The most significant bottleneck in wireless communication systems is an ever-increasing disproportion between the bandwidth demand and the available spectrum. A major challenge in the field of wireless communications is to maximise the spatial reuse of resources whilst avoiding detrimental co-channel interference (CCI). To this end, frequency planning and centralised coordination approaches are widely used in wireless networks. However, the networks for the next generation of wireless communications are often envisioned to be decentralised, randomly distributed in space, hierarchical and support heterogeneous traffic and service types. Fixed frequency allocation would not cater for the heterogeneous demands and centralised resource allocation would be cumbersome and require a lot of signalling. Decentralised radio resource allocation based on locally available information is considered the key. In this context, the busy burst (BB) signalling concept is identified as a potential mechanism for decentralised interference management in future generation networks. Interference aware allocation of time-frequency slots (chunks) is accomplished by letting receivers transmit a BB in a time-multiplexed mini-slot, upon successful reception of data. Exploiting channel reciprocity of the time division duplex (TDD) mode, the transmitters avoid reusing the chunks where the received BB power is above a pre-determined threshold so as to limit the CCI caused towards the reserved chunks to a threshold value. In this thesis, the performance of BB signalling mechanism in orthogonal frequency division multiple access - time division duplexing (OFDMA-TDD) systems is evaluated by means of system level simulations in networks operating in ad hoc and cellular scenarios. Comparisons are made against the state-of-the-art centralised CCI avoidance and mitigation methods, viz. frequency planning, fractional frequency reuse, and antenna array with switched grid of beams, as well as decentralised methods such as the carrier sense multiple access method that attempt to avoid CCI by avoiding transmission on chunks deemed busy. The results demonstrate that with an appropriate choice of threshold parameter, BB-based techniques outperform all of the above state-of-the-art methods. Moreover, it is demonstrated that by adjusting the BB-specific threshold parameter, the system throughput can be traded off for improving throughput for links with worse channel condition, both in the ad hoc and cellular scenario. Moreover, by utilising a variable BB power that allows a receiver to signal the maximum CCI it can tolerate, it is shown that a more favourable trade-off between total system throughput and link throughput can be made. Furthermore, by performing link adaptation, it is demonstrated that the spatial reuse and the energy efficiency can be traded off by adjusting the threshold parameter. Although the BB signalling mechanism is shown to be effective in avoiding detrimental CCI, it cannot mitigate CCI by itself. On the other hand, multiple antenna techniques such as adaptive beamforming or switched beam approaches allow CCI to be mitigated but suffer from hidden node problems. The final contribution of this thesis is that by combining the BB signalling mechanism with multiple antenna techniques, it is demonstrated that the hybrid approach enhances spatial reusability of resources whilst avoiding detrimental CCI. In summary, this thesis has demonstrated that BB provides a flexible radio resource mechanism that is suitable for future generation networks.

We present the discovery of the X-ray and optical afterglows of the short-duration GRB 150101B, pinpointing the event to an early-type host galaxy at z = 0.1343 +/- 0.0030. This makes GRB 150101B the most nearby short gamma-ray burst (GRB) with an early-type host galaxy discovered to date. Fitting the spectral energy distribution of the host galaxy results in an inferred stellar mass of approximate to 7 x 10(10) M-circle dot, stellar population age of approximate to 2-2.5 Gyr, and star formation rate of less than or similar to 0.4M(circle dot) yr(-1). The host of GRB 150101B is one of the largest and most luminous short GRB host galaxies, with a B-band luminosity of approximate to 4.3L(*) and half-light radius of approximate to 8 kpc. GRB 150101B is located at a projected distance of 7.35 +/- 0.07. kpc from its host center and lies on a faint region of its host rest-frame optical light. Its location, combined with the lack of associated supernova, is consistent with an NS-NS/NS-BH merger progenitor. From modeling the evolution of the broadband afterglow, we calculate isotropic-equivalent gamma-ray and kinetic energies of approximate to 1.3 x 10(49) erg and approximate to(6-14) x 10(51) erg, respectively, a circumburst density of approximate to(0.8-4) x 10(-5) cm(-3), and a jet opening angle of greater than or similar to 9 degrees. Using observations extending to approximate to 30 days, we place upper limits of less than or similar to(2-4) x 10(41) erg s(-1) on associated kilonova emission. We compare searches following previous short GRBs to existing kilonova models and demonstrate the difficulty of performing effective kilonova searches from cosmological short GRBs using current ground-based facilities. We show that at the Advanced LIGO/VIRGO horizon distance of 200 Mpc, searches reaching depths of approximate to 23-24 AB. mag are necessary to probe a meaningful range of kilonova models.

