A far ultraviolet polarization analyzer for rocket use
Far ultraviolet polarization analyzer for rocket measurement of resonantly scattered sunlight
ULTRAVIOLET LIGHT↗
SEARCH · Search NASA
Results for “RESONANCE SCATTERING”
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.
Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.
The atmosphere of Mars.
Mars atmosphere surface pressure, radiative equilibrium temperatures, sunlight resonance scattering distribution, etc
SURFACE PRESSURE↗
Discussion of an experiment to measure the polarization of dayglow Lyman alpha.
Dayglow Lyman alpha polarization measured for consistency with earth atmosphere H resonance scattering
Donahue, T. M.↗
Measurements of twilight helium 10,830 angstrom units emission.
Helium emission from resonant scattering of sunlight on upper atmosphere helium
Tinsley, B. A.↗
A far ultraviolet polarization analyzer for rocket use.
Rocket-borne far UV LiF resonantly scattered sunlight polarization analyzer, discussing optical filters spectrum division and Zeeman effect
Heath, D. F.↗
Vacuum leak detector features higher sensitivity
Technique for measuring partial pressures utilizes extremely large resonance scattering cross section of xenon at 1471 angstroms to scatter light in a vacuum cell. Output signal of ultraviolet-sensitive photodetector is proportional to the partial pressure and to the rate of inleakage of xenon probe gas.
Barrington, A. E.↗
Heavy ions from interplanetary dust.
Most atoms that are evaporated from interplanetary dust near the sun are quickly ionized and are probably carried away by the interplanetary magnetic field and the solar wind. The contribution of these heavy ions to the solar-wind flux has been estimated by using estimates of the mass required to maintain the zodiacal cloud. This contribution appears to be small compared with the heavy-ion flux of coronal origin. Many ions from dust remain singly ionized; some of these, such as Ca(+), can resonantly scatter solar radiation. The contribution of this interplanetary glow to the background of twilight glow has been estimated. Interplanetary glow may be detectable. Some atoms from dust may be accelerated by radiation pressure before being ionized. Estimates of velocities and fluxes for Fe indicate that this acceleration is not very effective.
Nakada, M. P.↗
High energy-resolution studies of electron impact optical excitation functions. I - The second positive system of N2.
The relative emission cross section for the N2 second positive system (0,0) and (1,0) bands excited by electron impact was measured for incident electron energies from threshold to 17 eV. The use of a high energy-resolution electron spectrometer coupled to an optical detection system made it possible to obtain the measurements with an incident electron beam having an energy half width of 50 meV. Calibration of the incident electron energy was provided by observing the scattering resonances in nitrogen and helium. The maximum of the (0,0) and (1,0) bands were found to be at approximately 14.02 and 14.3 eV, respectively. A small structural feature that was pressure-independent appeared only in the (0,0) band emission cross section. Another such feature was pressure-dependent and appeared more strongly in the (1,0) band cross section.
Finn, T. G.↗
Upper atmospheric probing by resonance fluorescence excited by tunable laser radiation.
Consideration of the application of the measurement of resonance fluorescence radiation excited by tunable laser radiation to the detection of atomic, molecular, and ionic species in the upper atmosphere. The species considered are N2, N2(+), NO, NO(+), O2(+), CO, CO(+), CH, Na, K, and Ca. Calculations of the resonance scattering cross sections, photon returns, and signal-to-noise ratios are given for these species for a range of conditions. Based on a probing altitude of 100 km, the detections of N2, NO, CO, CH, O2, and the trace metals appear feasible with state-of-the-art systems and within the concentration range present in the atmosphere.
Saunders, A. R.↗
Mariner 6 and 7 ultraviolet spectrometer experiment - Analysis of the O I 1304- and 1356-A emissions.
Analysis of the O I 1304- and 1356-A data from Mariner 6 and 7, and estimation of the atomic oxygen concentration of the Martian atmosphere. Derived values of the parameters describing the sources of excitation differ considerably from previous estimates. A detailed statistical treatment is used in the analysis. At an exospheric temperature of 350 K the atomic oxygen concentration at 135 km is estimated to be between 0.5 and 1%. The likely source of the 1304-A intensity is resonance scattering of solar 1304-A photons. For the 1356-A emission, the likely source is photodissociation of CO2. There is an indication of a diurnal variation of the Martian upper atmosphere.
Strickland, D. J.↗
Transfer of resonance-line radiation in differentially expanding atmospheres. II - Analytic solution for the case of coherence in the frame of the fluid.
