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  • 1
    Electronic Resource
    Electronic Resource
    trans-(±)-N,N'-Bis(salicylidene)-1,2-cyclohexanediamine (1997)
    Oxford [u.a.] : International Union of Crystallography (IUCr)
    Acta crystallographica 53 (1997), S. 1671-1673 
    Details
    ISSN: 1600-5759
    Source: Crystallography Journals Online : IUCR Backfile Archive 1948-2001
    Topics: Chemistry and Pharmacology , Geosciences , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1107/S0108270197008640
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  • 2
    Electronic Resource
    Electronic Resource
    (±)-7,7,9,9-Tetramethyl-2,3:4,5-dinaphtho-1,6,8-trioxa-7,9-disilacyclonona-2,4-diene (1998)
    Oxford [u.a.] : International Union of Crystallography (IUCr)
    Acta crystallographica 54 (1998), S. 145-146 
    Details
    ISSN: 1600-5759
    Source: Crystallography Journals Online : IUCR Backfile Archive 1948-2001
    Topics: Chemistry and Pharmacology , Geosciences , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1107/S0108270197010317
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  • 3
    Electronic Resource
    Electronic Resource
    Evidence for narrow Δ0(1232) states in the 12 C(e,e'pπ−}11 C Reaction (1999)
    Springer
    The European physical journal 4 (1999), S. 209-216 
    Details
    ISSN: 1434-601X
    Keywords: PACS: 24.30.Gd Nuclear physics: Resonance reactions – 25.30.Rw Electroproduction reactions – 14.20.Gk Baryon resonances with S = 0 – 21.80.+a Hypernuclei
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract: The reaction 12C(e,e'Δ0)11C →12C(e,e'pπ−)11C was investigated at the Mainz Microtron MAMI in a triple coincidence measurement using the three spectrometer setup of the A1 Collaboration. The good missing mass resolution of σm= 0.27 MeV/c2 allowed to select the events belonging to the ground state of 11C. Cutting on these events the excitation energy spectra of 12CΔ0 show evidence for two peaks of about 4 MeV width (FWHM) at 282 MeV and 296 MeV with a significance of about 4.5 standard deviations. The peaks are interpreted in a simple weak coupling model as bound Δ0 states in 12CΔ0.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/s100500050220
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  • 4
    Electronic Resource
    Electronic Resource
    Multi-Wavelength Analysis of the Flare on 2 October 1993 (1998)
    Springer
    Solar physics 182 (1998), S. 163-177 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract By use of Yohkoh hard X-ray flux and soft X-ray images, and of vector magnetograms and 2D spectral observations, a 1N/C6.5 flare observed on 2 October 1993 is analysed in detail. Evidence is provided not only morphologically but also quantitatively that the dynamics at kernels A and C of the flare in the impulsive phase were controlled mainly by electron beam bombardment, while the heating of kernel B is mainly due to heat conduction. By plotting the energy gradient of the electron energy flux as a function of energy for the various spectral indexes observed during the flare, the acceleration mechanism is found to be such that there is a constant energy E0, close to 20 keV, for which the electron flux d F1/dE is constant. It is shown that such a conclusion can be reached more directly by using the photon flux, which in that case must be constant for E=E0, whatever the value of the power index. This result implies also that the electron spectrum is represented by a power law and that the X-ray photons are produced in a thick target. Instantaneous momentum balance is shown to exist between the upflowing soft X-ray-emitting and the downflowing Hα- emitting plasma at the kernels of the flare. The observed Hα red asymmetry is well reproduced by the non-LTE computation, with the down-moving condensation included. The observation of the magnetic field suggests that the flare was triggered probably by magnetic flux emergence.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005033713559
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  • 5
    Electronic Resource
    Electronic Resource
    On a possible explanation of chromospheric line asymmetries of solar flares (1996)
    Springer
    Solar physics 166 (1996), S. 437-440 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We discuss the relationship between the chromospheric downward motions and the line asymmetries in solar flares by using a simple model. It is found that both the blue asymmetry and red asymmetry of the Hα line can be caused by downward motions, as long as the moving material is confined to different heights in the chromosphere. The Ca ii K line, however, mainly shows a red asymmetry. The results can qualitatively explain some observations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149410
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  • 6
    Electronic Resource
    Electronic Resource
    Coronal Loops Above a Sunspot Region (1997)
    Springer
