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  • 1
    Electronic Resource
    Electronic Resource
    The effect of estradiol on the sebaceous gland of the hamster ear and its antagonism by tamoxifen (1985)
    Springer
    Archives of dermatological research 277 (1985), S. 230-234 
    Details
    ISSN: 1432-069X
    Keywords: Sebaceous gland ; Estradiol ; Tamoxifen ; Histoplanimetry ; Androgen effects
    Source: Springer Online Journal Archives 1860-2000
    Topics: Medicine
    Notes: Summary To evaluate the antagonism between estradiol and tamoxifen in the sebaceous gland of the hamster ear, animals were topically treated, and the size of the sebaceous glands was measured by histoplanimetry. The systemic effects were described by determining the estradiol and testosterone plasma levels and within the testes, and the size of the seminal vesicles and the contralateral sebaceous gland. The administration of 0.1 μg estradiol resulted in a diminution in the size of the treated glands but left all other parameters unchanged, indicating a purely local effect. A higher dose of estradiol (1 μg) further decreased the size of the treated glands, but this was combined with a systemic effect, i.e. low plasma testosterone, decrease in testis size and a diminution of the contralateral ear gland. Ten micrograms of estradiol maximally suppressed all of the androgen effects without side effects. The administration of tamoxifen alone also decreased the size of the sebaceous glands without side effects, but it did not affect the production or effects of androgens. When administered in combination with estradiol, it antagonized the effects of this hormone completely. We conclude that tamoxifen inhibits the negative effect of estradiol on sebaceous-gland size. It acts predominantly in a systemic manner, because a metabolisation to monohydroxytamoxifen is necessary.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00404322
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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)
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