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Berichtet wird von einer 1858 veröffentlichten Novelle, in der Alexander von Humboldt als Titelheld erschien. Der Verfasser, der preußische Offizier Eugen Hermann von Dedenroth, sandte Humboldt ein Exemplar des Buches in der Hoffnung auf eine lobende Notiz. Stattdessen beklagte sich Humboldt öffentlich „über die Unzartheit deutscher literarischer Gewohnheiten“.
Der vorliegende Beitrag gibt einen Überblick über die Individualbeschwerden, die von den UN-Vertragsüberwachungsorganen – mit Ausnahme des Menschenrechtsausschusses – von August 2006 bis September 2007 behandelt wurden. Alle zitierten Dokumente sind über die Seiten des Büros der Hohen Kommissarin der für Menschenrechte der Vereinten Nationen (OHCHR) einsehbar.
X-ray spectroscopy is a sensitive probe of stellar winds. X-rays originate from optically thin shock-heated plasma deep inside the wind and propagate outwards throughout absorbing cool material. Recent analyses of the line ratios from He-like ions in the X-ray spectra of O-stars highlighted problems with this general paradigm: the measured line ratios of highest ions are consistent with the location of the hottest X-ray emitting plasma very close to the base of the wind, perhaps indicating the presence of a corona, while measurements from lower ions conform with the wind-embedded shock model. Generally, to correctly model the emerging Xray spectra, a detailed knowledge of the cool wind opacities based on stellar atmosphere models is prerequisite. A nearly grey stellar wind opacity for the X-rays is deduced from the analyses of high-resolution X-ray spectra. This indicates that the stellar winds are strongly clumped. Furthermore, the nearly symmetric shape of X-ray emission line profiles can be explained if the wind clumps are radially compressed. In massive binaries the orbital variations of X-ray emission allow to probe the opacity of the stellar wind; results support the picture of strong wind clumping. In high-mass X-ray binaries, the stochastic X-ray variability and the extend of the stellar-wind part photoionized by X-rays provide further strong evidence that stellar winds consist of dense clumps.
We summarize Chandra observations of the emission line profiles from 17 OB stars. The lines tend to be broad and unshifted. The forbidden/intercombination line ratios arising from Helium-like ions provide radial distance information for the X-ray emission sources, while the H-like to He-like line ratios provide X-ray temperatures, and thus also source temperature versus radius distributions. OB stars usually show power law differential emission measure distributions versus temperature. In models of bow shocks, we find a power law differential emission measure, a wide range of ion stages, and the bow shock flow around the clumps provides transverse velocities comparable to HWHM values. We find that the bow shock results for the line profile properties, consistent with the observations of X-ray line emission for a broad range of OB star properties.