@misc{ChampagnatRoelly2008,
  author    = {Champagnat, Nicolas and Roelly, Sylvie},
  title     = {Limit theorems for conditioned multitype Dawson-Watanabe processes and Feller diffusions},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18610},
  year      = {2008},
  abstract  = {A multitype Dawson-Watanabe process is conditioned, in subcritical and critical cases, on non-extinction in the remote future. On every finite time interval, its distribution is absolutely continuous with respect to the law of the unconditioned process. A martingale problem characterization is also given. Several results on the long time behavior of the conditioned mass process - the conditioned multitype Feller branching diffusion - are then proved. The general case is first considered, where the mutation matrix which models the interaction between the types, is irreducible. Several two-type models with decomposable mutation matrices are analyzed too .},
  language  = {en}
}
@misc{PueschelHespelingOppermannetal.1993,
  author    = {P{\"u}schel, Gerhard Paul and Hespeling, Ursula and Oppermann, Martin and Dieter, Peter},
  title     = {Increase in prostanoid formation in rat liver macrophages (Kupffer cells) by human anaphylatoxin C3a},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-16716},
  year      = {1993},
  abstract  = {Human anaphylatoxin C3a increases glycogenolysis in perfused rat liver. This action is inhibited by prostanoid synthesis inhibitors and prostanoid antagonists. Because prostanoids but not anaphylatoxin C3a can increase glycogenolysis in hepatocytes, it has been proposed that prostanoid formation in nonparenchymal cells represents an important step in the C3a-dependent increase in hepatic glycogenolysis. This study shows that (a) human anaphylatoxin C3a (0.1 to 10 mug/ml) dose-dependently increased prostaglandin D2, thromboxane B, and prostaglandin F2alpha formation in rat liver macrophages (Kupffer cells); (b) the C3a-mediated increase in prostanoid formation was maximal after 2 min and showed tachyphylaxis; and (c) the C3a-elicited prostanoid formation could be inhibited specifically by preincubation of C3a with carboxypeptidase B to remove the essential C-terminal arginine or by preincubation of C3a with Fab fragments of a neutralizing monoclonal antibody. These data support the hypothesis that the C3a-dependent activation of hepatic glycogenolysis is mediated by way of a C3a-induced prostanoid production in Kupffer cells.},
  language  = {en}
}
@misc{PueschelNathJungermann1987,
  author    = {P{\"u}schel, Gerhard Paul and Nath, Annegret and Jungermann, Kurt},
  title     = {Increase of urate formation by stimulation of sympathetic hepatic nerves, circulating noradrenaline and glucagon inthe perfused rat liver},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-16728},
  year      = {1987},
  abstract  = {In the isolated rat liver perfused in situ stimulation of the nerve bundles around the portal vein and the hepatic artery caused an increase of urate formation that was inhibited by the α1-blocker prazosine and the xanthine oxidase inhibitor allopurinol. Moreover, nerve stimulation increased glucose and lactate output and decreased perfusion flow. Infusion of noradrenaline had similar effects. Compared to nerve stimulation infusion of glucagon led to a less pronounced increase of urate formation and a twice as large increase in glucose output but a decrease in lactate release without affecting the flow rate. Insulin had no effect on any of the parameters studied.},
  language  = {en}
}
@inproceedings{Szeifert2007,
  author    = {Szeifert, T.},
  title     = {Wind variabilities and asymmetries in Luminous Blue Variables},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18146},
  year      = {2007},
  abstract  = {Luminous Blue Variables show strong changes in their stellar wind on time scales of typically years to decades when they expand and contract radially at approximately constant luminosity. Micro-variability on shorter time scales and amplitudes can be observed superimposed to the larger scale radial changes. I will show long-term time series of high resolution spectra which we have collected in the past 20 years for many of the well known LBVs together with a few time series of weekly sampling (HR Car, R40, R71, R110, R127, S Dor) covering a time windows of up to a few months. Wind variability is seen on short and intermediate time scales with the line profiles changing from P Cygni to inverse P Cygni and double peeked profiles sometimes for the same star and spectral line. On longer time scales the ionisation levels for all chemical elements change drastically due to the strong change of the temperature on the stellar surface. While on the long term the characteristic radial changes may have impact on the over all mass loss rates, the variabilities and asymmetries on short and intermediate time scales may cause false estimates of the mass loss rates when confronting models with the observed line profiles},
  language  = {en}
}
@inproceedings{Moffat2007,
  author    = {Moffat, Anthony F. J.},
  title     = {Observational overview of clumping in hot stellar winds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17633},
  year      = {2007},
