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Published December 1989 | public
Journal Article Open

A sensitive time-resolved radiation pyrometer for shock-temperature measurements above 1500 K

Abstract

An optical system has been developed which can determine time-resolved temperatures in shocked materials by measuring the spectral radiance of light emitted from shocked solid samples in the visible and near-infrared wavelength range (0.5–1.0 µm). It can measure temperatures as low as 1500 K and has been successfully used to observe shock-induced chemical reactions in powder samples. The high sensitivity of this radiation pyrometer can be attributed to the large angular aperture (0.06 sr), the large bandwidth per channel (up to 0.1 µm), the large photodiode detection areas (1.0 cm^2), and the small number of calibrated channels (4) among which light is divided. Improved calibration techniques, as well as the layout of the instrument, eliminate certain sources of error encountered in previous shock-temperature experiments. Errors in the measured spectral radiance were reduced by: (1) recalibration before every experiment to account for changes in optical components; (2) direct calibration of voltage recorded at each digitizer to prevent transfer error by an intermediate step; (3) use of a spectral irradiance calibration lamp to exclude errors due to spatial inhomogeneities associated with spectral radiance sources; and (4) obtaining a large spatial average of light at each wavelength from the same portion of the sample to eliminate errors from possible inhomogeneities in the sample. The magnitude each of these errors could previously contribute was 1%–2% of the total signal. Absolute temperature uncertainties, determined from the standard deviation of the measured spectral radiances from the least-squares-fit values, are typically about 5%. Emissivities are poorly constrained by spectral radiance data because of a weak functional dependence, and uncertainties can easily exceed 50% for temperatures of around 2000 K.

Additional Information

Copyright © 1989 American Institute of Physics. Received 31 March 1989; accepted 7 August 1989. We are grateful for the advice and assistance of M. Anderson, G. Lyzenga, D. Schmitt, and R. Setchell. This work was performed at Sandia National Laboratories by DOE contract No. DE-AC04-76DP00789. It was supported at the California Institute of Technology under NASA Grant No. NGL-05-002-105 and NSF Grant No. EAR86-08249, Contribution No. 4073, Division of Geological and Planetary Sciences, California Institute of Technology.

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August 22, 2023
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