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  • 1
    Electronic Resource
    Electronic Resource
    Interactions between fullerene (C60) and endohedral alkali atoms (1992)
    s.l. : American Chemical Society
    The @journal of physical chemistry 〈Washington, DC〉 96 (1992), S. 9781-9787 
    Details
    Source: ACS Legacy Archives
    Topics: Chemistry and Pharmacology , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1021/j100203a038
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  • 2
    Electronic Resource
    Electronic Resource
    Electron bound states near a charged dielectric sphere (1986)
    College Park, Md. : American Institute of Physics (AIP)
    The Journal of Chemical Physics 85 (1986), S. 5204-5206 
    Details
    ISSN: 1089-7690
    Source: AIP Digital Archive
    Topics: Physics , Chemistry and Pharmacology
    Notes: We have calculated the binding energies for electron states which are localized just outside of the surface of a (liquid) dielectric sphere in which a positive ion impurity is dissolved. The model considers four quantities: the static and optical dielectric constants of the liquid, the conduction band minimum in the liquid, and the radius of the sphere. We find that surface states are possible for water and ammonia but for argon the ion is not sufficiently screened to permit surface states.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.451684
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  • 3
    Electronic Resource
    Electronic Resource
    Emergence of magnetic flux on the Sun as the cause of a 158-day periodicity in sunspot areas (1998)
    [s.l.] : Macmillan Magazines Ltd.
    Nature 394 (1998), S. 552-553 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The temporal behaviour of solar activity (as manifested in sunspots) has long been debated. The 11-year periodicity in the total number of sunspots is well established observationally, as is a periodicity of 152–158 days in the occurrence of high-energy solar flares that was seen during ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/29012
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  • 4
    Electronic Resource
    Electronic Resource
    North-South asymmetry in sudden disappearances of solar prominences (1987)
    Springer
    Solar physics 112 (1987), S. 317-323 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract This paper presents the results of a study of the N-S asymmetry in sudden disappearances (SD) of solar prominences during solar cycles 18–21, obtained as a part of a more extensive research on SD and reappearances during years 1931–1985 (Ballester, 1984). As can be seen, the N-S SD asymmetry curve is not in phase with the solar cycle and peaks about the time of solar minimum, the asymmetry reverses in sign during the solar maximum, being, this change of sign, coincident with the reversal of the Sun's magnetic dipole. The SD asymmetry curve can be fitted by a sinusoidal function with a period of eleven years. On the other hand, the SD asymmetry curve shows a strong coincidence with the N-S asymmetries presented by other solar activity manifestations as studied by different authors.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00148786
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  • 5
    Electronic Resource
    Electronic Resource
    Periodicities in the north-south asymmetry of solar activity (1989)
    Springer
    Solar physics 119 (1989), S. 411-414 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract This paper tries to cast additional evidence on the proposed periodic behaviour of the N-S asymmetry in sudden disappearances (SD) of solar prominences (Vizoso and Ballester, 1987). We have performed a Blackman-Tukey power spectrum of the values of the SD N-S asymmetry and the results shows a significant peak, above 95% confidence level, at 12.4 years, another peak at 2.3 years fails to be statistically significant. Moreover, power spectrum performed with the values of N-S asymmetry of flare number and flare index (Vizoso and Ballester (1987) display significant peaks, above 95% confidence level, around 3.1–3.2 years.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00146187
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  • 6
    Electronic Resource
    Electronic Resource
    Prominence motions and their implications for magnetic fields (1984)
    Springer
    Solar physics 90 (1984), S. 37-40 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Using results obtained in our earlier paper (Ballester and Kleczek, 1983) and the equipartition principle we attempt to calculate the lower limits of magnetic fields in three solar prominences. The values are then compared with the magnetic fields found by experimental methods. Furthermore, we have calculated by Ampère's law the lower limits of electric currents inside the conical surface where the knot's motion is located. The results obtained are compared with a few determinations of electric currents in prominences, that can be found in the bibliography. An attempt is made to use a three-currents system to explain the configuration of magnetic fields in solar prominences.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153783
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  • 7
    Electronic Resource
    Electronic Resource
    Kinematics of solar prominences (1983)
    Springer
    Solar physics 87 (1983), S. 261-269 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Using a 16-mm film recorded by R. B. Dunn at Sacramento Peak Observatory with a 15-inch coronagraph, we have studied motions of three solar prominences from the kinematic point of view. We applied three methods proposed earlier (Billings and Pecker, 1954; Palus, 1972; Makhmudov et al., 1980) to three prominences of the film. A new method based on geometrical considerations is introduced. The results of all the four methods are compared and discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00224839
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  • 8
    Electronic Resource
    Electronic Resource
    Short-term periodicities in sunspot areas during solar cycle 22 (1995)
    Springer
    Solar physics 156 (1995), S. 145-155 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We have analyzed the daily record of sunspot areas during the current cycle 22 looking for the short-term periodicity of around 155 days which was present during some previous solar cycles. Two different methods have been used to compute the power spectra and the results indicate that such periodicity has been absent during the current solar cycle, which confirms the results obtained by other authors who used flares or flare-related data. However, we have found that, during some intervals of time, a periodicity close to 86 days is statistically significant. A similar periodicity was found by Landscheit (1986) in energetic X-ray flares, between 1970 and 1982 (second and first half of solar cycles 20 and 21, respectively), and by Bai (1992b) for important solar flares during solar cycle 20.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00669581
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  • 9
    Electronic Resource
    Electronic Resource
    Coronal MHD perturbation field generated by localized perturbers in a photospheric active region (1995)
    Springer
    Solar physics 159 (1995), S. 229-249 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We investigate the two-dimensional boundary value problem of the linear wave excitation in the solar corona by a pair of periodic perturbers localized at the photosphere. The physical properties of the corona allow us to consider a magnetic configuration such as a potential arcade which is in a magneto-hydrostatic equilibrium with the surrounding plasma. The model excludes the A1fvén mode and since the slow mode is absent in a potential arcade, the excited waves are then the fast magneto-acoustic modes. The characteristic magnetic field scale length is twice the scale height of the coronal plasma, assumed isothermal and the induced fluid motions are in the direction perpendicular to the magnetic field, in the cross-sectional plane of the arcade. A particular example of two localized perturbers in a photospheric active region is given, pointing out the effects produced in the perturbed fields by the variation of the different parameters involved. Such example shows that, while a modification of the linear size or the horizontal wave number of the perturbers does not affect significantly the propagating disturbances, the variation of the perturbers' frequency produces important effects. Such effects can be summarized by saying that low-frequency perturbers are able to disturb the whole coronal magnetic configuration above the active region while high-frequency perturbers only disturb the coronal region just above them, producing a channeling feature. Moreover, for high frequencies the perturbations grow withz all the way from the photosphere while for very low frequencies evanescent waves are dominant, although thanks to the influence of the medium their amplitude starts to grow from somez on.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00686531
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  • 10
    Electronic Resource
    Electronic Resource
    A note on magnetic fields and electric currents in solar prominences (1984)
    Springer
    Solar physics 94 (1984), S. 151-154 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We determine magnetic fields and electric currents in three prominences without simplifications used in our previous papers.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00154815
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