Radio astronomy
Radio astronomical studies of microwave spectrum, radial velocity, dielectric constants, and emissions
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Results for “RADIAL VELOCITY”
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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On the remarkable spectroscopic complexities of Cyg X-2.
Cyg X-2 radial velocity variation measured from Ca II, He II and Ca I absorption lines
Demoulin, M.-H.↗
Discrepancies between radar data and the lunar ephemeris.
Eckert-Brown lunar ephemeris predictions discrepancies with radar data of radial velocities
Pettengill, G. H.↗
Optical and radio evidence of large-scale peculiar motions in the Cassiopeia-Perseus arm.
Cassiopeia-Perseus spiral arm shown to contain interstellar medium moving with peculiar radial velocity on basis of optical and radio observation
Rickard, J. J.↗
Wavelength errors in spectrographs. I - The effect of surface irregularities in camera mirrors.
Radial velocity errors in high dispersion astronomical spectrographs in terms of variable spectral shifts along plate produced by mirror surface irregularities
Tull, R. G.↗
Gas turbine combustor insensitive to compressor outlet distortion
Short-length annular combustor for turbojet engines eliminates change of exit temperature profile. Individual scoops of full annular height control air distribution so that shifts in the radial velocity profile of air entering the combustor will not affect combustion process or alter exit temperature profile.
Humenik, F.↗
Plasma velocity measurements by Abel-unfolding of Doppler shifts
Cylindrical axial plasma flow fields velocity radial dependence measurement by double-wedge spectroscopy using Abel unfolding of Doppler shifts
Ahlborn, B.↗
Observations of water-vapor emission associated with infrared stars
Water vapor emission detection from IR stars, discussing radial velocities of microwave lines
Barrett, A. H.↗
Concerning a proposed test for the expansion of clusters of galaxies
Galaxy cluster expansion theory, noting dispersion in radial velocities of members
Noerdlinger, P. D.↗
Dynamics of the Perseus cluster of galaxies
Radio observation for radial velocities in center region of Perseus cluster of galaxies
Chincarini, G.↗
Kinematics of the Huygenian region of the Orion nebula
The nebular (O II) lambda 3726 and (O III) lambda 5007 radial velocity measures of Wilson, et al (1959) are presented in contour map form. The space motions of theta 1 and theta 2 Orionis and the nebular measures are discussed.
Fischel, D.↗
Rocket spectroscopy of zeta Orionis.
Analysis of a spectrum of zeta Ori extending from 922 to 1453 A with approximately 0.8 A resolution recorded at rocket altitudes. All lines used in existing models of stellar atmospheres appear in the recorded spectrum with the exception of those masked by telluric N2 or strong P Cygni-type profiles and by an O V line at 1371.29 A. Fifteen multiplets of subordinate lines have been reliably identified, indicating an approximate range of excitation from 0 to 50 eV. Transitions in C III (1176 A), N III (991 A), N V (1239, 1243 A), O VI (1032, 1038 A), Si IV (1394, 1403 A), S IV (1063, 1074 A), and S VI (933, 944 A) have been observed as P Cygni-type profiles presumably arising in a circumstellar envelope. The degree of ionization, transitions present, and mean radial velocities are all consistent with viewing the envelope as a hot (about 100,000 K), rarefied plasma in which collisional ionization is important. Interstellar lines in C I (1277, 1280 A), C II (1036, 1334 A), N I (1134-1135 A), N I (1200-1201 A), N II (1084-1086 A), O I (1302, 1305 A), Si II (1190, 1193 A), Si II (1260 A), and Si II (1304 A) have been definitely identified. Other transitions in Ar II, S I, C I, and Fe II are tentatively identified. The equivalent width of the L alpha line is found to be 10.4 plus or minus 1.6 A, corresponding to a columnar density of 2.0 plus or minus 0.7 x 10 to the 20th per cu cm.
Smith, A. M.↗
The configuration of the interplanetary magnetic field.
The idealized basic structure of the interplanetary magnetic field is the familiar spiral wound on a cone whose axis is the solar rotation axis. Variations in the radial velocity of the solar wind produce large scale variations in pitch; slight distortions are also produced by the nonradial component of the solar wind velocity. The high velocity streams in the solar wind seem to be more significant than magnetic polarity alternation in the sector structure of the interplanetary medium. Superposed on the ideal spiral are a variety of smaller structures. Outwardly propagating nonsinusoidal Alfven waves with scale lengths of .1 to 10 million kilometers are common. When sharp crested, they are recognized as rotational discontinuities. Other, less easily identified, waves are present part of the time. Tangential discontinuities and other convected structures have been identified, as have interplanetary shock waves.
Davis, L., Jr.↗
The structure of the coma cluster of galaxies.
Analysis of radial velocities in the coma cluster (many of them new) in conjunction with previous data on the density distribution. The cluster extends more than 200 min in radius, with bright and faint galaxies distributed in nearly the same way. Some spirals are members. Several different determinations of M/L give values around 250. The cluster is stabilized by a 'missing mass' some seven times the mass of the galaxies, which must be distributed in the same way as the galaxies.
Rood, H. J.↗
Nearly spherical constant power detonation waves driven by focused radiation
Shape and inner flow of a tridimensional spark are studied. The spark is created by focusing a laser beam in a gas. A second order fully non-linear equation is derived for the radial velocity on the axis of symmetry in the neighborhood of the origin. Solutions to that equation display the existence of a forbidden region near the focus, thus indicating the limits of applicability of a small perturbation solution.
George, Y. H.↗
Low-intensity optical emissions from the interstellar medium
Spectrometric scans of faint optical emissions from interstellar gas are reported. Systematic variations along the galactic plane in both the intensity and radial velocity of the galactic H alpha suggest that the diffuse emission is strongly associated with three nearby galactic spiral arms.
Reynolds, R. J.↗
Visualization study of flow in axial flow inducer.
A visualization study of the flow through a three ft dia model of a four bladed inducer, which is operated in air at a flow coefficient of 0.065, is reported in this paper. The flow near the blade surfaces, inside the rotating passages, downstream and upstream of the inducer is visualized by means of smoke, tufts, ammonia filament, and lampblack techniques. Flow is found to be highly three dimensional, with appreciable radial velocity throughout the entire passage. The secondary flows observed near the hub and annulus walls agree with qualitative predictions obtained from the inviscid secondary flow theory.
Lakshminarayana, B.↗
Development of flow in the entrance region of a converging channel.
An approximate solution for the laminar flow of an incompressible viscous fluid in the entrance region of a converging channel is obtained. The radial velocity distribution at the entrance of the channel is taken to be a symmetric but otherwise arbitrary function of the angular position. Expressions for the velocity components and pressure are given. The case of the uniformly distributed entrance velocity is considered as an example.
Atabek, H. B.↗