L’expérience H.E.S.S. (High Energy Spectroscopic System) composée de cinq télescopes Tcherenkov observe le ciel en rayons gamma au-delà d'une centaine de GeV jusqu'à plusieurs dizaines de TeV. Les rayons gamma sont produits par des phénomènes non-thermiques parmi les plus violents dans l'univers au voisinage d'objets astrophysique comme les pulsars, supernovae ou trous noirs, mais pourraient être également produits par l'annihilation de particules de matière noire.De nombreuses sondes cosmologiques et astrophysiques suggèrent que 85% de la matière dans l'Univers est d'origine inconnue. Cette matière appelée matière noire, de nature non baryonique, serait constituée de particules non encore découvertes dont les candidats privilégiés seraient des particules massives interagissant faiblement (WIMPs) avec la matière ordinaire, particules prédites au-delà du Modèle Standard de la physique des particules.Des particules de matière noire peuvent s'annihiler en particules du Modèle Standard dans les régions denses de l'Univers. Parmi les produits d'annihilations se trouvent les photons dont la détection à hautes énergies par des télescopes au sol à effet Tcherenkov pourrait apporter des informations uniques sur la nature de la matière noire.H.E.S.S. observe des régions du ciel dense en matière noire comme le Centre Galactique et des galaxies naines satellites de la Voie Lactée.Une interprétation d'un excès de rayons gamma détecté au Centre Galactique par H.E.S.S. en termes d’accélération de protons par une population de pulsars millisecondes est présenté.10 ans d'observations du Centre Galactique avec le réseau H.E.S.S. I de quatre télescopes, cinq ans de prise de données vers la région du Centre Galactique avec le réseau complet H.E.S.S. II, et un jeu de deux ans de données vers des galaxies naines découvertes récemment sont analysés. Les recherches de signaux d'annihilation de matière noire vers ces cibles ont produit les limites plus fortes à présent sur la section efficace d'annihilation de matière noire dans la plage en masse du TeV. Le potentiel de détection de matière noire avec le futur réseau de télescopes CTA (Cherenkov Telescope Array) vers la région central du halo Galactique est étudiés. / The H.E.S.S. (High Energy Spectroscopic System) experiment is an array of five Cherenkov telescopes that observe the sky in gamma-rays from about 100 GeV up to several ten TeV.Gamma rays are produced in violent non-thermal phenomena in the Universe in the neighborhood of pulsars, supernovae, black holes, ..., and could also be produced by the annihilation of dark matter particles.Numerous cosmological and astrophysical probes suggest that 85% of the total matter budget in the Universe is of unknown origin. This component of matter known as dark matter is non baryonic and could consist of yet undiscovered particles which privileged candidates are arguably massive particles with electroweak couplings with ordinary matter (WIMPs).Dark matter particles may annihilate into Standard Model particles in dense regions of the Universe. Among the annihilation products are photons which detection at high energy with ground-based Cherenkov telescopes could bring unique information on the nature of the dark matter.H.E.S.S. observes dark-matter-dense regions of the sky such as the Galactic Center and dwarf galaxy satellites of the Milky Way. A study on the interpretation of an excess of gamma-rays detected by H.E.S.S. at the Galactic Center in terms of acceleration of protons by a population of unresolved millisecond pulsars is performed.10 years of observations of the Galactic Center with the four-telescope H.E.S.S.-I array, five years of data taking towards the Galactic Center region with the full H.E.S.S.-II array and a two-years dataset towards newly discovered dwarf spheroidal galaxies are analyzed. The search for dark matter annihilation signals towards these targets provided the strongest limits so far on dark matter annihilation cross section in gamma rays of TeV energies. The potential of dark matter detection with the upcoming Cherenkov Telescope Array (CTA) towards the inner Galactic halo are studied. They may annihilate into Standard Model particles in dense regions of the Universe. Among the annihilation products are high energy photons. The detection of these photons with ground-based Cherenkov telescopes may reveal the nature of the dark matter. H.E.S.S. have observed some dark-matter-dense regions of the sky likethe Galactic Center and dwarf galaxies satellites of the Milky Way. In this work 10 years of observations of the Galactic Center with the four-telescopes H.E.S.S.-I array, five years of data taking towards the Galactic Center region with the full H.E.S.S.-II array and a two-years dataset towards newly discovered dwarf spheroidal galaxies are analyzed. The searches for dark matter annihilation signals towards these targets produced the strongest limits so far on dark matter annihilation cross section in gamma rays of TeV energies.Perspectives of dark matter detection with the future array CTA (Cherenkov Telescope Array) towards the inner Galactic halo are also discussed. A study on the interpretation of an excess of gamma-rays detected by H.E.S.S. at the Galactic Center in terms of acceleration of protons by a population of unresolved millisecond pulsars complements the dark matter searches.

