Line width and inversion ratio of iron-doped rutile
Line width and inversion ratios of iron-doped rutile for optical maser applications
IRON↗
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Results for “LINE WIDTHS”
Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Measurement of multiplet intensities and noble gas-broadened line widths in the nu 3 fundamental of methane
Presented integrated intensity data at 300 K for J multiplets between P(11) and R(11) in the nu-3 fundamental of C-12 methane are shown to be in good agreement with most previously published pertinent values. Also, line widths measured at 100 K, 130 K, 190 K, 250 K, and 300 K for R(0), R(1), and R(2) broadened by He, Ne, and Ar are presented, and the line-width temperature dependence is discussed for the three cases of broadening.
Varanasi, P.↗
Contribution of thermal noise to the line width of Josephson radiation from superconducting point contacts
Contribution of thermal noise to line width of Josephson radiation from superconducting point contacts
Kamper, R. A.↗
Natural line widths of Moessbauer absorbers of variable low temperatures.
Clamping system for maintaining natural line widths of Mossbauer absorbers at varying temperatures
Dash, J. G.↗
An Empirical Expression for Line Widths of Ammonia from Far-Infrared Measurements
The hydrogen- and self-broadened line widths of 116 (sup 14)NH(sub 3) ground state transitions with J,K = 1,0 to 10,10 have been measured at 0.0006 cm(sup -1) resolution using a Bruker spectrometer between 40 to 210 cm(sup -1). These experimental widths have been reproduced to 2.4% and 11% respectively using an heuristically derived expression of the form....
remote sensing planets↗
The solar O III spectrum. II - Longer wavelengths, line widths, and the He II Lyman alpha radiation field
The solar O III spectrum above 900 A is analyzed, including several visible and infrared lines which are important in nebular studies. The dependence of the line intensities on the rate of photoexcitation by He Ly-alpha is determined, and the observability of these lines in the solar spectrum is studied. The impact approximation is employed to calculate the expected line widths of the stronger solar O III lines. The photoexciting field at 304 A calculated from the observed intensities of the O III lines below 900 A (Bhatia et al., 1982) is compared with the field predicted by a recent model (Avrett et al., 1976). It is shown that additional radiation trapping must be present beyond that given by this model.
Kastner, S. O.↗
Contribution of thermal noise to the line- width of Josephson radiation from superconducting point contacts.
Voltage-biased superconducting point contact Josephson radiation line width investigation for thermal noise contributions useful for low temperature thermometer
ELECTRIC CONTACT↗
Diatomic predissociation line widths
Predissociation by rotation and curve crossing in diatomic molecules is discussed. The pattern of predissociation line widths is seen as providing a highly sensitive yardstick for the determination of unknown potential curves. In addition, the computation of such a pattern for given potential curves is considered a matter of routine, unless the predissociation happens to occur from an adiabatic potential curve. Analytic formulas are used to provide physical insight into the details of the predissociation pattern, to the extent that a direct inversion procedure is developed for determination of the repulsive potential curves for Type 1 predissociations.
Child, M. S.↗
An estimate of line width and pressure from the high resolution spectrum of Jupiter at 11,000 angstrom units
Pressure and line width estimate from high resolution image tube spectra of Jupiter at 11,000 A
Farmer, C. B.↗
Intensity and line width measurements in the nu(u) fundamental band of (C-13)H4
Intensities and collision-broadened line widths have been measured in the nu(u) fundamental band of (C-13)H4 at 295 K, employing the Doppler-limited spectral resolution of a tunable diode laser spectrometer and a (C-13)-enriched sample of CH4, H2, He, Ar, N2, O2, and air were chosen as the broadening gases in order to provide the data needed in atamospheric and planetary atamospheric applications.
Varanasi, Prasad↗
Diode laser measurements of CO line widths at planetary atmospheric temperatures
A tunable diode laser spectrometer and the sweep integration technique were used to measure hydrogen-broadened half-widths and nitrogen-broadened half-widths of eight lines between P(1) and P(15) in the CO fundamental at several temperatures between 94 and 298 K. The results are of interest in connection with studies of the atmospheres of earth, Jupiter, Saturn, and Titan.
