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  • 1
    Electronic Resource
    Electronic Resource
    New York, NY [u.a.] : Wiley-Blackwell
    Biotechnology and Bioengineering 34 (1989), S. 1114-1125 
    ISSN: 0006-3592
    Keywords: Chemistry ; Biochemistry and Biotechnology
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Biology , Process Engineering, Biotechnology, Nutrition Technology
    Notes: Altered phosphorus concentration, oxygen supply rate, and programmed addition of sucrose and phosphorus were applied to Dioscorea deltoidea plant cells in airlift suspension to increase the formation of the secondary metabolite diosgenin. A low oxygen supply rate (kla′ of 3.9 h-1) completely inhibited formation of diosgenin. A high oxygen supply rate (kla′ of 17.1 h-1) led to the greatest formation of diosgenin in 30 g/L sucrose when the sucrose-to-phosphorus mole ratio was 42.5:1. Programmed addition of nutrients over a 15-day period reduced growth of cell mass relative to diosgenin mass. Intentional aggregation by entrapment of virtually all cells in reticulated polyurethane foam led to reduced cell-mass yield, diosgenin yield and concentration relative to suspended cells at the same conditions. Entrapment of a small fraction of the cells led to a delayed development of a suspension culture and to formation of significantly higher concentrations of diosgenin. Nearly all of this increase was attributable to the suspended cells. This result suggested sequestering of nonproductive cells by the matrix or sequestering of important nutrients by the matrix-bound cells. Entrapped cells attained densities of 40 g/L in the matrix.
    Additional Material: 10 Ill.
    Type of Medium: Electronic Resource
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  • 2
  • 3
    Publication Date: 1964-07-06
    Print ISSN: 0031-899X
    Electronic ISSN: 1536-6065
    Topics: Physics
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  • 4
    Publication Date: 1984-12-01
    Print ISSN: 0004-637X
    Electronic ISSN: 1538-4357
    Topics: Physics
    Published by Institute of Physics
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  • 5
    Publication Date: 2011-08-24
    Description: The detection of terrestrial-sized extrasolar planets from the ground has been thought to be virtually impossible due to atmospheric scintillation limits. However, we show that this is not the case especially selected (but nevertheless main sequence) stars, namely small eclipsing binaries. For the smallest of these systems, CM Draconis, several months to a few years of photometric observations with 1-m-class telescopes will be sufficient to detect the transits of any short-period planets of sizes 〉 or = 1.5 Earth radii (RE), using cross-correlation analysis with moderately good photometry. Somewhat larger telescopes will be needed to extend this detectability to terrestrial planets in larger eclipsing binary systems. (We arbitrarily define "terrestrial planets" herein as those whose disc areas are closer to that of Earth's than Neptune's i.e., less than about 2.78 RE.) As a "spin-off" of such observations, we will also be able to detect the presence of Jovian-mass planets without transits using the timing of the eclipse minima. Eclipse minima will drift in time as the binary system is offset by a sufficiently massive planet (i.e., one Jupiter mass) about the binary/giant-planet barycenter, causing a periodic variation in the light travel time to the observer. We present here an outline of present observations taking place at the University of California Lick Observatory using the Crossley 0.9-m telescope in collaboration with other observatories (in South Korea, Crete, France, Canary Islands, and New York) to detect or constrain the existence of terrestrial planets around main sequence eclipsing binary star systems, starting with CM Draconis. We demonstrate the applicability of photometric data to the general detection of gas giant planets via eclipse minima timings in many other small-mass eclipsing binary systems as well.