In this thesis we present new results for the 99.9% confidence level flux upper limits on the pulsed VHE gamma ray signal coming from the Crab pulsar. In order to achieve optimum hadronic background suppression we implement a new neural network based selection technique and apply it to Cherenkov shower imaging data from the WHIPPLE 10m IACT telescope at Mount Hopkins Arizona. Special emphasis will be given to the fact that the neural network selector is trained with real data exclusively. An energy estimator for gamma ray induced extensive air shower events has been derived from Monte Carlo simulations using the Monte Carlo framework GrISU. This estimator, applied to the image data, serves as input to the neural set selector and is needed to determine the energy dependent flux upper limits. We compare our results to the results from previous studies and the performance of our neural network selection technique to the so-called Supercuts and Optimized Supercuts methods.The new flux upper limits and the new technique show the potential to settle the question about the production mechanism of pulsar radiation. However, the current analysis does not answer this question fully.

Title: Point defects in materials for detection of X-ray and gamma radiation Author: Martin Rejhon Department: Institute of Physics of Charles University Supervisor: prof. Ing. Jan Franc, DrSc., Institute of Physics of Charles Uni- versity Abstract: Cadmium telluride and its compounds are suitable materials for pro- duction of X-ray and gamma-ray detectors working at room temperature. How- ever, the detector quality is affected by material imperfections, such as crystal defects and impurities. It results into forming of deep levels which act as re- combination and trapping centers. Then, the accumulated space charge at these deep levels influences electric and spectroscopic properties of the detector. In the end it may result in the polarization effect, when the electric field is localized in vicinity of one contact and detection properties are decreased. This thesis reports a complex study of a detector band structure by various meth- ods with focus on differences between CdTe, CdZnTe, CdTeSe and CdZnTeSe. The electro-optic Pockels effect is used to investigate the influence of the illumi- nation in range 900 − 1800 nm on the inner electric field. The temperature and time evolutions of the electric field after application of bias or switching of the additional light at 940 nm were measured to determine deep levels...

<p dir="ltr">Neutron star mergers generate powerful gravitational waves and various types of electromagnetic signals, including gamma-ray bursts (GRB), kilonovae, and their afterglows. Observing and modeling these signals help us understand the physical processes of the merger events. Radiation from mergers can also serve as probes to study nuclear physics and cosmology. In this report, I focus on two types of signals: the GRB afterglow and the kilonova. GRB afterglows are non-thermal radiation produced by the interaction of relativistic jets and circumburst material, where the jets are launched perpendicular to the merger plane. Kilonovae are the thermal radiation emitted from the hot materials ejected during the merger. Besides the modeling of these objects, I also investigate their application in multimessenger astrophysics, especially the constraint on the expansion rate of the Universe. </p><p dir="ltr">First, I developed a GRB afterglow model to account for the off-axis observation of a structured jet. Using a jet structure derived from a three-dimensional general relativistic magnetohydrodynamic simulation, we performed a joint analysis of the multimessenger data of the neutron star merger event GW170817, including the gravitational wave data and GRB afterglow data in the radio band. We have tightly constrained the observing angle of GW170817 and broken the degeneracy between the inclination angle and luminosity distance measured in gravitational waves. With a better constrained distance, we improved the standard siren measurement of the Hubble constant to $H_0 = 69.5\pm 4\ \mathrm{km\ s^{-1}\ Mpc^{-1}}$. The error bar has been reduced by a factor of 2. This work demonstrates that the modeling of off-axis GRB afterglow can significantly improve the standard siren method, provided that we have a reliable jet structure.