Control Networks on the Galilean Satellites: Solutions for Size and Shape

A control network is a series of identifiable points on a surface and a table of their coordniates (latitude, longitude, radius). To create a planetary control network, points (usually craters) are identified on pixtures and their image coordinates are measured in pixels. Each control point must be measured on two or more images. The navigation team supplies discrete spacecraft positions and approximate camera-pointing angles. An analytical triangulation program is used to compute the coordinates of the control points and to improve the camera-pointing angles. A control network supports the compilation of maps of a particular reregion or an entire body. The maps may abe planimetric or topographic. A reference surface is used to approximate the shape of a body or to measure elevations. The reference surface is usually a sphere or spheroid, so the map can be displayd in many popular projections. Ideally, the reference surfaces for the Galilean satellites should beellipsoids, because they are in synchronous orbits and experience strong tidal forces. However, most popular projections such as Mercator, Lambert, and stereographic lose their elegant and convenient properties when the reference surface is an ellipsoid. Experiments were made to solve for the three axes as indipendent variables in the analytical triangulation. The results are of little use, as the control points are not uniformly distributed and the image resolutions vary greatly. However, the control networks can be used to study planetary shapes when combined with gravity data to constrain models of internal structure

Discovery and physical properties of Dactyl, a satellite of asteroid 243 Ida

Observations of stellar occultions by asteroids have suggested that some may have satellites. But given the absence of any confirmatory evidence, the prevailing view has been that although such satellites probably do exist, they are likely to be rare. Here we report the discovery by the Galileo spacecraft of a satellites associated with the asteroid 243 Ida. Although the satellite, Dactyl, is only 1.6 km across, it has been imaged with sufficient resolution for geological analysis. We describe the physical properties of Dactyl, with emphasis on its notably smooth shape, its crater population (which includes a crater chain) and its photometric properties. We find that, spectroscopically, Dactyl resembles both Ida and the other members of the Koronis asteroid family, implying a similar composition; small spectral differences may reflect a space weathering process that slightly alters the colours with time. We argue that Dactyl originated during the breakup of the Koronis parent body, and that satellites could be common around other asteroids (particularly members of asteroid families)

Discovery of Grooves on Gaspra

We report the discovery of grooves in Galileo high-resolution images of Gaspra. These features, previously seen only on Mars' satellite Phobos, are most likely related to severe impacts. Grooves on Gaspra occur as linear and pitted depressions, typically 100-200 m wide, 0.8 to 2.5 km long, and 10-20 m deep. Most occur in two major groups, one of which trends approximately parallel to the asteroid's long axis, but is offset by some 15 deg.; the other is approximately perpendicular to this trends. The first of extensive flat facets identified by Thomas et al., Icarus 107. The occurence of grooves on Gaspra is inconsistent with other indications (irregular shape, cratering record) that this asteroid has evolved through a violent collisional history. The bodywide congruence of major groove directions and other structural elements suggests that the present- day Gaspra is a globally coherent body

Color Variations on the Surface of Gaspra.

3-filter color images of Gaspra (0.41, 0.56 and 0.99mm) reveal that the asteroid's surface is spectrally heterogeneous, with violet/ green and IR/green ratios varying by up to 10% and 20-30% respectiv- ly. Two types of spectral variations are recognized and correlate spatially with resolvable morphologic features. (I) Approximately the small patches have anomalously high violet/green ratios and low IR/green ratios. Indicating a bluer spectral slope and enhanced matic absorption. Most of these patches correlate with small impact craters, suggesting that relativly fresh substrate is exposed. (II) Central portions of the asteroid's "facets" have high violet/ green and high IR/green ratios, indicating subdued spectral contrast and mafic absorptions. Bluer, mafic patches associated with small craters are noticeably absent from these latter regions. The spatial and spectral properties of these spectrally subdued areas are suggesttive of accumulation of optically altered. Laterally transported material on gravitationally low portions of the asteroid.We are investigating mechanisms that could produce this distinct type of spectral heterogeneity

Electroweak measurements in electron–positron collisions at w-boson-pair energies at lep

Contains fulltext : 121524.pdf (preprint version ) (Open Access

Search for Charged Higgs bosons: Combined Results Using LEP Data

The four LEP collaborations, ALEPH, DELPHI, L3 and OPAL, have searched for pair-produced charged Higgs bosons in the framework of Two Higgs Doublet Models (2HDMs). The data of the four experiments are statistically combined. The results are interpreted within the 2HDM for Type I and Type II benchmark scenarios. No statistically significant excess has been observed when compared to the Standard Model background prediction, and the combined LEP data exclude large regions of the model parameter space. Charged Higgs bosons with mass below 80 GeV/c^2 (Type II scenario) or 72.5 GeV/c^2 (Type I scenario, for pseudo-scalar masses above 12 GeV/c^2) are excluded at the 95% confidence level