  abstract  = {In the old days (pre ∼1990) hot stellar winds were assumed to be smooth, which made life fairly easy and bothered no one. Then after suspicious behaviour had been revealed, e.g. stochastic temporal variability in broadband polarimetry of single hot stars, it took the emerging CCD technology developed in the preceding decades (∼1970-80's) to reveal that these winds were far from smooth. It was mainly high-S/N, time-dependent spectroscopy of strong optical recombination emission lines in WR, and also a few OB and other stars with strong hot winds, that indicated all hot stellar winds likely to be pervaded by thousands of multiscale (compressible supersonic turbulent?) structures, whose driver is probably some kind of radiative instability. Quantitative estimates of clumping-independent mass-loss rates came from various fronts, mainly dependent directly on density (e.g. electron-scattering wings of emission lines, UV spectroscopy of weak resonance lines, and binary-star properties including orbital-period changes, electron-scattering, and X-ray fluxes from colliding winds) rather than the more common, easier-to-obtain but clumping-dependent density-squared diagnostics (e.g. free-free emission in the IR/radio and recombination lines, of which the favourite has always been Hα). Many big questions still remain, such as: What do the clumps really look like? Do clumping properties change as one recedes from the mother star? Is clumping universal? Does the relative clumping correction depend on \$\dot{M}\$ itself?},
  language  = {en}
}
@inproceedings{PulsMarkovaNajarroetal.2007,
  author    = {Puls, Joachim and Markova, N. and Najarro, F. and Hanson, M. M.},
  title     = {Clumping in O-star winds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17683},
  year      = {2007},
  abstract  = {We review various diagnostics of clumping in O-star winds, with special emphasis on its radial stratification. Implications and problems are discussed, and promising NIR methods are presented.},
  language  = {en}
}
@inproceedings{StLouisMoffat2007,
  author    = {St-Louis, N. and Moffat, Anthony F. J.},
  title     = {Do clumping corrections increase with decreasing mass-loss rates?},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17696},
  year      = {2007},
  abstract  = {We report on new mass-loss rate estimates for O stars in six massive binaries using the amplitude of orbital-phase dependent, linear-polarimetric variability caused by electron scattering off free electrons in the winds. Our estimated mass-loss rates for luminous O stars are independent of clumping. They suggest similar clumping corrections as for WR stars and do not support the recently proposed reduction in mass-loss rates of O stars by one or two orders of magnitude.},
  language  = {en}
}
@inproceedings{Smith2007,
  author    = {Smith, Nathan},
  title     = {Independent signs of lower mass-loss rates for O-type stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17659},
  year      = {2007},
  abstract  = {I discuss observational evidence - independent of the direct spectral diagnostics of stellar winds themselves - suggesting that mass-loss rates for O stars need to be revised downward by roughly a factor of three or more, in line with recent observed mass-loss rates for clumped winds. These independent constraints include the large observed mass-loss rates in LBV eruptions, the large masses of evolved massive stars like LBVs and WNH stars, WR stars in lower metallicity environments, observed rotation rates of massive stars at different metallicity, supernovae that seem to defy expectations of high mass-loss rates in stellar evolution, and other clues. I pay particular attention to the role of feedback that would result from higher mass-loss rates, driving the star to the Eddington limit too soon, and therefore making higher rates appear highly implausible. Some of these arguments by themselves may have more than one interpretation, but together they paint a consistent picture that steady line-driven winds of O-type stars have lower mass-loss rates and are significantly clumped.},
  language  = {en}
}
@inproceedings{VotrubaFeldmeierKubatetal.2007,
  author    = {Votruba, V. and Feldmeier, Achim and Kub{\´a}t, Jiř{\´i} and R{\"a}tzel, D.},
  title     = {Multicomponent stellar wind of hot stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17677},
  year      = {2007},
  abstract  = {We developed a time-dependent multicomponent hydrodynamical code for simulation of the stellar wind from hot stars and applied it to stars with high and low density winds.},
  language  = {en}
}
@inproceedings{Lobel2007,
  author    = {Lobel, A.},
  title     = {Modeling DACs in UV lines of massive hot stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17856},
  year      = {2007},
  abstract  = {We apply the 3-dimensional radiative transport codeWind3D to 3D hydrodynamic models of Corotating Interaction Regions to fit the detailed variability of Discrete Absorption Components observed in Si iv UV resonance lines of HD 64760 (B0.5 Ib). We discuss important effects of the hydrodynamic input parameters on these large-scale equatorial wind structures that determine the detailed morphology of the DACs computed with 3D transfer. The best fit model reveals that the CIR in HD 64760 is produced by a source at the base of the wind that lags behind the stellar surface rotation. The non-corotating coherent wind structure is an extended density wave produced by a local increase of only 0.6\% in the smooth symmetric wind mass-loss rate.},
  language  = {en}
}