High Velocity Videoculography to Determination of the Pupil Dynamics

2008 ◽  
Author(s):  
Luís A. Villamar ◽  
E. Suaste ◽  
Gerardo Herrera Corral ◽  
Luis Manuel Montaño Zentina
Keyword(s):  
High Velocity

Galactic orbits of stars

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley
Keyword(s):  
Globular Cluster ◽  
Potential Field ◽  
High Velocity ◽  
Velocity Vector ◽  
Variable Stars ◽  
The Sun ◽  
Proper Motions ◽  
Rr Lyrae ◽  
The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

scholarly journals 9. New Spectroscopic Results on Subluminous Stars, V

1971 ◽  
Vol 42 ◽  
pp. 46-60 ◽  
Author(s):  
J. L. Greenstein
Keyword(s):  
High Velocity ◽  
Classification Scheme ◽  
Ultraviolet Excess ◽  
Horizontal Branch ◽  
Line Profiles ◽  
Hydrogen Line ◽  
Dwarf Stars ◽  
White Dwarf Stars ◽  
Halo Stars

Determination of temperature and surface gravity by colors and hydrogen-line profiles have been carried out for hot halo stars. A narrow horizontal branch is found stretching to above 40000 K; the hot O subdwarfs show a nearly vertical sequence, dropping towards the hot white dwarfs.Spectra for 285 white dwarf stars have been obtained, and the classification scheme is reviewed. Theoretical problems of these spectra remain, largely, unsolved.The red subluminous stars found by Eggen were studied spectroscopically; among 68 stars only one new red degenerate star was found. The others are very metal-poor, high-velocity stars with large ultraviolet excess.

scholarly journals The Nasa Solar Probe Mission: In Situ Determination of Interplanetary Out-of-The Ecliptic and Near-Solar Dust Environments

1991 ◽  
Vol 126 ◽  
pp. 29-32
Author(s):  
Bruce T. Tsurutani ◽  
James E. Randolph
Keyword(s):  
Solar Cycle ◽  
Solar System ◽  
Solar Eclipse ◽  
Orbital Period ◽  
High Velocity ◽  
Scientific Community ◽  
The Sun ◽  
Probe Mission

AbstractThe NASA Solar Probe mission will be one of the most exciting dust missions ever flown and will lead to a revolutionary advance in our understanding of dust within our solar system. Solar Probe will map the dust environment from the orbit of Jupiter (5 AU), to within 4 solar radii of the sun’s center. The region between 0.3 AU and 4 Rshas never been visited before, so the 10 days that the spacecraft spends during each (of the two) orbit is purely exploratory in nature. Solar Probe will also reach heliographic latitudes as high as ~ 15 to 28 above (below) the ecliptic on its trajectory inbound (outbound) to (from) the sun. This, in addition to the ESA/NASA Ulysses mission, will help determine the out-of-the-ecliptic dust environment. A post-perihelion burn will reduce the satellite orbital period to 2.5 years about the sun. A possible extended mission would allow data reception for 2 more revolutions, mapping out a complete solar cycle. Because the near-solar dust environment is not well understood (or is controversial at best), and it is very important to have better knowledge of the dust environment to protect Solar Probe from high velocity dust hits, we urgently request the scientific community to obtain further measurements of the near-solar dust properties. One prime opportunity is the July 1991 solar eclipse.

The Peru earthquake of October 17, 1966

1968 ◽  
Vol 58 (2) ◽  
pp. 645-661
Author(s):  
Cinna Lomnitz ◽  
Ramón Cabré
Keyword(s):  
Wave Energy ◽  
High Velocity ◽  
Travel Times ◽  
Direct Path ◽  
Coast Line ◽  
Isoseismal Map ◽  
Tsunami Observations ◽  
October 17 ◽  
Velocity Channel

Abstract Seismological results on the destructive Peru earthquake (M = 7.5) include: determination of epicenter, isoseismal map, tsunami observations, and some correlations between intensity and geologic factors. The epicenter was located off the coast of central Peru, about 190 kilometers northwest of Lima. Isoseismals were elongated in the direction of the coast line. The intensity exceeded VIII in the region of Huacho, and reached VII in Lima. There are indications, however, that accelerations and frequencies were both higher than would be expected in the regions for which the Modified Mercalli Scale was developed. Local high intensities were frequently correlated with the occurrence of recent alluvium. Analysis of tsunami travel times shows that the Peru Trench acts as a high-velocity channel which refracts wave energy to the coast in advance of the expected arrival over the direct path.

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