The CNO cycle consists of a set of nuclear reactions that convert hydrogen into helium and releases energy in stars. The cycle contributes less than 1% to our Sun's luminosity, but it is responsible for detectable neutrino fluxes that can bring direct information of the physical conditions in the solar core, provided that the nuclear reaction rate is known with sufficient precision. The 14N(p,γ)15O is the slowest reaction in the CNO cycle and estabilishes its rate. The experimental study has been performed both at the LUNA 400 kV accelerator deep underground in the Gran Sasso mountain in Italy and at a 3 MV Tandetron in the Helmholtz-Zentrum Dresden-Rossendorf. A proton beam was sent on solid TiN targets and the prompt photons were collected by a composite HPGe detector (at LUNA) or by up to four HPGe detectors (Dresden). The obtained results improve the fit of the excitation function in the R-matrix framework, that is used to extrapolate the S-factor at the very low astrophysical energies. In addition, the strength of two resonances at Ep = 430 and 897 keV of the 15N(p,αγ)12C reaction were measured, improving the precision for hydrogen depth profiling.

Neutrino astronomy is expanding into the ultra-high energy (>1017eV) frontier with the use of in-ice detection of Askaryan radio emission from neutrino-induced particle showers. There are already pilot arrays for validating the technology and the next few years will see the planning and construction of IceCube-Gen2, an upgrade to the current neutrino telescope IceCube. This thesis aims to facilitate that planning by providing faster simulations using deep learning surrogate models. Faster simulations could enable proper optimisation of the antenna stations providing better sensitivity and reconstruction of neutrino properties. The surrogates are made for two parts of the end-to-end simulations: the signal generation and the signal propagation. These two steps are the most time-consuming parts of the simulations. The signal propagation is modelled with a standard fully connected neural network whereas for the signal generation a conditional Wasserstein generative adversarial network is used. There are multiple reasons for using these types of models. For both problems the neural networks provide the speed necessary as well as being differentiable -both important factors for optimisation. Generative adversarial networks are used in the signal generation because of the inherent stochasticity in the particle shower development that leads to the Askaryan radio signal. A more standard neural network is used for the signal propagation as it is a regression task. Promising results are obtained for both tasks. The signal propagation surrogate model can predict the parameters of interest at the desired accuracy, except for the travel time which needs further optimisation to reduce the uncertainty from 0.5 ns to 0.1 ns. The signal generation surrogate model predicts the Askaryan emission well for the limited parameter space of hadronic showers and within 5° of the Cherenkov cone. The two models provide a first step and a proof of concept. It is believed that the models can reach the required accuracies with more work.

