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  • 1
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    The design and evaluation of grazing incidence relay optics (1989)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: X-ray astronomy, both solar and celestial, has many needs for high spatial resolution observations which have to be performed with electronic detectors. If the resolution is not to be detector limited, plate scales in excess of 25 microns arc/sec, corresponding to focal lengths greater than 5 m, are required. In situations where the physical size is restricted, the problem can be solved by the use of grazing incidence relay optics. A system was developed which employs externally polished hyperboloid-hyperboloid surfaces to be used in conjunction with a Wolter-Schwarzschild primary. The secondary is located in front of the primary focus and provides a magnification of 4, while the system has a plate scale of 28 microns arc/sec and a length of 1.9 m. The design, tolerance specification, fabrication and performance at visible and X-ray wavelengths of this optical system are described.
    Keywords: OPTICS
    Type: Solar X-ray Astronomy Sounding Rocket Program; 6 p
    Format: application/pdf
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  • 2
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    A two-temperature model for the flare of 5 September, 1973 (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: A study of the energetics and mass transfer during the X-ray flare on Sept. 5, 1973, using the observations in the objective grating mode of the spectrographic telescope on Skylab is presented. The data are approximately monochromatic images of a small X-ray source which show a continued rise in the emission for several minutes followed by a decline. The observations are analyzed using a two-temperature model to determine the changes in the distribution of emission measure and of the amount of material as a function of temperature. The development of the flare can be divided into three periods comprising evaporation which drives mass into the entire emitting region, cessation of evaporation, and decline in the emission measure.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 65; Mar. 198
    Format: text
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  • 3
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    The location of the site of energy release in a solar X-ray subflare (1975)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: A rapid sequence of high-resolution X-ray photographs was obtained by the S-054 X-ray Telescope Experiment on Skylab on 1973 September 1. During the course of this observation, photographs were obtained of a flarelike brightening in a simple, bipolar active region. Analysis reveals the following facts. The event had the form of a small, elongated bright feature whose narrowest dimension was less than seconds of arc. The brightness peak of the flarelike brightening was located within seconds of arc of the center of brightness of a preexisting loop structure that crossed the magnetic neutral line. This loop was observed to brighten gradually beginning approximately 10 minutes prior to the flarelike event. During the rise of the event, the 2-17 A X-ray brightness of the center of the subflare core rose by over a factor of 10 in a time period of 196 seconds or less.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 199; July 15
    Format: text
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  • 4
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    The temperature and density structures of an X-ray flare during the decay phase (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The X-ray flare of 9 August 1973 was characterized by a spatially small kernel structure which persisted throughout its duration. The decay phase of this flare was observed in the objective grating mode of the X-ray telescope aboard the Skylab. Data analysis was carried out by scanning the images with a microdensitometer, converting the density arrays to energy using laboratory film calibration data and taking cross sections of the energy images. The 9 August flare shows two distinct periods in its decay phase, involving both cooling and material loss. The objective grating observations reveal that the two phenomena are separated in time. During the earlier phase of the flare decay, the distribution of emission measure as a function of temperature is changing, the high temperature component of the distribution being depleted relative to the cooler body of plasma. As the decay continues, the emission measure distribution stabilizes and the flux diminishes as the amount of material at X-ray emitting temperatures decreases.
    Keywords: SOLAR PHYSICS
    Type: Open Meetings of Working Groups on Physical Sciences; May 29, 1975 - Jun 07, 1975; Varna; Bulgaria|Symposium and Workshop on Results from Coordinated Upper Atmosphere Measurement Programs; May 29, 1975 - May 31, 1975
    Format: text
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  • 5
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    The X-ray spectrographic telescope (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The S-054 X-ray telescope, which operated successfully throughout the eight-month Skylab mission, is a grazing incidence instrument with a spatial resolution of the order of 2 arc sec on axis. The total wavelength range observed by the instrument is 2 to 60 A. Crude spectral resolution within this range is achieved by means of a series of six X-ray filter materials. A spectrographic mode of operation, employing an objective grating, is used to obtain spectra of flare events and selected coronal features.
    Keywords: SOLAR PHYSICS
    Type: Instrumentation in astronomy II; Seminar-in-Depth; Mar 04, 1974 - Mar 06, 1974; Tucson, AZ
    Format: text
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  • 6
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    An atlas of soft X-ray images of the solar corona from Skylab (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Description: An atlas is presented which contains daily full-sun photographs of the soft X-ray solar corona taken in two filters with an X-ray telescope on the Apollo telescope mount of Skylab for the period from May 29 to November 27, 1973. The passband of the first filter covers the wavelength regions from 2 to 32 A and 44 to 54 A; the second filter covers the region from 2 to 17 A. Characteristics of the instrument, the wavelength response, and sensitivity are described along with the total data base, of which the atlas represents only 1%. Comparisons are made with observations of the white-light corona, photospheric magnetic field, H-alpha radiation from the chromosphere, and 284-A Fe XV emission from the corona. A complete bibliography of scientific papers that have used the data base and a bibliography of catalogs and atlases containing related data for the same observational period are provided.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal Supplement Series; 38; Sept
    Format: text
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