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Computer controlled ground based command and data acquisition software system for OAO-A2 spacecraft remote control stations, discussing interface with monitor and interrupt capabilities
Conference on scientific observations by OAO 2 of solar system, interstellar matter, stellar atmospheres, and galactic and extragalactic systems
The celescope instrumentation and data analysis system is described, the major problems encountered during orbital operation are summerized, and a few major problems that were anticipated but did not materialize are listed.
OAO data between 2000 A and 3600 A, obtained by the Wisconsin experimental package objective grating scanning spectrometer, are used to set upper limits to the abundances of many minor constituents in the atmospheres of Mars, Jupiter, Saturn, and Venus.
A number of high-quality spectra of Mars, Jupiter, the combined disk and rings of Saturn, as well as lower-quality spectra of Venus, have been obtained with an objective-grating spectrometer of the Wisconsin Experiment Package of OAO-2. An intercomparison of the Mars, Jupiter, and Saturn spectra has failed to disclose any discrete planetary absorptions. Continuous albedos have been derived for the four planets by using OAO-2 observations of G-type stars for wavelengths greater than 2700 A. The geometric albedo of Mars shows a steady increase below 3500 A which appears to be due to Rayleigh scattering combined with a decreasing surface reflectivity. The albedos of Venus, Jupiter, and Saturn show a maximum in reflectivity in the region of 2500 A.-
This paper considers the problem of irreversible dimensional changes of the order of one thousandth of an inch per inch in several candidate materials for orbiting observatories. Although there are a number of potential sources for such dimensional changes, those given major consideration here are applied stresses and residual stresses. Results of room-temperature microyield strength (MYS) and microcreep tests to detect permanent strains associated with both short- and long-duration loading are reported for several engineering materials, including four aluminum alloys (2024, 5456, 6061, and 2014), I400 beryllium, TZM molybdenum, AZ31 magnesium, two titanium alloys (Ti-6Al-4V and Ti-5Al-2.5Sn), 321 stainless steel, a graphite/epoxy composite, and low-expansion glass ceramics. The data indicate that: metallic materials have no true elastic limit; the MYS cannot be predicted reliably from, and is appreciably less than, the conventional yield strength: significant microcreep and stress relaxation can occur at stresses somewhat below the MYS.
Review of some of the problems encountered in the development of an improved Cerenkov counter for high energy cosmic ray experiments, and discussion of the approaches used or contemplated for the solution of these problems. The solution is felt to be contingent upon a better UV-reflecting paint and an improved radiator and photomultiplier positioning.
Tests were conducted on 20-Ah sealed nickel cadmium cells to evaluate initial and long-term performance at various charge rates, temperatures and voltage-control levels. An average ampere-hour recharge of 103 percent per orbit at 13 C was able to maintain cell capacity; required watt-hour recharge on an orbital basis was 8 to 10 percent greater than required ampere-hour recharge. Cells exhibited an early life burn-in characteristic. A discharge after periods of repetitive cycling yielded two voltage plateaus which were temporarily eliminated by the discharge.
The filter photometers in the Wisconsin Experiment Package on OAO-2 were used to obtain data for a carefully selected set of 24 blue Ap stars and 31 comparison standard B and A dwarfs and giants for a program of relative photometry. Observations were made in seven bandpasses over the effective wavelength range 1430A-4250A. The Ap stars observed include members of the Si, Hg-Mn and Sr-Cr-Eu peculiarity classes. Most of them are too blue in B-V for their published MK spectral classes. The blue Ap stars are markedly deficient in emitted ultraviolet flux and are underluminous as compared to normal stars with the same UBV colors. The Hg-Mn stars appear less flux deficient in the ultraviolet for their UBV colors than do Si or Sr-cr-Eu stars. Most of the Ap stars observed possess ultraviolet flux distributions, or ultraviolet color temperatures, consistent with their published MK spectral classes to well within the classification uncertainties.
During the 16 months that the Celescope Experiment operated, it took 8000 frames of data. This report describes the experiment, the data it gathered, the format of the magnetic tape containing the data, and a number of programs that were written to read and manipulate the tape. The tape version of the catalog contains Data on 5068 stars and is available from the National Space Sciences Data Center.
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Explore the source record for details and available documents.
Far-ultraviolet photometry by OAO-2 is presented for alpha squared CVn covering the entire 5.47-day period of this magnetic Ap variable. The light curves ranging from 1330 to 3320 A indicate that there are two important sources of back warming from far-ultraviolet absorption. Strong line blanketing by the rare earths redistributes flux longward of the Balmer discontinuity, causing the major observed photometric variations. In addition, a second source, which may be due to a combination of continuous opacities and line blanketing from the iron-peak and rare-earth groups below 1600 A, apparently redistributes flux into the region of the Balmer discontinuity. It is also found that ground-based determinations of the effective temperature are overestimated due to the flux redistribution from far-ultraviolet absorption. The effective temperature of alpha squared CVn derived from OAO and ground-based absolute fluxes is found to be 11,200 K, which remains constant over the cycle.
Description of the OAO-A2 satellite and of its use in carrying out stellar measurements. The OAO-A2 is an unmanned satellite which carries two experiments, one measuring individual stars and the other measuring star fields. The OAO-A2 has the ability to point anywhere in celestial space with an accuracy of one arc minute and thus gives rise to certain operational considerations not known with other satellites. A detailed description is given of the operations control center responsible for planning and directing the overall OAO mission. The mission planning cycle and mission operations are discussed. Techniques for recovery of stellar control after loss of the stellar reference provided by the star trackers are considered. Improvements in the OAO series incorporated in the OAO-C satellite are cited.
The paper describes preflight and inflight performance checkout of the three isothermalizer heat pipes onboard the OAO-C spacecraft. The three pipes are: an axially grooved pipe, a pedestal artery pipe, and a self-priming spiral artery pipe. All pipes are 1/2-inch diameter tube rolled into a 48-inch diameter hoop. They are constructed of aluminum and use ammonia as working fluid. Periodic inflight performance checks have been made since launch in August 1972. No degradation in performance of any of the pipes has been detected. The flight data are in excellent agreement with ground test data.
Ultraviolet albedos of Mars in the region from 2000 to 3600 A are discussed. When the reflectivity due to the known amount of CO2 on Mars is accounted for, the remaining reflectivity may be used to set an upper limit for the surface albedo. The result disagrees qualitatively with published ultraviolet reflectivities of limonite and carbon suboxide. An alternate interpretation of the observations leads to the conclusion that CO2 comprises at least 60% of the molecular atmosphere of Mars, assuming the remainder to be argon. A comparison of the OAO results with 1969 Mariner ultraviolet data reveals some important areas of conflict. Attempts to detect Mars at wavelengths less than 2000 A were unsuccessful, with only very high upper limits being set.
A comprehensive ultraviolet photometric survey of the blue Ap stars was conducted in order to determine whether the close similarity, deduced from ground observations, between the blue Ap stars and normal B stars with similar UBV colors is maintained at wavelengths shortward of 3000 A. Data are presented for 24 Ap stars and 31 normal comparison standard dwarfs and giants observed by the Wisconsin Experiment Package on OAO 2. Both normal and peculiar stars were chosen, with a few exceptions, for their minimal interstellar reddening and for the absence of known bright companions. The similarity between blue Ap stars and normal B stars of similar UBV colors is not maintained in the ultraviolet. The blue Ap stars emit less ultraviolet flux than normal stars of like UBV colors. They are underluminous and cool in effective temperature for their colors.