Varanasi, P.↗
Measurements of 2p-1s line widths in low-Z pionic atoms
High-resolution lithium-drifted silicon and germanium detectors for measuring line widths of 2p-1s transitions in low-Z pionic atoms
Harris, R. J., Jr.↗
Exciton Lifetime and Optical Line Width Profile via Exciton–Phonon Interactions: Theory and First-Principles Calculations for Monolayer MoS 2
Exciton dynamics dictates the evolution of photoexcited carriers in photovoltaic and optoelectronic devices. However, interpreting their experimental signatures is a challenging theoretical problem due to the presence of both electron–phonon and many-electron interactions. Here, we develop and apply here a first-principles approach to exciton dynamics resulting from exciton–phonon coupling in monolayer MoS 2 and reveal the highly selective nature of exciton–phonon coupling due to the internal spin structure of excitons, which leads to a surprisingly long lifetime of the lowest-energy bright A exciton. Moreover, we show that optical absorption processes rigorously require a second-order perturbation theory approach, with photon and phonon treated on an equal footing, as proposed by Toyozawa and Hopfield. Such a treatment, thus far neglected in first-principles studies, gives rise to off-diagonal exciton–phonon self-energy, which is critical for the description of dephasing mechanisms and yields exciton line widths in excellent agreement with experiment.
77 NANOSCIENCE AND NANOTECHNOLOGY↗
SDSS-IV MaNGA: calibration of astrophysical line-widths in the Hα region using HexPak observations
ABSTRACT We have re-observed $\rm \sim$40 low-inclination, star-forming galaxies from the MaNGA survey (σ ∼ 65 km s−1) at ∼6.5 times higher spectral resolution (σ ∼ 10 km s−1) using the HexPak integral field unit on the WIYN 3.5-m telescope. The aim of these observations is to calibrate MaNGA’s instrumental resolution and to characterize turbulence in the warm interstellar medium and ionized galactic outflows. Here we report the results for the Hα region observations as they pertain to the calibration of MaNGA’s spectral resolution. Remarkably, we find that the previously reported MaNGA line-spread-function (LSF) Gaussian width is systematically underestimated by only 1 per cent. The LSF increase modestly reduces the characteristic dispersion of H ii regions-dominated spectra sampled at 1–2 kpc spatial scales from 23 to 20 km s−1 in our sample, or a 25 per cent decrease in the random-motion kinetic energy. This commensurately lowers the dispersion zeropoint in the relation between line-width and star-formation rate surface-density in galaxies sampled on the same spatial scale. This modest zero-point shift does not appear to alter the power-law slope in the relation between line-width and star-formation rate surface-density. We also show that adopting a scheme whereby corrected line-widths are computed as the square root of the median of the difference in the squared measured line width and the squared LSF Gaussian avoids biases and allows for lower signal-to-noise data to be used reliably.
Chattopadhyay, Sabyasachi↗
X-ray line widths and coronal heating
Preliminary results of spectroscopy and imaging of a solar active region and flare plasma in soft X-ray emission lines are presented. Observed X-ray line widths in a nonflaring active region are broader than the Doppler width corresponding to the local electron temperature. An analysis of 41 soft X-ray flares within a single active region reveals a preference for flares to occur at locations that already show enhanced X-ray emission and to favor magnetic complexity over high gradient. However, flares do not appear to be directly responsible for the heating and X-ray production of the active regions.
Acton, L. W.↗
Average effects of large-scale convection on helioseismic line widths and frequencies
The formalism of Lavely and Ritzwoller (1992) is here applied to the model of stationary large-scale solar convection developed by Glatzmaier (1984) in order to determine a characteristic giant-cell convection signature in helioseismic data. Frequency and line-width measurements are presented on spatially filtered spectra, so that references to azimuthal orders apply to the m-value of the spatial filter's spherical harmonic. Attention is given to the 'Q-bowl' pattern of large-scale convection, a systematic, apparent line-broadening.
Lavely, Eugene M.↗
Effects of line width and spatial extent on measurements of the 0.51 MeV Galactic center line
Over the past 15 years, a number of measurements have been made of positron-electron annihilation radiation from the Galactic Center region. The results after 1979 show a significant decrease in measured flux intensity from that previously observed with the same instruments. This is probably due to time variations; however, the contributions of a spatially extended and/or energy-broadened component should also be considered. The entire data set is consistent with a time variable point source plus a distribution along the Galactic Disk. There is no strong evidence for a component broadened in energy.
Dunphy, P. P.↗
N2 pressure - broadened O3 line widths and strengths near 1129.4 cm-1
A Beer's Law experiment was performed with a tunable diode laser to find the N2 pressure broadening characteristics of a single 03 absorption line at 1129.426 cm for N2 pressures from 10 to 100 torr (O3 pressure = 3.16 torr). SO2 line positions were used for wavelength calibration. Line shapes were interatively fitted to a Lorentz function. Results were delta (HWHM in MHz) = 47.44 (+ or - 5.34) MHz + 1.730 (+ or - 0.088) MHz/torr *p(torr) with sigma = 0.9897. This intercept compares well with the Doppler O3 - O3 broadened (at 3.16 torr) width of 44.52 Hz. This result in a HWHM line width of 0.44 cm atm at 760 torr and 285 K. The line strengths integrated over delta nu = 0.55 cm were found to be N2 pressure dependent.
Copeland, G. E.↗