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  • 1
    Electronic Resource
    Electronic Resource
    Springer
    Colloid & polymer science 271 (1993), S. 997-1004 
    ISSN: 1435-1536
    Keywords: HLB temperature ; three-phase behavior ; microemulsions ; PIT
    Source: Springer Online Journal Archives 1860-2000
    Topics: Chemistry and Pharmacology , Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics
    Notes: Abstract The effect of monodisperse solubilities of each surfactant in an excess oil phase on the three-phase behavior was investigated in a water/octaethyleneglycol dodecyl ether (R12EO8)/tetraethyleneglycol dodecyl ether (R12EO4)/heptane system. The mid temperature of the three-phase region is defined as the HLB temperature. The HLB temperature is largely skewed to higher temperature in a dilute region due to the difference in the distribution of each surfactant between excess oil and microemulsion (surfactant) phases forming the three-phase body. Taking account of the monodisperse solubilities, the equation for the HLB temperature was obtained on the basis of geometrical calculation of a particular three-phase triangle. The equation well describes the three-phase behavior for a mixed surfactant system in a space of compositions and temperature. In the mixed surfactant system, the monodisperse solubility of R12EO8 in oil phase forming a three-phase body is monotonously increased with the rise in temperature, whereas that of R12EO4 is first increased and then is decreased. Consequently, the sum of both solubilities does not change greatly in a wide range of temperature.
    Type of Medium: Electronic Resource
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  • 2
    Electronic Resource
    Electronic Resource
    Springer
    Colloid & polymer science 105 (1997), S. 239-243 
    ISSN: 1435-1536
    Keywords: Highly concentrated emulsions ; HLB ; sucrose dodecanoate ; microemulsions ; phase behavior
    Source: Springer Online Journal Archives 1860-2000
    Topics: Chemistry and Pharmacology , Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics
    Notes: Abstract Conditions to produce highly concentrated emulsions or gel emulsions were investigated in water/sucrose dodecanoate/oil systems. HLB (Hydrophile-Lipophile Balance) of sucrose dodecanoate is changed by increasing the number of dodecane carboxylic groups attached to the sucrose ring. In order to know the correlation between the phase behavior and the formation of highly concentrated emulsions, the phase diagram of the water/mixed sucrose dodecanoate/decane system was constructed. In the sucrose monododecanoate system, the surfactant is mainly dissolved in water and forms micelles. With the increase in lipophilic chains, the sucrose surfactant tends to form reverse micelles in oil via microemulsions and lamellar liquid crystal. The formation of O/W-type and W/O-type highly concentrated emulsions is related to this phase behavior. The formation of W/O-type emulsions is enhanced upon addition of monolaurin.
    Type of Medium: Electronic Resource
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  • 3
    Publication Date: 2011-08-24
    Description: The existence of the periodic component seen in NGC 6814 with Exosat at 12,000 +/- 100 s is confirmed by a power spectrum and folded light curve analysis of unevenly sampled Ginga data. A comparison of the power spectra produced from simulated light curves with that observed enables the intrinsic shape of the power spectrum of the source to be determined despite the distortions introduced by the window function. The best estimate for the period is 12,132 +/- 3 s, where the error is that derived from simulations. An upper limit to the rate of change of period of about 10 exp -9 is inferred if the light curves are truly phase-coherent, but as this is not required by the data, the conservative upper limit is not greater than 5 x 10 exp -7. The large amount of power in the periodic component and its stability both suggest occultation of the source as its origin.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 400; 1; p. 138-152.
    Format: text
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  • 4
    Publication Date: 2011-08-24
    Description: The power spectra of the X-ray variable AGN are typically scale invariant with no characteristic timescale. The one strong exception to this is NGC 6814, where the EXOSAT data showed evidence for a periodic component at 12200 +/- 100 seconds. The power spectra of a GINGA lightcurve from this source, found using simulation techniques to account for the uneven sampling, also cannot be well fit by a single power law. A folded light curve analysis of GINGA data shows strong evidence for this periodic component. A second GINGA observation of this source taken one year later is consistent with the phenomena being completely periodic and phase coherent for 7 periods in the range of 12,110-12,145 seconds. Including the (optimistic) limits from the folding selects a period of 12130.39 +/- 0.05 seconds. Phase coherence is not maintained between this and the EXOSAT observations, as the structure of the folded light curves is very different. Thus the periodicity is long lived and stable, but phase coherence is only maintained on timescales of about 1 year.
    Keywords: ASTROPHYSICS
    Type: In: Testing the AGN paradigm; Proceedings of the 2nd Annual Topical Astrophysics Conference, Univ. of Maryland, College Park, Oct. 14-16, 1991 (A93-29801 11-90); p. 83-92.
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  • 5
    Publication Date: 2011-08-19
    Description: Simultaneous infrared, optical, ultraviolet, and X-ray observations of the low-luminosity Seyfert 1 galaxy, NGC 4051 are reported. A new method of reduction was developed to correct the optical flux for atmospheric variations due to seeing and extinction. The X-ray flux varied by factors of up to 2 on time-scales of tens of minutes, while the optical flux remained steady to within 1 percent. The results rule out all models, including Compton scattering and synchrotron models, in which a single electron population is responsible for the formation of both the infrared-to-optical and the X-ray spectra. The optical emission region must be an order of magnitude larger than, or completely separate from, the X-ray source.
    Keywords: ASTROPHYSICS
    Type: Royal Astronomical Society, Monthly Notices (ISSN 0035-8711); 243; 713-720
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