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  • 1
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    On the possibly overluminous triple star, 13 Ceti (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: The star system, 13 Ceti, consists of a short-period visual binary whose primary is itself a single-line spectroscopic binary. Currently existing data regarding the considered stellar system are examined, taking into account certain discrepancies. It is pointed out that the spectral type of the combined light of the system complicates any attempt to explain the observed overluminosity in terms of stellar evolution. Additional studies are recommended to clarify remaining questions concerning the characteristics of the stellar system.
    Keywords: ASTROPHYSICS
    Type: Astronomical Society of the Pacific; vol. 88
    Format: text
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  • 2
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    Chemistry between the stars (1976)
    In:  CASI
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    Publication Date: 2019-08-27
    Description: A unit is presented for the secondary school teacher of physics, chemistry, astronomy, or earth sciences. Included are a list of reference materials, teaching aids, and projects. Discussion questions and a glossary are also provided. Concepts developed are: the nature of interstellar space, spectroscopy, molecular signals from space and interstellar molecules and other areas of astronomy.
    Keywords: ASTROPHYSICS
    Type: NASA-EP-127
    Format: application/pdf
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  • 3
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    Evolution of the Solar System (1976)
    In:  CASI
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    Publication Date: 2019-08-27
    Description: The origin and evolution of the solar system are analyzed. Physical processes are first discussed, followed by experimental studies of plasma-solid reactions and chemical and mineralogical analyses of meteorites and lunar and terrestrial samples.
    Keywords: ASTROPHYSICS
    Type: NASA-SP-345
    Format: application/pdf
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  • 4
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    Effects of tidal distortion on binary-star velocity curves and ellipsoidal variation (1976)
    In:  Other Sources
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    Publication Date: 2019-08-27
    Description: Radial velocity curves for the more massive components of binaries with extreme mass ratios can show a large distortion due to tides, as first recognized by Sterne. Binaries in which the effect is large should be rare because nearly all such binaries would be in the rapid phase of mass transfer. However, the optical counterparts of some X-ray binaries may show the effect, which would then serve as a new means of extracting considerable information from the observations. The essential parts of the computational procedure are given. Light curves for ellipsoidal variables with extreme mass ratios were also computed, and were found to be less sinusoidal than those with normal mass ratios.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; 203; Jan. 1
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  • 5
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    A survey of mass-loss effects in early-type stars (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Intermediate-resolution data obtained with the Copernicus satellite are surveyed in order to define the region in the H-R diagram where mass loss occurs. The survey includes 40 stars, providing good coverage of supergiants from O4 to A2 and main-sequence stars from O4 to B7 as well as spotty coverage of late O giants and intermediate to late B stars. The spectral transitions examined are primarily resonance lines of ions of abundant elements plus some lines arising from excited states (e.g., C III at 1175.7 A and Si IV at 1122.5 A). Observed P Cygni profiles are discussed along with interesting features of some individual profiles. The data are shown to indicate that mass-loss effects occur over a wide portion of the H-R diagram, that mass ejection generally occurs when the holometric magnitude is greater than -6.0, and that the mass-ejection rate is usually high enough to produce P Cygni profile whenever the N V feature at 1240 A is present in a spectrum.
    Keywords: ASTROPHYSICS
    Type: European Astronomical Meeting on Stars and galaxies from observational points of view; Jul 01, 1975 - Jul 05, 1975; Tiflis; Georgian SSR
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  • 6
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    Mass flow in close binary systems (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The manner of mass flow in close binary systems is examined with a special view to the role of the so-called critical Roche (or Jacobian) lobe, taking into consideration relevant physical conditions such as radiation pressure that may affect the restricted three-body problem treatment. The mass does not necessarily flow from component one to component two through the L1 point to form a gaseous ring surrounding the latter. These considerations are applied to X-ray binaries with early-type optical components, such as Cyg X-1 (HDE 226868) and 3U 1700 - 37 (HD 153919). In the two bright close binary systems Beta Lyr and UW CMa, which are believed to be undergoing dynamic mass transfer, recent Copernicus observations show that the gas giving rise to the prominent ultraviolet emission lines surrounds the entire binary system rather than merely component two. Implications of these observations are also discussed.
    Keywords: ASTROPHYSICS
    Type: Symposium on Structure and evolution of close binary systems; Jul 28, 1975 - Aug 01, 1975; Cambridge
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  • 7
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    Binary X-ray stars and supernovae of type I (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Most of the strong galactic X-ray sources must be low-mass close binary systems, such as Her X-1 and Sco X-1. Two evolutionary scenarios are discussed, both involving type I supernovae that occur when mass-accreting white dwarfs are driven over their mass limit. In one, accepting the correctness of the idea that a neutron star or black hole is the seat of the X-ray emission, the SN occurs before the system is an X-ray source. Another possibility is that the white dwarf is the X-ray source, just prior to its collapse and the ensuing SN.
    Keywords: ASTROPHYSICS
    Type: Symposium on Structure and evolution of close binary systems; Jul 28, 1975 - Aug 01, 1975; Cambridge
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  • 8
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    A survey of mass loss from Be and shell stars using ultraviolet data from Copernicus (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Ultraviolet spectra of intermediate resolution have been obtained with Copernicus of twelve objects classified as Be or shell stars, and an additional 19 dwarfs of spectral classes B0-B4. Some of these spectra show marked asymmetries in certain resonance lines, especially the Si IV doublet at 1400 A, indicating the presence of outflowing material with maximum velocities of nearly 1000 km/sec. Direct evidence for mass loss at these velocities is seen for the first time in dwarf stars as late as B1.5. Later than B0.5, the only survey objects showing this phenomenon are Be stars. Among the stars considered there is a correlation between the presence of mass-loss effects and projected rotational velocity, suggesting that the UV flux from B1-B3 dwarfs is sufficient to drive high-velocity stellar winds only if rotation reduces the effective gravity near the equator. The role of mass-loss in producing the Be star phenomenon and the effects of rotation on mass loss are discussed.
    Keywords: ASTROPHYSICS
    Type: Merrill-McLaughlin Memorial Symposium; Sep 15, 1975 - Sep 18, 1975; Bass River, MA
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  • 9
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    Rotational bursting of interplanetary dust particles (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Rotationally induced bursting of interplanetary dust particles by a windmill effect stemming from solar radiation pressure, and eventual elimination of the particles from the solar system, is discussed. A life span on the order of 100,000 years for stony meteoritic material or tektite glass with radii of about 1 cm is arrived at for this process. A life span of a million years is computed for particles containing Fe, Ni, or Al with spin damping effects taken into cognizance. This depletion mechanism operates at a rate two orders of magnitude greater than that of the Poynting-Robertson effect in the case of nonmetallic particles and one order of magnitude greater in the case of metallic particles.
    Keywords: ASTROPHYSICS
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
    Format: text
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  • 10
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    Radial distribution of meteoric particles in interplanetary space (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The heliocentric distribution of meteoric particles in interplanetary space is derived, with consideration of the Poynting-Robertson effect, interparticle collision processes and cometary dust injection. Radial distribution functions were derived for zodiacal dust, radar meteors and the meteoroids of mass 10 to the -9th to about 10 to the -10th g (normalized to 1 AU). The number density was found to depend on particle size.
    Keywords: ASTROPHYSICS
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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