It is natural to consider the possibility that the most energetic particles detected (> 10^18 eV), ultra-high-energy cosmic rays (UHECRs), are originated at the most luminous transient events observed (> 10^52 erg s^-1), gamma-ray bursts (GRBs). As a result of the interaction of highly-accelerated, magnetically-confined protons and ions with the photon field inside the burst, both neutrons and UHE neutrinos are expected to be created: the former escape the source and beta-decay into protons which propagate to Earth, where they are detected as UHECRs, while the latter, if detected, would constitute the smoking gun of hadronic acceleration in the sources. Recently, km-scale neutrino telescopes such as IceCube have finally reached the sensitivities required to probe the neutrino predictions of some of the existing GRB models. On that account, we present here a revised, self-consistent model of joint UHE proton and neutrino production at GRBs that includes a state-of-the-art, improved numerical calculation of the neutrino flux (NeuCosmA); that uses a generalised UHECR emission model where some of the protons in the sources are able to "leak out" of their magnetic confinement before having interacted; and that takes into account the energy losses of the protons during their propagation to Earth. We use our predictions to take a close look at the cosmic ray-neutrino connection and find that the current UHECR observations by giant air shower detectors, together with the upper bounds on the flux of neutrinos from GRBs, are already sufficient to put tension on several possibilities of particle emission and propagation, and to point us towards some requirements that should be fulfilled by GRBs if they are to be the sources of the UHECRs. We further refine our analysis by studying a dynamical burst model, where we find that the different particle species originate at distinct stages of the expanding GRB, each under particular conditions. Finally, we consider a possibility of new physics: the effect of neutrino decay in the flux of UHE neutrinos from GRBs. On the whole, our results demonstrate that self-consistent models of particle production are now integral to the advancement of the field, given that the full picture of the UHE Universe will only emerge as a result of looking at the multi-messenger sky, i.e., at gamma-rays, cosmic rays, and neutrinos simultaneously. / Es ist eine natürliche Annahme, dass die energiereichsten beobachteten Teilchen (> 1018 eV), die ultra-hochenergetische Kosmische Strahlung (UHECRs), möglicherweise in Verbindung mit den leuchtkräftigsten zeitlich beschränkten Ereignissen (> 1052 erg s−1), sogenannten Gammablitzen (GRBs), stehen. Als Folge der Wechselwirkungen zwischen den extrem beschleunigten, in Magnetfeldern gefangenen Protonen und Ionen und den Photonfeldern im Inneren der Gammablitze wer- den sowohl Neutronen als auch UHE Neutrinos erwartet. Erstere köonnen die Quelle verlassen und zerfallen zu Protonen via β-Zerfall, welche zur Erde propagieren und dort als UHECR detektiert werden köonnen, während Letztere, wenn detektiert, den eindeutigen Beweis für die Beschleunigung von Hadronen in besagten Quellen erbringen würden. Vor Kurzem haben km3-große Neutrinoteleskope, wie IceCube, endlich die benötigte Sensitivität erreicht, um die Neutrinovorhersagen für einige existierende GRB-Modelle zu testen. In diesem Zusammenhang präsentieren wir hier ein überarbeitetes, selbstkonsistentes Modell der gemein- samen Produktion von UHE Protonen und Neutrinos in GRBs. Dieses enthält eine hochmoderne, verbesserte numerische Kalkulation des Neutrinoflusses (NeuCosmA), ein verallgemeinertes Emissionsmodell für UHECR, welches darauf beruht, dass einige Protonen direkt aus den Magnetfeldern innerhalb der Quelle entkommen können ohne wechselzuwirken, und bezieht die Energieverluste der Protonen auf ihrem Weg zur Erde mit ein. Wir nutzen unsere Voraussagen, um einen genaueren Blick auf die Verbindung zwischen Kosmischer Strahlung und Neutrinos zu werfen, und stellen fest, dass aktuelle UHECR