</p><p dir="ltr">Second, I upgrade the GRB afterglow model in the first work, extending it to the late time where lateral spreading of the GRB jet becomes important. In this model, the ultra-relativistic blastwave is approximated by an infinitely thin two-dimensional surface. With this approximation, the hydrodynamic equations can be analytically integrated over the radius. Further assuming axial symmetry, the three-dimensional hydrodynamic simulation can be reduced to one dimension, which significantly increases the computational efficiency. We have compared our method to full numerical simulations and existing GRB afterglow modeling tools. The comparison shows good agreement and verifies our approach. Compared to these tools, our model has better flexibility and is applicable in a broader context. This method has been developed into a numerical code, \texttt{jetsimpy}, which we have provided to the community. It will serve as a powerful tool in the era of multimessenger astrophysics.</p><p dir="ltr">Finally, I investigate the possibility of long-lived massive neutron stars as neutron star merger remnants. A long-lived massive neutron star can inject a significant amount of energy into the merger ejecta, boosting the luminosity of kilonova by several orders of magnitude. However, this type of event has not yet been observed in optical sky surveys. We developed a boosted kilonova model with a detailed calculation of the photoionization process to better describe the efficiency of energy injection from spin down power to the ejecta. Our study found that boosted kilonovae, if commonly occurring, they should have already been observed given the accumulated time in sky surveys. As a result, the absence of detection implies that long-lived massive neutron stars as neutron star merger remnants are likely to be rare in the Universe.</p>

Durch die Kopplung von Szintillationskristallen an Lichtwellenleiter könnten robuste Messgeräte für die spektroskopitsche Messung von Strahlungsfeldgrößen in Bohrlöchern in Betonstrukturen beim Rückbau von Kernkraftwerken realisiert werden. In dieser Arbeit wurden zwei Prototypen solcher Messgeräte entwickelt, wobei ein auf einem Gadolinium-Aluminium-Gallium-Granat-Szintillationskristall basierendes Messsystem mit einem Kunststofflichtwellenleiter mit hohem Durchmesser aufgrund seiner hohen Zählrate bevorzugt wurde. Mit diesem Messystem konnten spektroskopische Messungen von Gammastrahlung durchgeführt werden. Weiterhin konnte gezeigt werden, dass Kontaminationen einer bestimmten Aktivität bis in einen Abstand von mehreren Zentimetern von der Messsonde im Beton nachweisbar sind. Ein Schätzwert der minimale Messzeit zur Erkennung einer nachweisbaren Kontamination konnte bestimmt werden. Eine hinreichend große, gemessene Ereigniszahl ermöglicht zusätzlich die Bestimmung des Abstands einer radioaktiven, punktförmigen Kontamination eines bekannten Nuklids. Für ein bekanntes Nuklid konnte weiterhin aus der Zählrate ein Schätzwert für die Energiedosis am Ort der Messsonde mithilfe von Referenzmessungen der Dosis mittels Berylliumoxid-Detektoren bestimmt werden.:Inhaltsverzeichnis Abbildungsverzeichnis vii Tabellenverzeichnis ix 1 Einleitung 1 2 Physikalische Grundlagen 3 2.1 Radioaktiver Zerfall 3 2.2 Gröÿen des Strahlungsfelds 3 2.3 Wechselwirkungen von Photonen mit Materie 5 2.4 Lichtentstehung in anorganischen Szintillatoren 8 2.5 Lichtmessung 10 2.6 Pulshöhenverteilungen von Szintillationsdetektoren 12 2.7 Ein ussfaktoren der Lichtausbeute 14 3 Material und Methoden 16 3.1 Aufbau LSO-Sonde und Messungen mit radioaktiven Quellen 16 3.2 Aufbau Lichtkopplung mittels Linse 18 3.3 Aufbau und Versuchsablauf Quarzglaskopplungen 20 3.4 Aufbau GAGG-Sonde 21 3.5 Aufbau des Betonphantoms 24 3.5.1 Dichtebestimmung des Betonphantoms 24 3.6 Messablauf Tiefenkurven in Betonphantom 27 3.7 Datenanalyse mittels Kolmogorv-Smirnov-Test 27 4 Ergebnisse 29 4.1 Spektroskopische Eigenschaften LSO-Sonde 29 4.2 Winkelverteilung austretender Photonen aus Szintillationskristall 33 4.3 Quarzglaskopplung 36 4.4 Spektroskopische Eigenschaften GAGG-Sonde 43 4.5 Vergleich GAGG- und LSO-Sonde 47 4.6 Abstandsabhängigkeit der Zählrate 50 4.7 Abschätzung der maximalen Abschirmdicke von Beton für Kontaminationserkennung 53 4.8 Abschätzung der minimalen Messzeit zur Kontaminationserkennung 56 4.9 Abschirmungsdickenbestimmung mittels Abschirmungsparameter 57 4.10 Bestimmung der Dosis 62 5 Diskussion 64 6 Zusammenfassung 67 / A robust measuring system for spectroscopic measurementes of gamma-ray radiation in boreholes in concrete structures can be built by coupling of a scintillation crystal to a light guide. Two prototypes of such measuring systems are developed one based on a Gadolinium-Aluminium-Gallium-Garnet scintillation crystal with a plastic optical fiber with a high diameter is preferred due to the higher count rate. Spectroscopic