123 research outputs found

    The Pairing Mechanism in HTSC investigated by Electronic Raman Scattering

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    By means of electronic Raman scattering we investigated the symmetry of the energy gap Delta(k), its temperature dependence and its variation with doping of well characterized Bi2Sr2CaCu2O8+delta single crystals. The oxygen content delta was varied between the under- and the overdoped regime by subsequently annealing the same single crystal in Ar and O2, respectively. The symmetry analysis of the polarized electronic Raman scattering is consistent with a d_x^2-y^2-wave symmetry of the energy gap in both regimes. The gap ratio 2Delta_max/k_BT_c and its temperature dependence changes with doping similar to predictions of theories based on paramagnon coupling.Comment: 3 pages, LaTeX, 2 ps figures available on request to [email protected]

    De onderwijsenquête van 1799:Overzicht van de toestand van scholen en onderwijs in Nederland

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    Het eerste landelijke overzicht van de toestand van het onderwijs stamt uit 1799. Enige jaren daarvoor had de Bataafse Republiek een einde aan het gewestelijk en stedelijk particularisme van de Republiek van de Verenigde Nederlanden gemaakt en de eenheidsstaat uitgeroepen. Van de inwoners werd verwacht dat zij hun oude bindingen opgaven en zich zouden identificeren met de cultuur van de nieuwe staat. Om de eenheidsgedachte te stimuleren nam de overheid diverse maatregelen. Het onderwijs werd als hét middel om een bijdrage aan de fundering van de nationale staat te leveren, gezien. Van staatswege zou aan de herinrichting een reorganisatie van het gehele onderwijs leiding worden gegeven. In 1798 belastte de overheid een Agent van Nationale Opvoeding met deze taak

    Symmetry dependence of phonon lineshapes in superconductors with anisotropic gaps

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    The temperature dependence below TcT_{c} of the lineshape of optical phonons of different symmetry as seen in Raman scattering is investigated for superconductors with anisotropic energy gaps. It is shown that the symmetry of the electron-phonon vertex produces non-trivial couplings to an anisotropic energy gap which leads to unique changes in the phonon lineshape for phonons of different symmetry. The phonon lineshape is calculated in detail for B1gB_{1g} and A1gA_{1g} phonons in a superconductor with dx2y2d_{x^{2}-y^{2}} pairing symmetry. The role of satellite peaks generated by the electron-phonon coupling are also addressed. The theory accounts for the substantial phonon narrowing of the B1gB_{1g} phonon, while narrowing of the A1gA_{1g} phonon which is indistinguishable from the normal state is shown, in agreement with recent measurements on BSCCO.Comment: 15 pages (3 Figures available upon request), Revtex, 1

    Formation of SMBH seeds in Pop III star clusters through collisions : the importance of mass loss

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    Runaway collisions in dense clusters may lead to the formation of supermassive black hole (SMBH) seeds, and this process can be further enhanced by accretion, as recent models of SMBH seed formation in Population III star clusters have shown. This may explain the presence of supermassive black holes already at high redshift, z>6z>6. However, in this context, mass loss during collisions was not considered and could play an important role for the formation of the SMBH seed. Here, we study the effect of mass loss, due to collisions of protostars, in the formation and evolution of a massive object in a dense primordial cluster. We consider both constant mass loss fractions as well as analytic models based on the stellar structure of the collision components. Our calculations indicate that mass loss can significantly affect the final mass of the possible SMBH seed. Considering a constant mass loss of 5% for every collision, we can lose between 60-80% of the total mass that is obtained if mass loss were not considered. Using instead analytical prescriptions for mass loss, the mass of the final object is reduced by 15-40%, depending on the accretion model for the cluster we study. Altogether, we obtain masses of the order of 104M10^4M_{\odot}, which are still massive enough to be SMBH seeds.Comment: 12 pages, 9 figures, accepted by MNRA
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