Beobachtungen mittels gigantischen Luftschauerdetektoren zusammen mit den oberen Schranken auf den Neutrinofluss von GRBs bereits ausreichen, um Widersprüche zu einigen Emissions- und Propagationsmodellen aufzuzeigen, und deuten uns in die Richtung einiger Voraussetzungen, die von GRBs erfüllt sein müssen, sollten diese die Quellen der UHECRs sein. Des Weiteren verfeinern wir unsere Analyse, indem wir ein dynamisches Explosionsmodell studieren, mittels welcher wir herausfinden, dass unterschiedliche Teilchen von bestimmten Phasen des expandieren GRBs stammen, welche durch unterschiedliche Bedingungen charakterisiert sind. Zum Schluss betrachten wir die Möglichkeit von ”neuer Physik”, den Zerfall von UHE Neutrinos im Neutrinofluss von GRBs. Im Großen und Ganzen zeigen unsere Ergebnisse, dass selbstkonsistente Modelle mittlerweile ein integraler Bestandteil für den Fortschritt dieses Feldes geworden sind, wenn man berücksichtigt, dass der Gesamtzusammenhang des UHE Universums erst sichtbar wird, wenn man den Himmel in unterschiedlichen Kanälen betrachtet, genauer gesagt gleichzeitig in Gammastrahlung, in Kosmischer Strahlung und in Neutrinos.

Orientador: Luiz Marcos da Fonseca / Banca: Marcelo Dias Baruffi / Banca: Paulo Inácio da Costa / Resumo: Os receptores para a porção Fc das IgG (FcgR) estão amplamente expressos nas células do sistema imune e podem estimular uma variedade de respostas efetoras. Três classes de FcgR são descritas nos humanos: FcgRI, FcgRII e FcgRIII. O neutrófilo expressa constitutivamente as isoformas FcgRIIa (CD32) e FcgRIIIb (CD16), as quais apresentam um polimorfismo funcional decorrente do polimorfismo alélico. No FcgRIIa, a substituição da histidina (H) pela arginina (R) na posição 131 resulta nas variantes polimórficas FcgRIIa- R131 e FcgRIIa-H131, que diferem quanto à capacidade de ligação à IgG2 humana. Quanto ao FcgRIIIb (CD16), o polimorfismo genético é responsável pela expressão dos antígenos de neutrófilo (NA)1, NA2 e SH e resulta em um maior número de sítios de glicosilação em NA2. O FcgRIIIb é responsável pela aproximação dos ligantes na membrana para o FcgRIIa e também interage com o receptor para complemento tipo 3 (CR3) na superfície celular. A cooperação entre os FcgRIIa/IIIb com o CR3 promove a estimulação máxima das respostas do neutrófilo, dentre elas o burst oxidativo. Uma vez que a interação FcgRIIIb/CR3 ocorre via sítio de ligação lectina-sacarídeo, o objetivo deste estudo foi avaliar se o polimorfismo alélico do FcgRIIIb poderia afetar a cooperação entre os FcgR e os CR em mediar o burst oxidativo dos neutrófilos. As freqüências dos alelos H/R-131 e NA1/NA2/SH foram analisadas por genotipagem com oligonucleotídeos alelo-específicos e reação em cadeia da polimerase e a densidade de expressão dos receptores (FcgRIIa, FcgRIIIb, CR1 e CR3) foi determinada por citometria de fluxo. A distribuição dos genótipos para o FcgRIIIb (n=169) foi NA1/NA2 (52,1%), NA2 (27,8%) e NA1 (20,1%). Dentre 174 indivíduos, apenas 6,3% apresentaram o gene SH. Quanto aos genótipos para o FcgRIIa (n=143), a distribuição... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: Receptors for immunoglobulin G (FcgR) are known to be expressed on many cells of the immune system and they can trigger a variety of biological responses. Human FcgR belong to the Ig superfamily and three classes of these receptors have been recognized: FcgRI, FcgRII and FcgRIIl, with different affinities and specificities for IgG subclasses. Neutrophils express the FcgRIIa (CD32) and FcgRIIlb (CD16) isoforms, which display a functional polymorphism due to biallelic polymorphisms. In the case of FcgRIIa, an arginine (FcgRIIa-R131) or histidine (FcgRIIa-H131) at amino acid position 131 determines receptor affinity for IgG2, FcgRIIa-H131 being the isoform with highest affinity. On neutrophils, the FcgRIIIb bears the neutrophil antigen (NA) polymorphism, NA1, NA2 and SH, NA2 being the more glycosylated isoform. Cooperation of FcgRIIIb with FcgRIIa and CR3 (complement receptor type 3) is necessary for efficient neutrophil