Near Infrared Absorption Spectra of Silica: OH Overtones

Elliott, C. R.; Newns, G. R.

doi:10.1366/000370271779949294

Cited by 30 publications

(5 citation statements)

References 3 publications

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“…In fused silica glass there are several references to the strength of the SiOH absorption band at 3660 cm1 (18)(19)(20)(21)(22)(23)(24)(25).…”

Section: Resultsmentioning

confidence: 99%

“…Stephenson and Jack ( 23) have been most often quoted (20)(21)(22)(23) for the value of t = 77.5 L (mol cm)"1 obtained from measurements of weight gain and loss after treatment in H20 vapor for samples on which infrared measurements had been made. Hardy (25) also found a value of e = 77 L (mol cm)"1 from weight loss measurements in fused silica.…”

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

Infrared spectrophotometric determination of hydrogen-containing impurities in silicon tetrachloride

Kometani¹,

Wood²,

Luongo³

1987

Anal. Chem.

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“…In fused silica glass there are several references to the strength of the SiOH absorption band at 3660 cm1 (18)(19)(20)(21)(22)(23)(24)(25).…”

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Infrared spectrophotometric determination of hydrogen-containing impurities in silicon tetrachloride

Kometani¹,

Wood²,

Luongo³

1987

Anal. Chem.

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“…The number of OH groups affects the transmission properties of silica due to the fundamental OH absorption band at 2.72 µm and its corresponding overtones, whose major absorption peaks are located at 1.38 µm and 0.94 µm. It is known from the literature that, as far as the 0.94 µm overtone, the OH content affects the attenuation in the order of 1-2 dB km −1 ppm −1 [30][31][32][33]. Furthermore, in Figure 1 we observe the absorption band centered at 630 nm due to DID NBOHCs [14] for both the lowand medium-OH optical fibers.…”

Section: H2 Loading and Thermal Treatmentmentioning

confidence: 66%

Radiation Effects on Pure-Silica Multimode Optical Fibers in the Visible and Near-Infrared Domains: Influence of OH Groups

et al. 2021

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Signal transmission over optical fibers in the ultraviolet to near-infrared domains remains very challenging due to their high intrinsic losses. In radiation-rich environments, this is made even more difficult due to the radiation-induced attenuation (RIA) phenomenon. We investigated here how the number of hydroxyl groups (OH) present in multi-mode (MM) pure-silica core (PSC) optical fibers influences the RIA levels and kinetics. For this, we tested three different fiber samples: one “wet”, one “dry” and one with an intermediate “medium” OH content. The RIA of the three samples was measured in the 400–900 nm (~3 eV to ~1.4 eV) spectral range during and after an X-ray irradiation at a dose rate of 6 Gy(SiO2) s−1 up to a total accumulated dose of 300 kGy(SiO2). Furthermore, we evaluated the H2-pre-loading efficiency in the medium OH sample to permanently improve both its intrinsic losses and radiation response in the visible domain. Finally, the spectral decomposition of the various RIA responses allows us to better understand the basic mechanisms related to the point defects causing the excess of optical losses. Particularly, it reveals the relationship between the initial OH groups content and the generation of non-bridging oxygen hole centers (NBOHCs). Moreover, the presence of hydroxyl groups also affects the contribution from other intrinsic defects such as the self-trapped holes (STHs) to the RIA in this spectral domain.

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“…SiO 2 displays a noticeable positive slope in the visible range and shows an overall ∼ 15 % decrease in reflectivity across the 1.2-2.5 𝜇mwavelength range. We note the presence of hydration and hydroxylation features around 1.4 𝜇m (∼ 7140 cm −1 ), 1.9 𝜇m (∼ 5250 cm −1 ), as well as around 2.2 𝜇m (∼ 4545 cm −1 ) (see Elliott & Newns 1971;Lipp 1992;Pommerol & Schmitt 2008, and references therein). It is to be noted that the samples were measured at ambient conditions.…”

Section: Cophylab Dust Spectral Propertiesmentioning

confidence: 78%

Cometary dust analogues for physics experiments

Lethuillier

Feller

Kaufmann

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The CoPhyLab (Cometary Physics Laboratory) project is designed to study the physics of comets through a series of earth-based experiments. For these experiments, a dust analogue was created with physical properties comparable to those of the non-volatile dust found on comets. This ‘CoPhyLab dust’ is planned to be mixed with water and CO2 ice and placed under cometary conditions in vacuum chambers to study the physical processes taking place on the nuclei of comets. In order to develop this dust analogue, we mixed two components representative for the non-volatile materials present in cometary nuclei. We chose silica dust as representative for the mineral phase and charcoal for the organic phase, which also acts as a darkening agent. In this paper, we provide an overview of known cometary analogues before presenting measurements of eight physical properties of different mixtures of the two materials and a comparison of these measurements with known cometary values. The physical properties of interest are: particle size, density, gas permeability, spectrophotometry, mechanical, thermal and electrical properties. We found that the analogue dust that matches the highest number of physical properties of cometary materials consists of a mixture of either 60 per cent/40 per cent or 70 per cent/30 per cent of silica dust/charcoal by mass. These best-fit dust analogue will be used in future CoPhyLab experiments.

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Near Infrared Absorption Spectra of Silica: OH Overtones

Cited by 30 publications

References 3 publications

Infrared spectrophotometric determination of hydrogen-containing impurities in silicon tetrachloride

Infrared spectrophotometric determination of hydrogen-containing impurities in silicon tetrachloride

Radiation Effects on Pure-Silica Multimode Optical Fibers in the Visible and Near-Infrared Domains: Influence of OH Groups

Cometary dust analogues for physics experiments

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