    Solar physics 176 (1997), S. 267-277 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract By analysing the data of Yohkoh soft X-ray images, vector magnetograms and 2D spectral observations, coronal loops above a large sunspot on 16–19 May 1994 have been studied. It is shown that the loops follow generally the alignment of concentrated magnetic flux. The results indicate that the soft X-ray emission is low just above the sunspot, while some loops connecting regions with opposite magnetic polarities show strong soft X-ray emission. Especially, the part of the loops near the weaker magnetic field region tends to be brighter than the one near the stronger magnetic field. The temperature around the top of the loops is typically ∼3 × 106 K, which is higher than that at the legs of the loops by a factor of 1.5–2.0. The density near the top of the loops is about 5 x 109 cm-3, which is higher than that of the leg parts of the loops. These loops represent probably the sites where strong magnetic flux and/or current are concentrated.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1004934213329
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  • 7
    Electronic Resource
    Electronic Resource
    Analysis of 2-d flare spectra: Velocity fields derived from Hα line asymmetries (1995)
    Springer
    Solar physics 158 (1995), S. 81-93 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We derive a time series of two-dimensional velocity fields for a flare region on 1992 December 16, based on the asymmetries of the Hα line. The Hα spectra were obtained by an imaging spectrograph at the Solar Tower Telescope of Nanjing University. Four sites with evident chromospheric downflows are found to appear and decay consecutively in the studied region. The value of maximum velocities is 30–40 km s−1 and the lifetime of downflows is 2–3 min at these sites. It is also shown that the asymmetries only exist at the line wing, while the line center has nearly no shifts for this flare. Finally, we make a discussion on the characteristics of the velocity distribution and its correlations with the intensity distribution, as well as with the hard X-ray emission.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00680836
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  • 8
    Electronic Resource
    Electronic Resource
    A CCD imaging spectrograph in the improved solar tower of Nanjing University (1995)
    Springer
    Solar physics 159 (1995), S. 127-135 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Since 1992 the solar tower telescope of Nanjing University (118°51′ E, 32°03′ N) as well as its multichannel solar spectrograph, originally established in 1982, have been reconstructed and a two-channel imaging spectrograph has been operated successfully. The apertures of the coelostat and the secondary mirror are both 60 cm. The spherical objective mirror, having an aperture of 43 cm and a focal length of 2170 cm, produces a solar image of 20 cm diameter. Two auxiliary telescopes using a small fraction of the coelostat's aperture were set up for guiding and Hα monochromatic monitoring. A multichannel spectrograph can be operated in six wavebands simultaneously. A CCD imaging spectrograph can be used for data acquisition at Hα and Caii K line wavebands automatically and simultaneously. The instrument consists of two CCD cameras, an image processor (SR-151), a personal computer, and a mechanical scanning device. The principal characteristics of the instruments are described. Some observational results are presented as examples.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00733036
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  • 9
    Electronic Resource
    Electronic Resource
    Molecular basis of inter-alpha-trypsin inhibitor heavy chain H1 (ITIH1) polymorphism (1995)
    Springer
    Human genetics 〈Berlin〉 95 (1995), S. 435-436 
    Details
    ISSN: 1432-1203
    Source: Springer Online Journal Archives 1860-2000
    Topics: Biology , Medicine
    Notes: Abstract A genetic polymorphism of the inter-alpha-trypsin inhibitor heavy chain H1 (ITIH1) was analyzed at the nucleic acid level. Three common alleles, ITIH1*1, ITIH1*2 and ITIH1*3, were characterized by mutations at codons 551 and 561 in exon 14. ITIH1*1 was characterized by GAG (Glu) at codon 551 and CAG (Gln) at codon 561, ITIH1*2, by GTG (Val) and CGG (Arg), and ITIH1*3, by GAG (Glu) and CGG (Arg).
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00208970
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  • 10
    Electronic Resource
    Electronic Resource
    An unusual behaviour of the white-light flare on 11 October, 1974 (1995)
    Springer
    Solar physics 158 (1995), S. 387-390 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract It was found that in the spectrum of the white-light flare on 11 October, 1974, at the time of continuum maximum, the intensity of K1 in the Caii K line increased very significantly and reached nearly half of the continuum intensity. The duration of this unusual increase is less than 4 min. It seems that existing semi-empirical models can reproduce neither this characteristic nor the chromospheric condensation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00795672
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