The Pinhole/Occulter Facility is a novel instrumentation concept and will observe solar phenomena and cosmic X-ray sources with an unprecedented anzular resolution of 0.2 arc s. It achieves this by using coded-aperture imaging over a 50-m baseline, with a deployable boom used to separate an aperture mask from position-sensitive X-ray detector arrays.The existence of a remote occulting mask will make it possible to have largediameter telescopes for white-light and ultraviolet observations of the corona. These will provide qualitative improvements in sensitivity and diagnostic capability over the series of coronagraphs flown to date, giving our clearest view of 'd
Plans for the deployment of a comprehensive set of instruments designed to study the high-energy emissions of solar flares have been developed as part of a series of studies for an Advanced Solar Observatory (ASO). These studies have identified the Space Station as the preferred mode for the deployment of the full ASO. The accident of the Space Shuttle Challenger in 1986, and the growth in the estimated costs for the Space Station during the fiscal year 1989 budget discussions, have created an uncertain climate within the United States Space Program, making it difficult to predict the schedule for major programs such as the ASO. Approaches to the deployment of instruments for the study of high-energy solar emissions alone, or in conjunction with other solar instruments are discussed. As an independent entity the High-Energy Facility could be on a co-orbiting platform.
A large occulting system in space can be used for high-re solution X-ray observations and for large-aperture coronagraphic observations in visible and UV light. The X-ray observations will combine high angular resolution in hard (>10 keV) X-radiation with the high sensitivity of a multiple-pinhole camera, and will permit sensitive observations of bremsstrahlung from nonthermal particles in the corona. The large-aperture coronagraphs have two major advantages: high angular resolution and good photon collection. This will permit observations of small-scale structures in the corona for the first time and will give sufficient counting rates above the coronal background rates for sensitive diagnostic analysis of intensities and line profiles for coronal structures in the solar wind acceleration region.
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