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The STARLAB accomplishments to date include both the feasibility definition and detailed design study efforts on critical subsystems. Topics of discussion for this report include: (1) STARLAB capabilities; (2) scientific programs; (3) STARLAB technical description; (4) STARLAB Phase B studies; and (5) technical conclusions Technical recommendations.
The paper describes a 1-m high-resolution wide field-of-view telescope (Starlab) to be used on board the Space Shuttle. The purpose of Starlab is to obtain optical astronomical observations in the UV domain of the spectrum. The discussion focuses on scientific programs and technical description of the Starlab. The use of photographic film and rapid reconfiguration is possible because Starlab is flown in the Shuttle-attached mode. The Starlab uses an f/15-modified Ritchey-Chretien telescope, followed by an instrument selector that gives access to the conventional Cassegrain focus or, by inserting a diagonal mirror, to a radial focal plane. Results of five critical subsystem-design studies confirm the feasibility of using state-of-the-art design practices in meeting the Starlab science and engineering requirements.
Passive microwave techniques for geophysical probing from aircraft and space have employed frequencies 1-300 GHz and have yielded information about atmospheric temperature and composition profiles and about surface parameters such as sea state, ice and snow type and extent, soil moisture, etc. The initially scientific program is now evolving into various operational spacecraft observatory systems; this mini-review summarizes recent accomplishments and future opportunities.
The Far Ultraviolet Space Telescope (FAUST) a compact, wide field-of-view, far ultraviolet instrument designed for astronomical observations of extended and point sources is discussed. The design and application of the instrument are described. The prime objective is to observe faint astronomical sources with sensitivities higher than previously available. Scientific programs will include: (1) a search for ultraviolet stars which are predicted to exist at the stage of evolution prior to the final death of a star; (2) observations of galaxies and quasars; and (3) joint programs with other Spacelab 1 experiments. The secondary objective is to verify the suitability of the Spacelab as a platform for far ultraviolet astronomy: data will be provided on the ultraviolet background levels due to astronomical, terrestrial, and spacecraft generated sources; the levels of contaminants which affect ultraviolet instruments; and the capability of the Orbiter for stable pointing at celestial sources for useful periods of time.
The High Resoltuion Spectrograph (HRS) in conjunction with the Space Telescope (ST), extends ultraviolet astronomical spectroscopy to higher spectra, spatial, and time resolutions than previously achieved, as well as to fainter and more distant celestial objects. Other significant advances inherent in the instrument are high photometric accuracy and efficient operation via exposure meter control and real time rejection of bad data. These capabilities are provided to accomplish the scientific programs of the HRS investigation definition team, which concern the interstellar medium, stellar winds, and evolutionary aspects of stellar atmosphere studies; the determination of chemical abundances relevant to stellar evolution; the investigation of quasars and Seyfert galaxy nuclei; and the analysis of the atmospheres of solar system objects, including comets.
The scientific need and the technical feasibility of a 10-m class far infrared telescope in space were studied and culminated in the recommendation of the large deployable reflector (LDR). The scientific considerations for such a project are described and the general characteristics of LDR are derived. A scientific program culminating in LDR is suggested.
The progress which has been made in constructing a new type of X-ray telescope, which operates at normal incidence in the soft X-ray region by the use of multilayer coatings is described. The principles involved in state-of-the-art multilayer technology and some high-resolution imaging results are discussed. A rocket payload incorporating a multilayer X-ray mirror is presently being constructed. It is of Ritchey-Chretien design and the expected spatial resolution is 1/4 arcsec. The scientific program for solar-coronal studies and future instrumental developments are also discussed.
Among the topics discussed are: the political aspects of the exploration of Mars, preparatory mission scenarios in advance of manned Martian exploration, and scientific programs for a base on Mars. Consideration is also given to: mission strategies and spacecraft design for a Mars base program; concepts for the realization of a manned mission to Mars; dirigible airship applications to Martian surface exploration; and the power requirements of several Martian base designs. Additional topics include: the impact of propellant manufacturing on early manned exploration of the solar system; water supply issues for a manned Mars base; and psychological and interpersonal adaptation to life on Mars.
