@misc{Wendel2022,
  type      = {Master Thesis},
  author    = {Wendel, Christoph},
  title     = {Bestimmung des hochenergetischen Spektrums des Crab-Pulsars anhand eines Outer Gap-Modells},
  doi       = {10.25972/OPUS-25719},
  url       = {http://nbn-resolving.de/urn:nbn:de:bvb:20-opus-257191},
  school      = {Universit{\"a}t W{\"u}rzburg},
  year      = {2022},
  abstract  = {Im Rahmen eines selbst-konsistenten Outer-Gap-Modells der Pulsar-Magnetosph{\"a}re wurde die elektromagnetische sehr hochenergetische Strahlung des Crab-Pulsars simuliert. Dies wurde parallel anhand zweier verschiedener F{\"a}lle getan, die sich in den angenommenen Gleichungen f{\"u}r die elektrische Feldst{\"a}rke und f{\"u}r den Kr{\"u}mmungsradius der magnetischen Feldlinien unterscheiden. Die Kinetik der geladenen Teilchen bei ihrer Propagation durch die Outer Gap wurde unter Einbeziehung von Kr{\"u}mmungsstrahlung, inverser Compton-Streuung und Triple Paarbildung betrachtet. Das theoretisch simulierte Spektrum wird mit von Fermi-LAT und von den MAGIC Teleskopen gemessenen Daten verglichen.},
  subject      = {Neutronenstern},
  language  = {de}
}
@phdthesis{Maier2008,
  author    = {Maier, Andreas},
  title     = {Adaptively Refined Large-Eddy Simulations of Galaxy Clusters},
  url       = {http://nbn-resolving.de/urn:nbn:de:bvb:20-opus-32274},
  school      = {Universit{\"a}t W{\"u}rzburg},
  year      = {2008},
  abstract  = {It is aim of this work to develop, implement, and apply a new numerical scheme for modeling turbulent, multiphase astrophysical flows such as galaxy cluster cores and star forming regions. The method combines the capabilities of adaptive mesh refinement (AMR) and large-eddy simulations (LES) to capture localized features and to represent unresolved turbulence, respectively; it will be referred to as Fluid mEchanics with Adaptively Refined Large-Eddy SimulationS or FEARLESS.},
  subject      = {Turbulenz},
  language  = {en}
}
@article{ChatterjeeChaelTiedeetal.2023,
  author    = {Chatterjee, Koushik and Chael, Andrew and Tiede, Paul and Mizuno, Yosuke and Emami, Razieh and Fromm, Christian and Ricarte, Angelo and Blackburn, Lindy and Roelofs, Freek and Johnson, Michael D. and Doeleman, Sheperd S. and Arras, Philipp and Fuentes, Antonio and Knollm{\"u}ller, Jakob and Kosogorov, Nikita and Lindahl, Greg and M{\"u}ller, Hendrik and Patel, Nimesh and Raymond, Alexander and Traianou, Efthalia and Vega, Justin},
  title     = {Accretion flow morphology in numerical simulations of black holes from the ngEHT model library: the impact of radiation physics},
  series = {Galaxies},
  volume    = {11},
  journal   = {Galaxies},
  number    = {2},
  issn      = {2075-4434},
  doi       = {10.3390/galaxies11020038},
  url       = {http://nbn-resolving.de/urn:nbn:de:bvb:20-opus-304084},
  year      = {2023},
  abstract  = {In the past few years, the Event Horizon Telescope (EHT) has provided the first-ever event horizon-scale images of the supermassive black holes (BHs) M87* and Sagittarius A* (Sgr A*). The next-generation EHT project is an extension of the EHT array that promises larger angular resolution and higher sensitivity to the dim, extended flux around the central ring-like structure, possibly connecting the accretion flow and the jet. The ngEHT Analysis Challenges aim to understand the science extractability from synthetic images and movies to inform the ngEHT array design and analysis algorithm development. In this work, we compare the accretion flow structure and dynamics in numerical fluid simulations that specifically target M87* and Sgr A*, and were used to construct the source models in the challenge set. We consider (1) a steady-state axisymmetric radiatively inefficient accretion flow model with a time-dependent shearing hotspot, (2) two time-dependent single fluid general relativistic magnetohydrodynamic (GRMHD) simulations from the H-AMR code, (3) a two-temperature GRMHD simulation from the BHAC code, and (4) a two-temperature radiative GRMHD simulation from the KORAL code. We find that the different models exhibit remarkably similar temporal and spatial properties, except for the electron temperature, since radiative losses substantially cool down electrons near the BH and the jet sheath, signaling the importance of radiative cooling even for slowly accreting BHs such as M87*. We restrict ourselves to standard torus accretion flows, and leave larger explorations of alternate accretion models to future work.},
  language  = {en}
}
@article{KrausMouchaRoth2022,
  author    = {Kraus, Daniela and Moucha, Annika and Roth, Oliver},
  title     = {A sharp Bernstein-type inequality and application to the Carleson embedding theorem with matrix weights},
  series = {Analysis and Mathematical Physics},
  volume    = {12},
  journal   = {Analysis and Mathematical Physics},
  number    = {1},
  issn      = {1664-235X},
  doi       = {10.1007/s13324-021-00639-5},
  url       = {http://nbn-resolving.de/urn:nbn:de:bvb:20-opus-270485},
  year      = {2022},
  abstract  = {We prove a sharp Bernstein-type inequality for complex polynomials which are positive and satisfy a polynomial growth condition on the positive real axis. This leads to an improved upper estimate in the recent work of Culiuc and Treil (Int. Math. Res. Not. 2019: 3301-3312, 2019) on the weighted martingale Carleson embedding theorem with matrix weights. In the scalar case this new upper bound is optimal.},
  language  = {en}
}
@phdthesis{Schulz2016,
  author    = {Schulz, Robert Frank},
  title     = {A radio view of high-energy emitting AGNs},
  url       = {http://nbn-resolving.de/urn:nbn:de:bvb:20-opus-137358},
  school      = {Universit{\"a}t W{\"u}rzburg},
  year      = {2016},
  abstract  = {The most energetic versions of active galactic nuclei (AGNs) feature two highly-relativistic plasma outflows, so-called jets, that are created in the vicinity of the central supermassive black hole and evolve in opposite directions. In blazars, which dominate the extragalactic gamma-ray sky, the jets are aligned close to the observer's line of sight leading to strong relativistic beaming effects of the jet emission. Radio observations especially using very long baseline interferometry (VLBI) provide the best way to gain direct information on the intrinsic properties of jets down to sub-parsec scales, close to their formation region. In this thesis, I focus on the properties of three AGNs, IC 310, PKS 2004-447, and 3C 111 that belong to the small non-blazar population of gamma-ray-loud AGNs. In these kinds of AGNs, the jets are less strongly aligned with respect to the observer than in blazars. I study them in detail with a variety of radio astronomical instruments with respect to their high-energy emission and in the context of the large samples in the monitoring programmes MOJAVE and TANAMI. My analysis of radio interferometric observations and flux density monitoring data reveal very different characteristics of the jet emission in these sources. The work presented in this thesis illustrates the diversity of the radio properties of gamma-ray-loud AGNs that do not belong to the dominating class of blazars.},
  subject      = {Aktiver galaktischer Kern},
  language  = {en}
}