption lines, including 2223 cm−1line, were due to complexes of interstitial Si and H. From the temperature dependence of the intensity of 2223 cm−1line, the formation energy of interstitial Si in Au-doped Si was determined to be about 2.1 eV

OPTICAL ABSORPTION SPECTRA OF ARSENIC AND PHOSPHORUS IN SILICON

1962 ◽  
Vol 40 (10) ◽  
pp. 1480-1489 ◽  
Author(s):  
J. W. Bichard ◽  
J. C. Giles
Keyword(s):  
Optical Absorption ◽  
Absorption Spectra ◽  
Excited States ◽  
Ground State ◽  
Absorption Lines ◽  
Full Width ◽  
Optical Absorption Spectra ◽  
Phosphorus Impurity ◽  
Line Widths ◽  
Phosphorus In Silicon

The optical absorption spectra of arsenic and phosphorus donor impurities in silicon have been studied under conditions of improved resolution. Absorption lines due to transitions from the impurity ground state to the excited states 2p0, 2p±, 3p0, 3p±, 4p0, 4 p±, and 5p0, and 5p± have been observed at 4.2° K. The relative intensities of some of these absorption lines are compared with existing experimental and theoretical estimates. The contribution of instrumental broadening to the observed line widths is assessed and natural line widths are estimated. The estimates indicate values for the natural line widths which are much less than those previously reported. For phosphorus impurity, the natural line widths are estimated to be less than 0.08 × 10−3 electron volts full width at half-maximum. The possibility of concentration broadening is discussed in connection with the arsenic data.

Article

1998 ◽  
Vol 76 (4) ◽  
pp. 411-413
Author(s):  
Yixing Zhao ◽  
Gordon R Freeman
Keyword(s):  
Absorption Spectrum ◽  
Optical Absorption ◽  
Temperature Dependence ◽  
Optical Absorption Spectrum ◽  
Infrared Light ◽  
Solvated Electron ◽  
Solvated Electrons ◽  
Tert Butanol ◽  
Solvent Dependence ◽  
Increasing Temperature

The energy and asymmetry of the optical absorption spectrum of solvated electrons, es- , change in a nonlinear fashion on changing the solvent through the series HOH, CH3OH, CH3CH3OH, (CH3)2CHOH, (CH3)3COH. The ultimate, quantum-statistical mechanical, interpretation of solvated electron spectra is needed to describe the solvent dependence. The previously reported optical spectrum of es- in tert-butanol was somewhat inaccurate, due to a small amount of water in the alcohol and to limitations of the infrared light detector. The present note records the remeasured spectrum and its temperature dependence. The value of the energy at the absorption maximum (EAmax) is 155 zJ (0.97 eV) at 299 K and 112 zJ (0.70 eV) at 338 K; the corresponding values of G epsilon max (10-22 m2 aJ-1) are 1.06 and 0.74. These unusually large changes are attributed to the abnormally rapid decrease of dielectric permittivity of tert-butanol with increasing temperature. The band asymmetry at 299 K is Wb/Wr = 1.8.Key words: optical absorption spectrum, solvated electron, solvent effects, tert-butanol, temperature dependence.

scholarly journals The Absorption Line Systems of the Supershell LMC2 in the Large Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 154-155
Author(s):  
Adeline Caulet
Keyword(s):  
Optical Absorption ◽  
Interstellar Medium ◽  
Gas Phase ◽  
Absorption Line ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Absorption Lines

The interstellar medium of LMC2, a well studied supershell in the Large Magellanic Cloud, has been probed in UV and optical absorption lines. The data allow to derive the kinematics, abundances and depletions of gas clouds in this supershell. The relative gas-phase abundances of observed elements with respect to sulphur are useful to determine the origins of the supershell absorption-line clouds.

scholarly journals Sub-milliarcsecond Radio Structure of AO 0235+164

1984 ◽  
Vol 110 ◽  
pp. 47-48
Author(s):  
Dayton L. Jones ◽  
Mike M. Davis ◽  
Steve C. Unwin
Keyword(s):  
Optical Absorption ◽  
Flux Density ◽  
Radio Spectrum ◽  
Absorption Lines ◽  
Radio Structure ◽  
Spectrum Radio ◽  
Bl Lac ◽  
Line Redshift ◽  
To Come ◽  
Absorption Frequencies

AO 0235+164 is a very compact, flat-spectrum radio source. It is identified with a BL Lac object, and has optical absorption-line systems at z = 0.524 and z = 0.852. A complex set of HI absorption lines is seen at z = 0.524 (932 MHz), and several of these lines change significantly in depth over periods of less than a year. This is the only known case of variable extragalactic absorption lines. A faint nebulosity 2 arcsec south of AO 0235 + 164 has an emission-line redshift of z = 0.52 and may be an intervening galaxy. The radio spectrum of this source (between major outbursts) is remarkably flat, with the total flux density staying between about 1 and 3 Jy over a range of at least 1000 in frequency. Such a flat spectrum would lead one to expect a complex, wavelength-dependent structure consisting of several components with different self-absorption frequencies. However, the observed radio structure of 0235+164 is about as simple as one could imagine – it is a nearly unresolved point source in VLBI experiments from 900 MHz to 22 GHz. Recent VLBI experiments at 6 and 13 cm have shown evidence for some elongation of the source in a generally NE-SW direction, but only at low contour levels (< 15% of the peak). The major portion of the flux density appears to come from a core which is unresolved in VLBI experiments over a range of ~ 25 in frequency.

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