A change coupled device (CCD) is used in a scanning mode to find new asteroids and recover known asteroids and comet nuclei. Current scientific programs include recovery of asteroids and comet nuclei requested by the Minor Planet Center (MPC), discovery of new asteroids in the main belt and of unusual orbital types, and follow-up astrometry of selected new asteroids discovered. The routine six sigma limiting visual magnitude is 19.6 and slightly more than a square degree is scanned three times every 90 minutes of observing time during the fortnight centered on New Moon. Semiautomatic software for detection of moving objects is in routine use; angular speeds as low as 11.0 arcseconds per hour were distinguished from the effects of the Earth's atmosphere on the field of view. A typical set of three 29-minute scans near the opposition point along the ecliptic typically nets at least 5 new main-belt asteroids down to magnitude 19.6. In 18 observing runs (months) 43 asteroids were recovered, astrometric and photometric data on 59 new asteroids were reported, 10 new asteroids with orbital elements were consolidated, and photometry and positions of 22 comets were reported.
The present conference on U.S. space transportation systems development discusses opportunities for aerospace students in prospective military, civil, industrial, and scientific programs, current strategic conceptualization and program planning for future U.S. space transportation, the DOD space transportation plan, NASA space transportation plans, medium launch vehicle and commercial space launch services, the capabilities and availability of foreign launch vehicles, and the role of commercial space launch systems. Also discussed are available upper stage systems, future space transportation needs for space science and applications, the trajectory analysis of a low lift/drag-aeroassisted orbit transfer vehicle, possible replacements for the Space Shuttle, LEO to GEO with combined electric/beamed-microwave power from earth, the National Aerospace Plane, laser propulsion to earth orbit, and a performance analysis for a laser-powered SSTO vehicle.
From February 26 to March 1, 1979, 32 solar flare investigators attended a workshop at Cambridge, MA to define objectives and devise a scientific program for the study of energy release in flares (SERF) during the coming solar maximum. Herein, some major results of the ensuing five-year effort to observe and understand the flare energy release process and its effects (energetic particle production, coronal and chromospheric heating, electromagnetic radiations, and mass motions and ejections) are reviewed. The central issue - what processes store and release the energy liberated in flares - remains unresolved except in the most general terms (e.g., it is generally agreed that the energy is stored in sheared or stressed magnetic fields and released by field annihilation during some MHD instability). Resolving that issue is still one of the most important goals in solar physics, but the advances during the SERF program have brought it closer.
The Comet Nucleus Sample Return (CNSR) mission, one of the four cornerstones of the ESA scientific program, is one of the most complex space ventures within the next century, both from technological and deep space exploration point of view. In the Rosetta scenario the sample acquisition phase represents the most critical point for the global mission's success. The proposed paper illustrates the main results obtained in the context of the CNSR-SAS ongoing activity. The main areas covered are related to: (1) sample properties characterization (comet soil model, physical/chemical properties, reference material for testing); (2) concepts identification for coring, shovelling, harpooning and anchoring; (3) preferred concept (trade off among concepts, identification of the preferred configuration); and (4) proposed development activity for gaining the necessary confidence before finalizing the CNSR mission. Particular emphasis will be given to the robotic and flexibility aspects of the identified sample acquisition systems (SAS) configuration, intended as a means for the overall system performance enhancement.
A conceptual plan for the development of a comprehensive long duration solar space observatory, The Advanced Solar Observatory (ASO) is described. The ASO is intended to provide solar astronomers with the observational power necessary to address fundamental problems relating to the solar convection zone and activity cycle; the thermal and nonthermal processes that control the transport of energy, mass, and magnetic flux in the solar atmosphere; the generation of the solar wind; and the dynamics of the inner heliosphere. The ASO concept encompasses three proposed Space Station-based instrument ensembles: (1) the High Resolution Telescope Cluster, which includes far ultraviolet, extreme ultraviolet, and X-ray telescopes; (2) the Pinhole/Occulter Facility, which includes Fourier transform and coded aperture hard X-ray and gamma ray telescopes and occulted ultraviolet and visible light coronagraphs; and (3) the High Energy Facility, which contains neutron, gamma ray, and low frequency radio spectrometers. Two other facilities, the Orbiting Solar Laboratory, and a package of Global Dynamics Instrumentation, will, with the Space Station ensembles, form a comprehensive capability for solar physics. The scientific program of the ASO, current instrument concepts for the Space Station based ASO instrument ensembles, and plans for their accommodation on the Space Station are described.