responses, including the oxidative burst. Since the FcgRIIIb/CR3 cooperation occurs via lectin-sacharide-like interaction, the aim of this study was to evaluate whether the allelic polymorphism, NA1 and NA2, could influence the cooperation of FcgRIIIb with CR3 in mediating the oxidative burst of neutrophils. FcgRIIa and FcgRIIIb genotyping analysis were performed by polymerase chain reaction with allelespecific primers and surface expressions of FcgRIIa, FcgRIIIb, CR1 and CR3 on neutrophils were determined by flow cytometry. The FcgRIIIb genotype distribution (n=169) was NA1/NA2 (52.1%), NA2 (27.8%) and NA1 (20.1%). SH gene was found in 11 (6.3%) volunteers from 174 subjects. With respect to the FcgRIIa genotype (n=143), the distribution observed was R131 (41.2%), H/R131 (38.5%) and H (20.3%). Neutrophils were stimulated with immune complexes (IC)-IgG opsonized or not with complement and the oxidative burst... (Complete abstract click electronic access below) / Mestre

Rationale: Inadequate monitoring of neuromuscular blockade (NMB) may result in worse patient outcomes, therefore NMB monitor availability is a minimum requirement for perioperative care according to the South African Society of Anaesthesiologists’ (SASA) 2018 Practice Guidelines. The authors performed an audit of peripheral nerve stimulators (PNS) functionality and availability at their institution. In the researcher’s experience the peripheral nerve stimulators (PNS) in use at his institution are not always easily available and some units malfunction at times. There are also not many units that can give a graphical display of a train of four ratio. This observation spurred the idea to do an audit on neuromuscular monitoring at this institution, by focusing on the availability and functionality of peripheral nerve stimulators. Methods: After ethics approval was obtained, an audit was performed. In order to assess function, the PNS were attached to an electrical circuit with a skin equivalent resistance. The resultant current impulses generated using Train-of-Four (TOF) mode and Double Burst Stimulation modes (DBS) were recorded with a voltage scope meter and visually assessed that the TOF was present and appeared equal. PNS availability was assessed in theatre and recovery areas against the SASA guideline standard of nerve stimulator availability. Results: Of the 65 PNS units assessed, 39 units were deemed to be dysfunctional and 26 units fully functional. The most frequent fault found (30 units) related to faulty or absent PNS electrode cables. Eight functional PNS units with TOF ratio display capability were found. The working PNS showed good inter-device peak voltage measurement correlation. Of the 59 areas identified where PNS should be easily available, only 37 areas met the PNS availability criteria suggested in the SASA guidelines. Discussion: This audit revealed that overall there were not enough functional PNS available at the institution, when measured against the SASA standard. The clinical significance of these findings would vary depending on the actual usage rate of NMBs in the area concerned. The logistics of tracking aPNS unit’slocationalso turnsoutto be paramountinsituationswherenerve stimulators have to be shared between areas. From a technical point of view, the working PNS were found to be very consistent in their delivered voltage bursts. Future use of the first generation PNS (without TOF ratio display) will continue to decline, because of their inability to monitor neuromuscular function bymodern standards, and the poor availability ofreplacement parts for models no longer manufactured. The cost and availability of repairs and cable replacementsshould be factored into the decision when acquiring more PNS units. Conclusion: This audit highlighted the need for more new generation PNS with TOF-ratiodisplay- ability to align the institution with the recommendations from SASA standards and the anaesthetic literature. It also highlighted the accuracy and consistency of delivered current bursts by the working PNS devices.

