Earth orbital space astronomy
Manned earth orbital space astronomy instruments, facilities and research objectives
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Manned earth orbital space astronomy instruments, facilities and research objectives
Research in upper air physics, radio astronomy, and rocket spectroscopy
Describing conceptual design for High Energy Astronomy Observatory spacecraft and major systems
Data displays of Radio Astronomy Explorer 1
Design and characteristics of optical system for X ray astronomy applications
Design and performance of extreme ultraviolet optical telescope for space astronomy
Performance of magnetically focused ultraviolet image converter for space astronomy
Magnesium fluoride- and lithium fluoride-optical coatings for aluminum mirror in space astronomy
High altitude sites for IR astronomy for Polar, Sub-Polar, and mid-latitudes
IR astronomy, considering basic principles, instrumentation energy production and radiation, spectroscopy, detectors and atmospheric absorption and emission
Folded all-reflecting Schmidt camera UV image converter system for space astronomy applications, discussing pressure sensitivity effects on UV direct recording emulsion
IR astronomy high altitude sites, discussing optimal geographic locations, observation conditions criteria, transportation and survival measures
X ray astronomy orthogonal mirror telescopes, noting collecting efficiency, angular resolution and focusing
Balloon X ray astronomy techniques and observations, noting collimated scintillation counter instrumentation and PCM telemetry
Space radio astronomy, discussing frequency range in terrestrial atmosphere, RAE-1 satellite, cosmic and solar emissions and magnetopause generation, propagation and absorption processes
The galactic X-ray observations are a detailed study of the temporal behavior of pulsating X-ray sources. NASA's first X-ray astronomy satellite Uhuru (Explorer 42) has recently discovered fast time variability of pulsations in the output from several sources. The variability occurs on a time scale of minutes, seconds, or less, implying that the emitting regions are very small in size, much smaller than the sun, although they are emitting about a thousand times more power. Fast time variability may provide the clue that is needed to understand the mechanisms which drive pulsating sources. The Apollo observations record the emission from several objects continuously for a period of about an hour. The spacecraft can be pointed at the source for the entire time. On the other hand, Uhuru can observe only for about a minute or two per sighting. Consequently, Apollo has the capability for determining whether periodicities exist in the 10-1000 second range.
This Project Plan for the Small Astronomy Satellite (SAS-D) is Goddard Space Flight Center's plan for accomplishing the project. It is issued in compliance with NASA Handbook NHB 7121.2 and NMI 7120.1, dated May 4, 1970, Subject: Approval and Implementation of Office of Space Science and Applications (OSSA) Research and Development (R&D) Projects. The Project Plan, as approved by GSFC executive management and NASA Headquarters, is the project manager's charter and defines his specific plan of action. System definition phase activities of the SAS-D Project will be a continuation of the analytical work that established the overall feasibility of the project. The system concept derived from that analytical work is defined in the Phase A (Mission Definition Phase) technical report. System definition phase activities will include detailed engineering analysis and preliminary breadboarding necessary to establish a single project approach from the feasible approaches. This document will be revised at the end of the system definition phase to provide greater detail on acquisition phase planning and to specify a specific system design.