Problems with the HST instantaneous imaging performance and pointing performance are discussed. Optical tests have clearly demonstrated that the HST suffers from spherical aberration. The top level specification was that 70 percent of the energy be focused in a 0.1 in. radius, but the present, and close to optimum, focus setting gives only about 16 percent. The pointing control system also is having problems with the results that the spacecraft achieves a stability of about 0.007 rms in quiescent periods, falling short of specification which requires that such performance be maintained for 24 hr. The finite guidance sensors are not guiding well on faint stars. There is a loss of sky coverage at high Galactic latitude, especially for the Wide-Field/Planetary Camera. The consequences of these defects for the scientific program are examined.
Summarized here are the activities of a one-day workshop convened to assess the effectiveness and priority setting mechanisms used by NASA's Office of Space Science and Applications in carrying out its diverse scientific programs. Among the topics discussed were strategic planning, decision making, and goal setting.
The STEP experiment is a joint ESA/NASA mission candidate for selection as the next medium science project in the ESA scientific program. ESA and NASA have undertaken a joint feasibility study of STEP. The principles of STEP and details of the mission are presented and the mission and spacecraft are described. The primary objective of STEP is to measure differences in the rate of fall of test masses of different compositions to one part in 10 exp 17 of the total gravitational acceleration, a factor of 10 exp 8 improvement in sensitivity over previous experiments. STEP constitutes a comparison of gravitational and inertial mass or a test of the weak equivalence principle (WEP). A test of WEP that is six orders of magnitude more accurate than previous tests will reveal whether the underlying structure of the universe is filled with undiscovered small forces, necessitating a fundamental change in our theories of matter on all scales.
A concise overview of the committee on Earth Observations Satellites (CEOS) and its Working Groups, covering the history and purpose of the Committee and its accomplishments to date are provided. The report will be updated annually before each Plenary meeting, and as developments in the Working Groups warrant. The committee on Earth Observations Satellites (originally named the International Earth Observations Satellite committee, IEOS) was treated in 1984, in response to a recommendation from the Economic Summit of Industrialized Nations Working Group on Growth, Technology, and Employment's Panel of Experts on Satellite Remote Sensing. This group recognized the multidisciplinary nature of satellite Earth observations, and the value of coordinating across all proposed missions. Thus, CEOS combined the previously existing groups for coordination on Ocean Remote-Sensing Satellites (CORSS) and coordination on Land Remote-Sensing Satellites (CLRSS), and established a broad framework for coordination across all spaceborne Earth observations missions. The first three LEOS Plenary meetings focused on treating and guiding the Working Groups deemed necessary to carry out the objectives of the CEOS members. After the third meeting, it was agreed that a more active orientation was required by the Plenary, and additional issues were brought before the group at the fourth meeting. At the fifth Plenary, international scientific programs and relevant intergovernmental organizations accepted invitations and participated as affiliate members of CEOS. This enabled progress toward integrating satellite data users' requirements into the CEOS process. Data exchange principles for global change research were also adopted. An interim CEOS Plenary meeting was held in April 1992, in preparation for the United Nations Conference on Environment and Development (UNCED). Brief encapsulations of the Plenary sessions immediately follow the Terms of Reference that govern the activities of CEOS as a whole; Terms of Reference for the individual Working Groups are included as Appendix A. A complete listing of CEOS members is offered as Appendix B.
The Lunar Transit Telescope (LTT), a unique, nonmoving astronomical survey telescope, is described. The autonomous operation of the soft-landed telescope is discussed and scientific programs enabled by LTT data are listed. The moon is discussed as a viable spacecraft for this mission. In particular, perturbations to the moon's stable rotation are shown to negligibly impact LTT image quality. The stable bearing properties of the lunar regolith are shown suitable for LTT support, as well. Meteoroid impacts on the telescope optics are shown to be a minor problem. A cosmic ray mitigation system which ensures data integrity is described. An opportunity for international collaboration in the reception of LTT data is proposed.