Derivation of an exact solution for the problem of line transfer by resonant scattering (assumed coherent in the fluid frame) in a differentially expanding atmosphere. The probabilistic method developed is a generalization of the method of addition of layers plus a decomposition of the radiation field into partial radiation fields due to those photons that scatter exactly n times before escaping (n = 0, 1, 2, 3,
Noerdlinger, P. D.↗
Neutral hydrogen in cometary comas.
The strong L alpha radiation observed recently in comets Tago-Sato-Kosaka and Bennett can be explained in terms of the resonant scattering of solar L alpha radiation on neutral hydrogen formed by the photodissociation of H2O which is vaporized from a nucleus having an ice core. A complete hydrodynamic description of an atmosphere composed of H2O and its daughter products OH, H and O coupled through frictional interaction as well as production and loss processes is given. Numerical results are computed in a typical case, and it is found that a temperature of about 3000 K for the cometary atmosphere provides the best fit with observation.
Mendis, D. A.↗
Acceleration of heavy ions by radiation pressure.
The possible acceleration of heavy ions by the resonance scattering of radiation near bright stellar objects is examined. Planck spectra are assumed. At any radiation temperature, heavy-ion energies are found to be limited by aberration and Doppler effects. Photoionization is found to limit maximum radiation temperatures and energies for each ion. Collisional ionization by ambient electrons and ions may further limit heavy-ion energies. Because of these limitations, the production of the more energetic cosmic rays by this mechanism appears to be very improbable. If supernova radiation temperatures are high enough, they may produce heavy ions with energies up to several hundreds of MeV per nucleon. O and B stars appear to be able to accelerate certain heavy ions to 200 and 80 MeV per nucleon, respectively.
Nakada, M. P.↗
Air pollution measurements from satellites
A study is presented on the remote sensing of gaseous and particulate air pollutants which is an extension of a previous report. Pollutants can be observed by either active or passive remote sensing systems. Calculations discussed herein indicate that tropospheric CO, CO2, SO2, NO2, NH3, HCHO, and CH4 can be measured by means of nadir looking passive systems. Additional species such as NO, HNO3, O3, and H2O may be measured in the stratosphere through a horizon experiment. A brief theoretical overview of resonance Raman scattering and resonance fluorescence is given. It is found that radiance measurements are most promising for general global applications, and that stratospheric aerosols may be measured using a sun occultation technique. The instrumentation requirements for both active and passive systems are examined and various instruments now under development are described.
Ludwig, C. B.↗
A study of the origin, nature, and behavior of particulate matter and metallic atoms in the mesosphere, lower thermosphere, and at the mesopause
In a study of particulate matter and metallic atoms in the vicinity of the mesopause, three areas have received the most effort. These areas are: the significance of cometary dust influxes to the earth's atmosphere; the relation of nightglows to atmospheric motions and aerosols; and the feasibility of using an airborne resonant scatter lidar to study polar noctilucent clouds, the sodium layer, and fireball dust.
Poultney, S. K.↗
Coordinated analysis of airborne spectrophotometric measurements from the mid-day auroras
Measurements made in the midday auroras are analyzed and compared to measurements from the nighttime auroras. The auroral emission features in the UV spectrum, the N2(+)ING, the N22PG, and N2VK bands, are discussed. Spectral profiles of different bands are presented, and intensity distributions are obtained. Three mechanisms are suggested which can account for the marked differences between the intensity distributions of the N2(+)ING bands of the high altitude midday auroras and the low altitude nighttime auroras: (1) differences in vibrational, rotational, and transitional temperatures; (2) resonant scattering of solar radiation; and (3) excitation of slow ions.
Sivjee, G. G.↗
A study of X-ray emission from galactic and extragalactic sources with emphasis on soft and ultra-soft wavelengths
A Black Brant VC rocket was used to scan the Coma and Virgo clusters in order to measure structure in the X-ray sources. The rocket also made measurements of soft X-ray spectra, soft X-ray background flux during a 50 deg scan of the sky, soft X-rays from De Voucoulers 50, set limits to the energy dependence of soft X-ray background spectra, and the flux of solar 584 A radiation resonantly scattered by interstellar He flowing through the solar system.
Bowyer, C. S.↗
Interplanetary Lyman-beta emissions
Derivation of the intensity of the diffuse hydrogen Lyman-beta glow at 1025 A which is due to resonance scattering of the solar H I 1025 A line by interstellar and interplanetary hydrogen. Two sources of neutral hydrogen are considered: the local interstellar medium interacting with the solar system, and the dust deionization of the H(+) component of the solar wind. It is shown that if the dust geometrical factor is less than or equal to five quintillionths per cm, observations of backscattered Lyman-beta radiation will provide a unique determination of the density and temperature of the local interstellar medium.
Paresce, F.↗