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  • 1
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    Cassini radio and plasma wave investigation - Data compression and scientific applications (1993)
    In:  Other Sources
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    Publikationsdatum: 2011-08-24
    Beschreibung: The Radio and Plasma Wave Science (RPWS) experiment being built for the Cassini spacecraft will study a wide range of plasma and radio wave phenomena in the magnetosphere of Saturn and will also make valuable measurements during the cruise phase and at other encounters. A feature of data from wave receivers is the capability of producing vastly more data than the spacecraft telemetry link is capable of transmitting back to the Earth. Thus, techniques of on-board data compression and data reduction are important. The RPWS instrument has one processor dedicated to data compression tasks.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: British Interplanetary Society, Journal (ISSN 0007-094X); 46; 3; p. 115-120.
    Format: text
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  • 2
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    Searching the SOHO online catalogs (1994)
    In:  CASI
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    Publikationsdatum: 2004-12-03
    Beschreibung: The SOHO on-line catalogs will contain information about the observations from several made or planned campaigns, that must be available to scientists who wish to use SOHO data. The World Wide Web (WWW) was chosen as the interface to the SOHO on-line catalogs, because it is easy to use, well suited to a geographically distributed user community, and freely available. Through the use of a forms-capable WWW client such as Mosaic or Lynx, a scientist will be able to browse through the catalogs of observations in a very simple, self explanatory way. Data files can then be selected from the returned lists for either immediate transferring or sending on tape by mail, with appropriate checks for whether data is in the public domain or not.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: ESA, Proceedings of 3rd SOHO Workshop on Solar Dynamic Phenomena and Solar Wind Consequences; p 429-432
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  • 3
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    Turbulent transport in the solar nebula (1990)
    In:  CASI
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    Publikationsdatum: 2013-08-29
    Beschreibung: This paper describes the current state of an ongoing project to simulate turbulent flow in a solar nebula, which is the flattened disk of dust and gas out of which a solar system forms. The goal of this project is to determine a model for the transport of mass and angular momentum in the nebula. The nebula flow exhibits compressibility, thermal conduction, viscosity, internal heating through viscous dissipation, a stable shear due to Keplerian rotation, and a gravitational acceleration in the vertical direction which is linear with altitude. These properties combine to give flow patterns not seen in terrestrial applications. Primordial solar systems are known to exist and are presumably undergoing an evolution similar to the early stages of our own solar system; for example, the IRAS infrared telescope has discovered such a protoplanetary system around the star Vega. Solar nebula evolution is the subject of much research in the astrophysical community. In the long run, researchers hope to gain a better understanding of planetary formation and the processes which dissipate the solar nebula with time.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Annual Research Briefs, 1989; p 175-184
    Format: text
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  • 4
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    Coordinated observations with high resolution spectrographs (HRTS, SERTS, MSDP) (1991)
    In:  Other Sources
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    Publikationsdatum: 2011-08-19
    Beschreibung: Some of the advantages of coordinated observations with ground-based and space instrumentation in research on prominences are examined. The dynamical behavior of a prominence in transition zone lines (HRTS) and the coronal environment of a filament (SERTS) are discussed. Fe XIV and Si X line ratios were found to be important for NE diagnostic.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: of the COSPAR 28th Plenary Meeting, The Hague, Netherlands, June 25-July 6, 1990. A91-47654 20-92) Advances in Space Research (ISSN 0273-1177); 255-258
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  • 5
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    Observations of the solar corona with a high resolution EUV imaging spectrograph (1992)
    In:  CASI
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    Publikationsdatum: 2019-06-28
    Beschreibung: An extreme ultraviolet imaging spectrograph was used to obtain coronal observations with high spectral and spatial resolution. The imaging properties of the instrument enable measurements of spectral line shapes and positions in discrete spatial elements of a region, so that the dynamic characteristics of the coronal plasma, as well as the distribution of emission measure with temperature and well known density diagnostics, can be studied for specific features. The instrumentation is described and several results of a sounding rocket flight on 5 May 1989, when the corona over NOAA Region 5464 including emission over the umbra of the region's largest sunspot and the pre-impulsive phase emission of a small flare was recorded, are summarized.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition; p 229-232
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  • 6
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    On comparing helioseismic two-dimensional inversion methods (1994)
    In:  Other Sources
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    Publikationsdatum: 2019-07-13