    Keywords: Exobiology
    Type: Journal of geophysical research (ISSN 0148-0227); Volume 101; E6; 14823-9
    Format: text
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  • 6
    Publication Date: 2011-08-19
    Description: Various methods outlined for indirect planetary detection would greatly benefit (in some cases require) the determination of the planetary orbital plane, which is theoretically equivalent to the stellar equatorial plane. Determining the stellar space orientation, therefore, would greatly benefit extrasolar planetary detection. Stellar rotation periods determined from short-term variations in Ca II H and K sunspot emission are utilized together with both stellar radii measurements and Doppler-broadened spectral line profiles to get the stellar inclination to the line of sight. The clocklike on-the-plane-of-the-sky component determination utilizes the concentration of sunspot-associated plage areas at central stellar latitudes when viewed in Ca II H or K emission. One can perform Ca II H and K emission speckle interferometry to measure the clocklike angle of this stellar Ca II H and K emission band, modeling it as an elliptical intensity distribution. Both components should be determinable to within 10 deg for at least the resolvable fifth magnitude stars.
    Keywords: ASTROPHYSICS
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  • 7
    Publication Date: 2013-08-31
    Description: The element lithium is observed to be underabundant in the Sun by a factor of approx. equal to 100. To account for this depletion, Boothroyd et al. (Ap. J., in press 1991) proposed a model in which the Sun's zero-age-main-sequence mass was approx. 1.1 solar magnitude. If this is the explanation for the lithium depletion, then astronomical observations of F/G dwarfs in clusters suggest that the timescale for mass loss is approx. equal to 0.6 Gyr. Assuming this approximate timescale, the authors investigated several planetological implications of the astrophysical model.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Abstracts for the International Conference on Asteroids, Comets, Meteors 1991; p 238
    Format: application/pdf
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  • 8
    Publication Date: 2013-08-31
    Description: Global mean temperatures near 273 K on early Mars are difficult to explain in the context of standards solar evolution models. Even assuming maximum CO2 greenhouse warming, the required flux is approximately 15 percent too low. Here we consider two astrophysical models that could increase the flux by this amount. The first model is a nonstandard solar model in which the early Sun had a mass somewhat greater than today's mass (1.02-1.06 solar mass). The second model is based on a standard evolutionary solar model, but the ecliptic flux is increased due to focusing by an (expected) heavily spotted early Sun.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Workshop on Early Mars: How Warm and How Wet?, Part 1; p 23
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  • 9
    Publication Date: 2011-08-19
    Description: Near-infrared images of Venus, obtained from a global network of ground-based observatories during January and February 1990, document the morphology and motions of the night-side near-infrared markings before, during, and after the Galileo Venus encounter. A dark cloud extended halfway around the planet at low latitudes and persisted throughout the observing program. It had a rotation period of 5.5 + or - 0.15 days. The remainder of this latitude band was characterized by small-scale (400 to 1000 km) dark and bright markings with rotation periods of 7.4 + or - 1 days. The different rotation periods for the large dark cloud and the smaller markings suggest that they are produced at different altitudes. Midlatitudes (+ or - 40 to 60 deg) were usually occupied by bright east-west bands. The highest observable latitudes (+ or - 60 deg to 70 deg) were always dark and featureless, indicating greater cloud opacity. Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 253; 1538-154
    Format: text
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  • 10
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    In:  Other Sources
    Publication Date: 2011-08-19
    Description: Stellar rotation periods recently determined from short-term variations in Ca II H and K emission-line flux associated with starspot activity can be combined with both rotational spectral-line-broadening velocity measurements and independent measurements of stellar radii to give the inclination of the star's rotation axis to the line of sight. Assuming that the limits of distribution of sunspots on the sun apply similarly to solar-type stars, interferometric measurements of stellar radii in Ca II H and K flux may be performed to determine the clock-like, on-the-plane-of-the-sky orientation as well. Various stellar-radius measuring techniques are discussed, and photon limits on the measurability of this latter parameter are derived for Ca II H and K speckle interferometry. The accuracy with which the space orientation of stars can be determined is discussed in the context of existing data as well as photon limits. The importance of determining the space orientation of stars is then discussed, with emphasis on its important application to the present search for extrasolar planetary systems.
    Keywords: ASTRONOMY
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 287; 307-314
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