ITC/USA 2006 Conference Proceedings / The Forty-Second Annual International Telemetering Conference and Technical Exhibition / October 23-26, 2006 / Town and Country Resort & Convention Center, San Diego, California / As the integrated Network Enhanced Telemetry (iNET) program moves forward in resolving systems engineering design and architecture definition, critical technology “gaps” and a migration path to realizing the integration of this technology are needed to insure a smooth transition from the current legacy point to point telemetry links to a network oriented telemetry system. Specifically identified by the DoD aeronautical telemetry community is the need for a migration to a network solution for command, control, and transfer of test data by optimizing the physical, data link, and network layers. In this paper, we present a network centric telemetry preliminary architecture approach based on variants of 802.11 that leverages the open standards as well as the previous Advanced Range Telemetry (ARTM) work on the physical layer waveform. We present a burst modem approach based on the recent AOFDM 802.11a work, a TDMA-like MAC layer based on 802.11e, and then add additional MAC layer features to allow for the multi-hop aeronautical environment using a variant of the current working standard of 802.11s. The combined benefits of the variants obtained from 802.11a, 802.11e, and 802.11s address the needs for both spectrum efficiency in the aeronautical environment and the iNET program.

Movies, songs, conferences, video streams and other multimedia services are spreading in everybody’s life, needs and work. Different types of audio and video codecs of various qualities appear to be used for different purposes. However, each codec can be suitable for a special usage, as for example a codec that can be use for high quality film may not be suitable for streaming it into network. The main purpose of this thesis is to compare the performance of different codecs in one particular scenario and indicate which codec performance is the best. The thesis work includes the investigation of several codec aspects (audio and video) and problems related to choosing a multimedia codec (coder/decoder) suitable for large-scale multimedia distribution over the Internet. More specifically, the work focuses on various features of modern media codecs, compares them and finds the best application for each of them. Furthermore, the thesis provides an overview of available research results related to this work and codec comparison tables for codecs and their features. Additionally, as part of this work, a testbed was developed to measure the performance of codecs when used to stream media over a network. The testbed enabled the collection of various QoS parameters, such as bandwidth usage and burst, size for each codec considered in this thesis. / Address: Minervavägen 22A, Room 2, 371 41 Karlskrona, sweden. Cel: +46706456674

Emerging topic detection algorithms have the potential to assist researchers in maintaining awareness of current trends in biomedical fields--a feat not easily achieved with existing methods. Though topic detection algorithms for news-cycles exist, several aspects of this particular area make applying them directly to scientific literature problematic. This dissertation offers a framework for emerging topic detection in biomedicine. The framework includes a novel set of weightings based on the historical importance of each topic identified. Features such as journal impact factor and funding data are used to develop a fitness score to identify which topics are likely to burst in the future. Characterization of bursts over an extended planning horizon by discipline was performed to understand what a typical burst trend looks like in this space to better understand how to identify important or emerging trends. Cluster analysis was used to create an overlapping hierarchical structure of scientific literature at the discipline level. This allows for granularity adjustment (e.g. discipline level or research area level) in emerging topic detection for different users. Using cluster analysis allows for the identification of terms that may not be included in annotated taxonomies, as they are new or not considered as relevant at the time the taxonomy was last updated. Weighting topics by historical frequency allows for better identification of bursts that are associated with less well-known areas, and therefore more surprising. The fitness score allows for the early identification of bursty terms. This framework will benefit policy makers, clinicians and researchers.