measurements of gamma-ray radiation with this measuring system can be performed. It can be shown that contamination of a specific activity can be detected even if they are located in concrete in a distance of several centimeters from the radiation sensor. for the minimal measurement time of 38 s An estimated value to detect a traceable contamination could be determined. If a high number of events can be detected, even the distance between a point like radioaktive source of a known nuclide and the radiation sensor can be determined. An estimated value for the applied dose at the place of the radiation sensor could be determined for a known nuclide with the help of the count rate. Therefore, reference measurements of dose with berylliumoxide detectors were performed.:Inhaltsverzeichnis Abbildungsverzeichnis vii Tabellenverzeichnis ix 1 Einleitung 1 2 Physikalische Grundlagen 3 2.1 Radioaktiver Zerfall 3 2.2 Gröÿen des Strahlungsfelds 3 2.3 Wechselwirkungen von Photonen mit Materie 5 2.4 Lichtentstehung in anorganischen Szintillatoren 8 2.5 Lichtmessung 10 2.6 Pulshöhenverteilungen von Szintillationsdetektoren 12 2.7 Ein ussfaktoren der Lichtausbeute 14 3 Material und Methoden 16 3.1 Aufbau LSO-Sonde und Messungen mit radioaktiven Quellen 16 3.2 Aufbau Lichtkopplung mittels Linse 18 3.3 Aufbau und Versuchsablauf Quarzglaskopplungen 20 3.4 Aufbau GAGG-Sonde 21 3.5 Aufbau des Betonphantoms 24 3.5.1 Dichtebestimmung des Betonphantoms 24 3.6 Messablauf Tiefenkurven in Betonphantom 27 3.7 Datenanalyse mittels Kolmogorv-Smirnov-Test 27 4 Ergebnisse 29 4.1 Spektroskopische Eigenschaften LSO-Sonde 29 4.2 Winkelverteilung austretender Photonen aus Szintillationskristall 33 4.3 Quarzglaskopplung 36 4.4 Spektroskopische Eigenschaften GAGG-Sonde 43 4.5 Vergleich GAGG- und LSO-Sonde 47 4.6 Abstandsabhängigkeit der Zählrate 50 4.7 Abschätzung der maximalen Abschirmdicke von Beton für Kontaminationserkennung 53 4.8 Abschätzung der minimalen Messzeit zur Kontaminationserkennung 56 4.9 Abschirmungsdickenbestimmung mittels Abschirmungsparameter 57 4.10 Bestimmung der Dosis 62 5 Diskussion 64 6 Zusammenfassung 67

Gamma Ray Burst (GRB) are very bright cosmological explosions signalling the catastrophic formation of a black hole. Therefore, they act like real light beacons that could be detected through-out the Universe and be used as probes to study the contents and phases of the early Universe. However, only a handful sample is known so far. This is for two reasons: instrumental biases that may prevent their detection and the difficulty to find a near Infrared counterpart preventing their redshift measurements. The wide-field trigger camera ECLAIRs to-fly on-board the Space-based multi-band Variable Object Monitor (SVOM) mission will detect γ-/X-ray transients down to energies of 4 keV, as well as creating an alert for multi-wavelength/messenger follow-ups. My study focuses on analysing how ECLAIRs will detect GRBs, and more particularly high-redshift GRBs, based on a well-selected sample of GRBs with redshift measurement associated (see Section 2). Studying how ECLAIRs will see them may help identifying possible instrument biases as well as common observational characteristics for such GRBs that may be used in turn to recognise such special GRBs once SVOM will be launched. Using software tools developed within the ECLAIRs collaboration, I built an end-to-end simulator which I used to simulate the detection by ECLAIRs of the GRBs in the sample at their original redshift and higher redshifts (up to z = 15). I implemented a suited version of the count-rate trigger on-board ECLAIRs to assess the detectability of these bursts, and I retrieved their duration over the background when detected (see Section 2). The analysis shows good performance for detecting high-redshift GRBs in the centre of the Field of View (fully-coded), but significantly reduced, in comparison to other GRBs, for partially-coded detection. 5 of the GRBs with z &gt; 3.83 present a successful detection up to at least z = 15 (see Section 3). The retrieved rest-frame duration of a GRB remains constant for several redshifts in the simulations if the detected burst did not present a low-flux emission in their lightcurve, which is common for high redshift GRBs. On the other hand, if the original lightcurve of a burst presents this low-flux emission, it becomes buried in noise when simulating it at higher redshifts. This confirms the tip-of-the-iceberg detection bias which depends on the lightcurve burst morphology, and it may explain why the current sample seems to present lower burst durations at higher redshifts.