    Beschreibung: We consider inversion techniques for investigating the structure and dynamics of the solar interior as functions of radius and latitude. In particular, we look at the problem of inferring the radial and latitudinal dependence of the Sun's internal rotation, using a fully two-dimensional least-squares inversion algorithm. Concepts such as averaging kernels, measures of resolution, and trade-off curves, which have previously been used in the one-dimensional case, are generalized to facilitate a comparison of two-dimensional methods. We investigate the weighting given to different modes and discuss the implications of this for observational strategies. As an illustration we use a mode set whose properties are similar to those expected for data from the GONG network.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 433; 1; p. 389-416
    Format: text
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  • 7
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    Evidence for mass outflow in the low solar corona over a large sunspot (1992)
    In:  Other Sources
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    Publikationsdatum: 2019-07-12
    Beschreibung: Spatially resolved EUV coronal emission-line profiles have been obtained in a solar active region, including a large sunspot, using an EUV imaging spectrograph. Relative Doppler velocities were measured in the lines of Mg IX, Fe XV, and Fe XVI with a sensitivity of 2-3 km/s at 350 A. The only significant Doppler shift occurred over the umbra of the large sunspot, in the emission line of Mg IX (at Te of about 1.1 x 10 exp 6 K). The maximum shift corresponded to a peak velocity toward the observer of 14 +/- 3 km/s relative to the mean of measurements in this emission line made elsewhere over the active region. The magnetic field in the low corona was aligned to within 10 deg of the line of sight at the location of maximum Doppler shift. Depending on the closure of the field, such a mass flow could either contribute to the solar wind or reappear as a downflow of material in distant regions on the solar surface. The site of the source, near a major photospheric field boundary, was consistent with origins of low-speed solar wind typically inferred from interplanetary plasma observations.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X); 392; 2 Ju
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  • 8
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    Correlation of He II Lyman alpha with He I 10830 A, and with chromospheric and EUV coronal emission (1993)
    In:  Other Sources
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    Publikationsdatum: 2019-08-27
    Beschreibung: This paper describes the results of comparing Solar EUV Rocket Telescope and Spectrograph (SERTS-3) images obtained in the transition region line of He II 304 A with chromospheric He I 10830 A absorption; with strong coronal lines of Mg IX 368 A, Fe XV 284 A and 417 A, and Fe XVI 335 A and 31 A; with H-alpha; with Ca II 8542 A; and with magnetograms in Fe I 8688H-alpha. All of the images are illustrated, and the image reconstruction techniques used are described and evaluated. The high correlation of the He II 304 A and He I 10830 A images, originally found by Harvey and Sheeley (1977), is confirmed and is put on a quantitative basis. We find that the supergranulation network has greater contrast, and that filaments appear darker, in 10830 A than in 304 A. In active regions, the 304 A line follows more closely the behavior of H-alpha and Ca II 8542 A than the 10830 A line.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 147; 1; p. 29-46.
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  • 9
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    Simultaneous observations of solar plage with the solar extreme ultraviolet rocket telescope and spectrograph (SERTS), the VLA, and the Kitt Peak magnetograph (1993)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: We obtained simultaneous images of solar plage on 1991, May 7 with SERTS, the VLA,4 and the NASA/National Solar Observatory spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. Using intensity ratios of Fe XVI to Fe XV emission lines, we find that the coronal plasma temperature is (2.3-2.9) x 10 exp 6 K throughout the region. The column emission measure ranges from 2.5 x 10 exp 27 to l.3 x 10 exp 28 cm exp -5. The calculated structure and intensity of the 20 cm wavelength thermal bremsstrahlung emission from the hot plasma observed by SERTS is quite similar to the observed structure and intensity of the 20 cm microwave emission observed by the VLA. Using the Meyer (1991, 1992) revised coronal iron abundance, we find no evidence either for cool absorbing plasma or for contributions from thermal gyroemission. Using the observed microwave polarization and the SERTS plasma parameters, we calculate a map of the coronal longitudinal magnetic field. The resulting values, about 30-60 G, are comparable to extrapolated values of the potential field at heights of 5000 and 10,000 km.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 411; 1; p. 410-417.
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  • 10
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    Sources of uncertainty in direct seismological measurements of the solar helium abundance (1992)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: The methods by which Dappen et al. (1988, 1990, 1991) and Dziembowski et al. (1990, 1991, 1992) recently obtained discrepant estimates of the helium abundance in the solar convection zone are compared. The aim of the investigation reported in this paper is to identify the main source of the discrepancy. Using as proxy data eigenfrequencies of a set of modes of a theoretical solar model, computed with the same physics as were the frequencies of a reference model with which these data are compared, the two methods yield similar results. Thus we ascertain that the principal source of the discrepancy is not in the inversions themselves, which yield essentially a measure of the variation of the adiabatic exponent gamma of the material in the He II ionization zone. Instead it is in the approximations adopted in the treatment of heavy elements in the equation of state used to relate the variation of gamma to chemical composition. We obtain acceptably consistent results when inverting solar data by two methods using the same equation of state. We attempt to identify the likely residual sources of uncertainty.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Royal Astronomical Society, Monthly Notices (ISSN 0035-8711); 259; 3; p. 536-558.
    Format: text
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