Die Emission solarer Typ II Radiobursts ist ein seit Jahrzehnten beobachtetes Phänomen der heliosphärischen Plasmaphysik. Diese Radiobursts, die im Zusammenhang mit der Propagation koronaler Schockfronten auftreten, zeigen ein charakteristisches, zweibandiges Emissionsspektrum. Mit expandierendem Schock driften sie zu niedrigeren Frequenzen. Analytische Theorien dieser Emission sagen nichtlineare Plasmawellenwechselwirkung als Ursache voraus, doch aufgrund des geringen Sonnenabstands der Emissionsregion ist die in-situ Datenlage durch Satellitenmessungen äusserst schlecht, so dass eine endgültige Verifikation der vorhergesagten Vorgänge bisher nicht möglich war. Mit Hilfe eines kinetischen Plasma-Simulationscodes nach dem Particle-in-Cell Prinzip wurde in dieser Dissertation die Plasmaumgebung in der Foreshock-Region einer koronalen Schockfront modelliert. Das Propagations- und Kopplungsverhalten elektrostatischer und elektromagnetischer Wellenmoden wurde untersucht. Die vollständige räumliche Information über die Wellenzusammensetzung in der Simulation erlaubt es, die Kinematik nichtlinearer Wellenkopplungen genauestens zu untersuchen. Es zeigte sich ein mit der analytischen Theorie der Drei-Wellen-Wechselwirkung konsistentes Bild der Erzeugung solarer Radiobursts: durch elektromagnetischen Zerfall elektrostatischer Moden kommt es zur Erzeugung fundamentaler, sowie durch Verschmelzung gegenpropagierender elektrostatischer Moden zur Anregung harmonischer Radioemission. Kopplungsstärken und Winkelabhängigkeit dieser Prozesse wurden untersucht. Mit dem somit zur Verfügung stehenden, numerischen Laborsystem wurde die Parameter-Abhängigkeit der Wellenkopplungen und entstehenden Radioemissionen bezüglich Stärke des Elektronenbeams und des solaren Abstandes untersucht. / The emission of solar type II radiobursts is a phenomenon of heliospheric plasma physics which has been observed for several decades. These radio bursts, which appear in conjunction with propagating coronal shocks, show a characteristic two-banded emission spectrum, drifting towards lower frequencies as the shock expands. Analytic theories predict nonlinear plasma wave interaction as the cause of these emissions. However, due to its low solar distance, in-situ satellite measurements of the emission regions’ properties are extremely scarce. Hence, a conclusive verification of the predicted processes was hitherto not attainable. Using a kinetic plasma simulation code based on the particle-in-cell approach, the plasma environment in a coronal shock’s foreshock region was modelled in this thesis. The propagation and coupling behaviour of electrostatic and electromagnetic wavemodes was investigated. Complete spatial information of the wave composition as obtainable from the simulations allowed to finely analyze the kinematics of nonlinear wave interactions. The results showed excitation of solar radiobursts in agreement with analytics predictions of three wave interaction processes, based on the nonlinear processes: electromagnetic decay of electrostatic modes is responsible for the fundamental and coalcescense of counterpropagating electrostatic waves responsable for the harmonic radio emission. Coupling strengths and angular dependences of these processes were then studied. With the numerical laboratory system obtained through this modelling effort, the parameter dependence of wave copulings and resulting radio emissions were explored, based on variation of electron beam strength and solar distance of the emission region.

