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  • 1
    Electronic Resource
    Electronic Resource
    355. Zur Wirksamkeit von Fibrinogen und Thrombin bei der Deckung experimenteller Verbrennungswunden (1983)
    Springer
    Langenbeck's archives of surgery 361 (1983), S. 907-907 
    Details
    ISSN: 1435-2451
    Keywords: Burn injuries ; Mesh graft ; Fibrin glue ; Verbrennung ; Mesh-Graft ; Fibrinkleber
    Source: Springer Online Journal Archives 1860-2000
    Topics: Medicine
    Description / Table of Contents: Zusammenfassung Experimentelle Verbrennungswunden an der Rückenhaut von Ratten (n = 20) im Bereich des thoracolumbalen Übergangs wurden mit Haut-Mesh-graft gedeckt, wobei in der Versuchsgruppe zusätzlich Fibrinkleber (Tissuecol) verwendet wurde. Planimetrische Auswertungen der nach 14 Tagen verbleibenden Wundflächen sowie mikroangiographische, histologische und thermographische Untersuchungen zeigen ein verbessertes Einheilen des Transplantates bei gleichzeitiger Fibrinkleberapplikation, was durch den festen initialen Kontakt zum Wundgrund und die verbesserte Blutstillung erklärt werden kann.
    Notes: Summary Experimental bum injuries in the dorsal thoracolumbar region of rats were covered by skin mesh grafts. In the treated group, fibrin adhesive (Tissucol) was also applied. Fourteen days after transplantation planimetric localization of the remaining wound area, microangiographic, histologic and thermographic studies demonstrated a better healing of the transplant additionally treated with fibrin adhesive. This can be explained by the fibrin-initiated contact with the wound and the hemostyptic effect of the fibrin adhesive.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF01276181
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Coalescing neutron stars as gamma ray bursters? (1995)
    Springer
    Astrophysics and space science 231 (1995), S. 423-426 
    Details
    ISSN: 1572-946X
    Keywords: Hydrodynamics ; Binaries: Close ; Stars: neutron ; Gamma rays: bursts
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We investigate the dynamics and evolution of coalescing neutron stars. The three-dimensional Newtonian equations of hydrodynamics are integrated by the “Piecewise Parabolic Method” on an equidistant Cartesian grid. The code is purely Newtonian, but does include the emission of gravitational waves and their back-reaction. The properties of neutron star matter are described by the equation of state of Lattimer and Swesty (1991). Energy loss by all types of neutrinos and changes of the electron fraction due to the emission of electron neutrinos and antineutrinos are taken into account by an elaborate “neutrino leakage scheme”. We simulate the coalescence of two identical, cool neutron stars with a baryonic mass of ≈ 1.6M ⊙ and a radius of ≈ 15 km and with an initial center-to-center distance of 42 km. The initial distributions of density and electron concentration are given from a model of a cold neutron star in hydrostatic equilibrium. We investigate three cases which differ by the initial velocity distribution in the neutron stars. The orbit decays due to gravitational-wave emission and after one revolution the stars are so close that dynamical instability sets in. Within 1 ms the neutron stars merge into a rapidly spinning (P ≈ 1 ms), high-density body (ρ ≈ 1014 g/cm3) with a surrounding thick disk of material with densitiesρ ≈ 1010 − 1012 g/cm3 and orbital velocities of 0.3-0.5 c. The peak emission of gravitational waves has a maximum luminosity of a few times 1055 erg/s and is reached for about 1 ms. The amplitudes of the gravitational waves are close to 3 ⋅ 10−23 at a distance of 1 Gpc and the typical frequency is near the dynamical value of the orbital motion of the merging neutron stars of 2 KHz. In a post-processing step, the rate of neutrino-antineutrino annihilation is calculated from the neutrino luminosities generated during the hydrodynamical simulations. We find the integral annihilation rate to be a few 1050 erg/s during the phase of strongest neutrino emission, which is too small to generate the observed bursts considering the fact that the merged object of about 3M⊙ will most likely collapse to a black hole within milliseconds.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00658662
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    Paper (German National Licenses)
    Fulltext
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