Missing page viii. Page 171 was repeated with different text. / <p> The decay of 14.9 min. ⁸⁹Rb to levels in ⁸⁹Sr has been studied by use of Ge(Li) detectors, NaI(Tl) detectors and a magnetic beta ray spectrometer. Fourteen gamma rays have been studied by ɣ-ɣ and β-ɣ coincidence experiments and establish levels at 0, 1.031, 2,000, 2.277, 2.567, 2.708, 2.770, 3.225 and 3.500 MeV. The Q value is 4.486 ± .012 Mev. </p> <p> The techniques of beta and gamma ray spectroscopy using Ge(Li), NaI(Tl) and plastic beta detectors have been applied in the study of the decay of 3.2 min. ⁸⁹Kr to levels in ⁸⁹Rb. Seventy nine of the one hundred and eleven observed gamma rays have been classified in the proposed decay scheme. The Q value is 5.15 ± .03 MeV. </p> / Thesis / Doctor of Philosophy (PhD)

Trotz der beeindruckenden Fortschritte, die die Röntgen- und Gammastrahlenobservatorien in den letzten Jahrzehnten erzielt haben, ist der Energiebereich zwischen 200 keV und 50 MeV nach wie vor kaum erforscht. Diese Lücke, die in der Literatur oft als ``MeV-Lücke'' bezeichnet wird, ist nicht auf einen Mangel an überzeugender Wissenschaft zurückzuführen, sondern auf technische Herausforderungen und Nachweisschwierigkeiten, die mit MeV-Beobachtungen einhergehen. COMPTEL an Bord von CGRO (1991-2000) war das letzte Teleskop, das eine vollständige Durchmusterung des MeV-Himmels mit einer relativ bescheidenen Empfindlichkeit durchführte. Für die Zukunft sind zahlreiche Missionen vorgeschlagen worden, insbesondere AMEGO, die die Leistung von COMPTEL um mindestens eine Größenordnung verbessern sollen. Der Zeitrahmen für die Entwicklung, den Aufbau und den Start solch großer Missionen beträgt jedoch etwa 10 Jahre und ist mit erheblichen Kosten verbunden. In diesem Szenario könnte ein viel kleinerer Satellit, der sich der neuen Welle von schnellen, relativ kostengünstigen Weltraumforschungsmissionen anschließt, die durch CubeSats ermöglicht werden, in kürzerer Zeit rentabel sein. In dieser Arbeit werden die Verfügbarkeit und die Leistung eines Compton-Teleskops auf der Grundlage des CubeSat-Standards, genannt MeVCube, untersucht. Die Auswirkungen der Materialwahl und verschiedener CubeSat-Nutzlasten wurden durch Simulationen bewertet. Trotz der begrenzten Größe kann selbst ein kleines Teleskop, das auf einem CubeSat fliegt, den Energiebereich von Hunderten von keV bis zu einigen MeV mit einer Empfindlichkeit abdecken, die mit der der letzten Generation von Großmissionen wie COMPTEL und INTEGRAL vergleichbar ist. Es wurden auch experimentelle Messungen an Cadmium-Zink-Tellurid-Halbleiterdetektoren und einer für den Weltraumbetrieb geeigneten Ausleseelektronik mit geringem Stromverbrauch durchgeführt. / Despite the impressive progresses achieved both by X-ray and gamma-ray observatories in the last decades, the energy range between 200 keV and 50 MeV remains poorly explored. This gap in coverage, often referred in literature as the ``MeV gap'', is not due to lack of compelling science, but instead to technical challenges and detection difficulties that comes with MeV observations. COMPTEL, on-board CGRO (1991-2000), was the last telescope to accomplish a complete survey of the MeV-sky with a relatively modest sensitivity. Many missions have been proposed for the future, most notably AMEGO, aiming to improve COMPTEL's performance by at least one order of magnitude. However, the timescale for development, assembly and launch of such large missions is around 10 years, with substantial costs. Looking at this scenario, a much smaller satellite, joining the new wave of rapid, relatively inexpensive space science missions enabled by CubeSats, may be profitable on a shorter time-scale. This thesis evaluates the availability and performance of a Compton telescope based on the CubeSat standard, named MeVCube. The impact of material choice and different CubeSat payloads has been evaluated through simulations. Despite the limited size, even a small telescope flying on a CubeSat can cover the energy range from hundreds of keV up to few MeVs with a sensitivity comparable to that of the last generation of large-scale missions like COMPTEL and INTEGRAL. Experimental measurements on Cadmium-Zinc-Telluride semiconductor detectors and low-power read-out electronics suitable for space operation have been performed as well.