In this work, we take a look at the connection of gamma-ray bursts (GRBs) and ultra-high-energy cosmic rays (UHECR) as well as the possibilities how to verify this connection. The currently most promising approach is based on the detection of high-energy neutrinos, which are associated with the acceleration of cosmic rays. We detail how the prompt gamma-ray emission is connected to the prediction of a neutrino signal. We focus on the interactions of photons and protons in this regard. At the example of the current ANTARES GRB neutrino analysis, we show the differences between numerical predictions and older analytical methods. Moreover, we discuss the possibilities how cosmic ray particles can escape from GRBs, assuming that UHECR are entirely made up of protons. For this, we compare the commonly assumed neutron escape model with a new component of direct proton escape. Additionally, we will show that the different components, which contribute to the cosmic ray flux, strongly depend on the burst parameters, and test the applicability on some chosen GRBs. In a further step, we continue with the considerations regarding the connection of GRBs and UHECR by connecting the GRB source model with the cosmic ray observations using a simple cosmic ray propagation code. We test if it is possible to achieve the observed cosmic ray energy densities with our simple model and what the consequences are regarding the prompt GRB neutrino flux predictions as well as the cosmogenic neutrinos. Furthermore, we consider the question of neutrino lifetime and how it affects the prompt GRB neutrino flux predictions. In a final chapter, we show that it is possible to apply the basic source model with photohadronic interactions to other types of sources, using the example of the microquasar Cygnus X-3. / In dieser Arbeit beschäftigen wir uns mit dem Zusammenhang von Gammablitzen (GRBs) und ultra-hochenergetischer kosmischer Strahlung (UHECR) sowie mit den Möglichkeiten, wie dieser Zusammenhang überprüft werden kann. Der zur Zeit erfolgsversprechendste Ansatz basiert auf der Detektion von hochenergetischen Neutrinos, die mit der Beschleunigung von kosmischer Strahlung assoziiert werden. Wir zeigen detailliert, wie die prompte Emission im Bereich der Gammastrahlung mit der Voraussage eines Neutrinosignals zusammenhängt. Ein besonderes Augenmerk legen wir hierbei auf die Wechselwirkung von Photonen und Protonen. Am Beispiel der aktuellen Analyse des ANTARES Neutrinoteleskops zu Neutrinos von Gammablitzen zeigen wir, wie sich numerische Voraussagen von älteren analytischen Methoden unterscheiden. Des Weiteren diskutieren wir Möglichkeiten, wie die Teilchen der kosmischen Strahlung aus einem Gammablitz entkommen können, wenn die ultra-hochenergetische kosmische Strahlung nur aus Protonen bestehen würde. Wir vergleichen dazu das meistens angenommene Entkommen in Form von Neutronen mit einer neuen Komponente von direkt ausströmenden Protonen. Auch zeigen wir, dass die unterschiedlichen Komponenten, die zur kosmischen Strahlung beitragen, stark von den verwendeten Parametern der Gammablitze abhängen, und uberprüfen die Modelle an einigen ausgewählten Gammablitzen. In einem weiteren Schritt führen wir die Überlegungen zu dem Zusammenhang von Gammablitzen und ultra-hochenergetischer kosmischer Strahlung fort, in dem wir mittels eines einfachen Propagationscodes für kosmische Strahlung eine Verbindung zwischen dem Quellmodell für Gammablitze und den Beobachtungsdaten der kosmischen Strahlung herstellen. Wir überprüfen, inwieweit sich die beobachteten Energiedichten der kosmischen Strahlung mittels unseres einfachen Modells realisieren lassen und welche Konsequenzen dies für die Voraussagen der prompten Neutrinoemission von Gammablitzen sowie den kosmogenischen Neutrinos hat. Außerdem gehen wir der Frage nach, wie die vorausgesagten prompten Neutrinoflüsse von einer endlichen Lebenszeit der Neutrinos beeinflusst werden würden. In einem letzten Kapitel übertragen wir das verwendete grundlegende Quellmodell mit photohadronischen Wechselwirkungen auf eine andere Klasse von Quellen, am Beispiel von Voraussagen fürden Mikroquasar Cygnus X-3.