Effect of Temperature on the Vacuum Ultraviolet Transmittance of Lithium Fluoride, Calcium Fluoride, Barium Fluoride, and Sapphire*

Laufer, Allan H.; Pirog, J. A.; McNesby, J. R.

doi:10.1364/josa.55.000064

Cited by 80 publications

(21 citation statements)

References 12 publications

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“…The transmission spectra are not corrected for surface reflections, but it is apparent that the transmission edge is blue-shifted to 162.5 nm at 30 K. The transmission edge is defined for both temperatures as the wavelength at which the transmittance has decreased to 10%, in accordance with previous reports [16]. The blue shift is due to the decrease in the amplitude of crystal lattice vibrations at low temperature resulting from the thermal contraction of the lattice [16,17]. Operating at low temperatures would improve the transparency of Nd 3+ :LaF 3 to VUV radiation.…”

Section: Methodssupporting

confidence: 58%

Significant blue-shift in photoluminescence excitation spectra of Nd3+:LaF3 potential laser medium at low-temperature

et al. 2015

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Section: Methodssupporting

confidence: 58%

Significant blue-shift in photoluminescence excitation spectra of Nd3+:LaF3 potential laser medium at low-temperature

et al. 2015

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“…The 1165-1 resonance line emitted by krypton was filtered out by a CaF 2 window. 7 The argon resonance lamps, on the other hand, emitted the two resonance lines at 1048 and 1067 1. The 1048-1 line decreases rapidly from 40% to less than 10% of the total emission after approximately 1O!6 quanta have been transmitted through a window of LiF with a 0.5-mm thickness and 20-mm diameter.…”

Section: Methodsmentioning

confidence: 99%

“…(7) we have lim (t:.Cv/RZc) = 3PaUPooa. (7) a1-+O; t-+O These two relationships may then be solved for the two quantities pat and paaa.…”

mentioning

confidence: 99%

Gas-Phase Photolysis and Radiolysis of Cyclopropane

Scala

Ausloos

1968

The Journal of Chemical Physics

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If one desired to attempt to represent some actual experimental data by an analytical equation of state, one could proceed as follows:(1) From the coexistence curve data, determine the limiting slope of a1 2 or aa 2 versus t. This limiting slope determines -6Pat/ paaa.(2) From heat capacity data determine the discontinuity in C v at the critical point. From Eq. (7) we have lim (t:.Cv/RZc) = 3PaUPooa.These two relationships may then be solved for the two quantities pat and paaa.(3) Determine the limiting slope at the critical point of the rectilinear diameter of the coexistence curve. This limiting slope is given by4 ! (da1 da a ) 2 dt+ dt = 3pat (_ -.±. _ ! poot + ! Paaaa) . (29) paoo 15 3 pat 5 paaa (4) Determine the discontinuity in the second temperature derivative of the pressure at the critical point. With pat and Pooa known, Eqs. (19) and (29) can then be solved for poot and paaaa. These values of the four quantities pat, paaa, paat, and paooa can then be imposed on an analytical equation of state when attempting to represent experimental data by such an equation.

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“…1 of Fraser et al (1993b), the limiting ratio I p /I s in this case is 524 N. P. Bannister et al: WFAI for low Earth orbit missions ission curve for 0.5 mm thick CaF 2 filter. Data from Laufer et al (1965).…”

Section: Wfai Optic Design and Detector Requirementsmentioning

confidence: 99%

A Wide Field Auroral Imager (WFAI) for low Earth orbit missions

et al. 2007

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Abstract.A comprehensive understanding of the solar wind interaction with Earth's coupled magnetosphere-ionosphere system requires an ability to observe the charged particle environment and auroral activity from the same platform, generating particle and photon image data which are matched in time and location. While unambiguous identification of the particles giving rise to the aurora requires a Low Earth Orbit satellite, obtaining adequate spatial coverage of aurorae with the relatively limited field of view of current space bourne auroral imaging systems requires much higher orbits. A goal for future satellite missions, therefore, is the development of compact, wide field-of-view optics permitting high spatial and temporal resolution ultraviolet imaging of the aurora from small spacecraft in low polar orbit. Microchannel plate optics offer a method of achieving the required performance. We describe a new, compact instrument design which can observe a wide field-of-view with the required spatial resolution. We report the focusing of 121.6 nm radiation using a spherically-slumped, square-pore microchannel plate with a focal length of 32 mm and an F number of 0.7. Measurements are compared with detailed ray-trace simulations of imaging performance. The angular resolution is 2.7±0.2 • for the prototype, corresponding to a footprint ∼33 km in diameter for an aurora altitude of 110 km and a spacecraft altitude of 800 km. In preliminary analysis, a more recent optic has demonstrated a full width at half maximum of 5.0±0.3 arcminutes, corresponding to a footprint of ∼1 km from the same spacecraft altitude. We further report the imaging properties of a convex microchannel plate detector with planar resistive anode readout; this detector, whose active surface has a radius of curvature of only 100 mm, is shown to meet the spatial resolution and sensitivity requirements of the new wide field auroral imager (WFAI).

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Effect of Temperature on the Vacuum Ultraviolet Transmittance of Lithium Fluoride, Calcium Fluoride, Barium Fluoride, and Sapphire*

Cited by 80 publications

References 12 publications

Significant blue-shift in photoluminescence excitation spectra of Nd3+:LaF3 potential laser medium at low-temperature

Significant blue-shift in photoluminescence excitation spectra of Nd3+:LaF3 potential laser medium at low-temperature

Gas-Phase Photolysis and Radiolysis of Cyclopropane

A Wide Field Auroral Imager (WFAI) for low Earth orbit missions

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