Gammastrahlenblitze (Gamma-Ray Bursts, GRBs) gehören zu den energiereichsten transienten Ereignissen im Universum und werden als mögliche Quellen von ultra-hochenergetischen kosmischen Strahlen (Ultra-High-Energy Cosmic Rays, UHECRs) gehandelt. Eine eindeutige Bestätigung durch UHECR-Messungen ist jedoch schwierig, da die Richtungsinformation der kosmischen Strahlen während ihrer Ausbreitung aufgrund von Ablenkung durch Magnetfelder teilweise verloren geht. In dieser Dissertation folgen wir einem alternativen multi-messenger Ansatz in welchem die Anwesenheit von kosmischen Strahlen in einem astrophysikalischen Objekt durch Neutrino- oder Photon-Signaturen angezeigt wird. Hierfür simulieren wir GRBs im Internal-Schock-Szenario, welches verschiedene Emissionszonen entlang des astrophysikalischen Jets erfasst, und berechnen nukleare Wechselwirkungen mit modernsten numerischen Codes. In diesem Rahmen diskutieren wir unter welchen Voraussetzungen die Quellklasse von GRBs UHECR-Daten beschreiben kann ohne Neutrinolimits. Letzere begründen sich im Mangel an gemessenen hoch-energetischen (High-Energy, HE) Neutrinos, die mit bekannten GRBs assoziert werden konnten. Die Neutrinolimits können alternativ in Objekten niedriger Leuchtkraft eingehalten werden, die typischerweise eine niedrige Neutrinoproduktionseffizienz haben. Wir präsentieren leptonische Strahlungsmodellierungen für die Unterklasse von GRBs niedriger Leuchktraft mit einem Fokus auf sehr hoch-energetischer (Very-High-Energy, VHE) Emission welche von aktuellen/zukünfitgen Instrumenten beobachtet werden könnte und bestimmen wir die maximalen Energien verschiedener Atomkerne. Die Präsenz von Hadronen kann alternativ durch Signaturen in verschiedenen Wellenlängen des Photonspektrums angezeigt werden. Wir erforschen diesen Ansatz in lepto-hadronischen Modellen für GRBs mit hoher Leuchtkraft, wobei wir kritisch diskutieren, welche Bedingungen erfüllt sein müssen damit typische GRB-Spektren reproduziert werden können. / Gamma-Ray Bursts (GRBs) are among the most energetic transients in the Universe and candidate sources of Ultra-High-Energy Cosmic Rays (UHECRs). A clear confirmation from UHECR measurements is however challenging, as the directional information of cosmic rays is partially lost due to deflection by (inter-)galactic magnetic fields. In this dissertation we follow an alternative multi-messenger approach, in which the presence of UHECRs in an astrophysical object is indicated by neutrino or photon signatures produced in nuclear interactions. For this, we simulate GRBs in the multi-zone internal shock model, which accounts for different emission zones along the astrophysical jet and calculate nuclear interactions with state-of-the-art numerical codes. In this framework we discuss under which conditions the population of GRBs can still account for UHECR measurements while obeying current neutrino limits that stem from the lack of detected High-Energy (HE) neutrinos which could be associated with known GRBs. These neutrino limits may alternatively be met in low-luminosity objects, which typically have low neutrino production efficiency. We present leptonic radiation models of the sub-class of low-luminosity GRBs, with a focus on Very-High-Energy (VHE) emission potentially observable by current/future instruments. Connecting to UHECRs, we determine maximal energies of different cosmic-ray nuclei. The presence of nuclei may also be indicated by multi-wavelength signatures in the photon spectrum. We explore this approach in lepto-hadronic models of high-luminosity bursts, where we also critically review the conditions necessary to reproduce typical GRB spectra within our model.

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