Das Hauptziel dieser Arbeit ist die Charakterisierung extrem starker Quellen, die höchstwahrscheinlich die kosmische Strahlung beschleunigen. In dieser Arbeit wurden VHE-Gammastrahlenbeobachtungen mit den MAGIC-Teleskopen verwendet, um die Eigenschaften von Blazaren zu untersuchen. Um die Mechanismen zu untersuchen, die zur Breitbandemission von Blazaren führen, wird ein stationärer lepto-hadronischer Code unter Verwendung eines einfachen semianalytischen Frameworks entwickelt. Daher implementiert der Code neben den leptonischen Wechselwirkungen auch die relevanten hadronischen Wechselwirkungskanäle: Protonensynchrotronstrahlung, Photo-Meson-Wechselwirkungen, Proton-Proton-Wechselwirkungen und Paarkaskaden. Die Dissertation präsentiert die Ergebnisse derMAGIC- und Multiwellenlängen-Monitoring-Kampagne des Blazars 1ES 1959 + 650 im Jahr 2016. Im Jahr 2016 durchlief die Quelle eine äußerst aktive Phase und zeigte am 13. Juni, 14. Juni und 1. Juli 2016 drei bemerkenswert helle VHE-Gammastrahlenfackeln. Um die Breitbandspektren der Quelle während der bemerkenswerten Fackelaktivitäten zu untersuchen, wurden drei verschiedene theoretische Modelle übernommen: leptonisch, hadronisch und gemischt lepto-hadronisch. Sowohl das hadronische als auch das gemischte leptohadronische Modell ergaben während der intensiven Aktivitätsperiode Neutrinoflüsse, die unter der Empfindlichkeit der gegenwärtigen Generation von Neutrinoteleskopen liegen. Die Beobachtung eines hochenergetischen Neutrinos durch IceCube im räumlichen und zeitlichen Zusammentreffen mit einem aufflammenden Blazar mit dem Namen TXS 0506 + 056 ergab 2017 erstmals Hinweise auf Identifizierung einer extragalaktischen kosmischen Strahlenquelle. Die Modellierung der elektromagnetischen Daten und des vorhergesagten Neutrinoflusses impliziert, dass die Quelle tatsächlich ein potenzieller Neutrinostrahler und damit ein Beschleuniger für energiereiche kosmische Strahlen sein könnte. / The main aim of this thesis is to characterize extremely powerful sources that are most likely accelerating cosmic rays. Cosmic-ray sources are also believed to produce photons and neutrinos that act as direct tracers of their sources of origin. In this thesis VHE gamma-ray observations by the MAGIC telescopes were used to study the properties of blazars. To investigate the mechanisms giving rise to the broadband emission from blazars, a stationary lepto-hadronic code is developed using a simple semi-analytical framework. Hence along with the leptonic interactions, the code also implements the relevant hadronic interaction channels: proton synchrotron radiation, photo-meson interactions, proton-proton interactions and pair cascades. The thesis presents the results from theMAGIC and multi-wavelength monitoring campaign of the blazar 1ES 1959+650 during 2016. In 2016 the source underwent into an extremely active phase and exhibited three remarkably bright VHE gamma-ray flares on 13th June, 14th June and 1st July of 2016. On two of these nights, signs of rapid flux variability within sub-hour timescales was clearly resolved by the MAGIC observations. In order to investigate the broadband spectra of the source during the remarkable flaring activities, three different theoretical models were adopted: leptonic, hadronic and mixed lepto-hadronic. Both the hadronic and mixed leptohadronic models yielded neutrino fluxes during the intense activity period, that falls below the sensitivity of the current generation of neutrino telescopes. In 2017, the observation of a high-energy neutrino by IceCube in spatial and temporal coincidence with a flaring blazar named TXS 0506+056 yielded for the first time, hints towards identification of an extragalactic cosmic-ray source. The modelling of the electromagnetic data and the predicted neutrino flux implies that the source could indeed be a potential neutrino emitter and hence an accelerator of high-energy cosmic rays.

The Standard Model of Elementary Particle Physics (SM) is the present theoryfor the elementary particles and their interactions and is a well-established theorywithin the physics community. The SM is a combination of Quantum Chromodynamics(QCD) and the Glashow{Weinberg{Salam (GWS) electroweak model. QCDis a theory for the strong force, whereas the GWS electroweak model is a theoryfor the weak and electromagnetic forces. This means that the SM describes allfundamental forces in Nature, except for the gravitational force. However, the SMis not a nal theory and some of its problems will be discussed in this thesis.In the rst part of this thesis, several properties of baryons are studied suchas spin structure, spin polarizations, magnetic moments, weak form factors, andnucleon quark sea isospin asymmetries, using the chiral quark model (QM). TheQM is an eective chiral eld theory developed to describe low energy phenomena of baryons, since perturbative QCD is not applicable at low energies. The resultsof the QM are in good agreement with experimental data.The second part of the thesis is devoted to the concept of quantum mechanicalneutrino oscillations. Neutrino oscillations can, however, not occur within the GWSelectroweak model. Thus, this model has to be extended in some way. All studiesincluding neutrino oscillation are done within three avor neutrino oscillationmodels. Both vacuum and matter neutrino oscillations are considered. Especially,global ts to all data of candidates for neutrino oscillations are presented and alsoan analytical formalism for matter enhanced three avor neutrino oscillations usingtime evolution operators is derived. Furthermore, investigations of matter eectswhen neutrinos traverse the Earth are included.The thesis begins with an introductory review of the QM and neutrino oscillationsand ends with the research results, which are given in the nine accompanyingscientic articles. / QC 20100616

Mon travail s'inscrit dans un contexte de préparation aux futures expériences haute-sensibilité et haute-résolution sensibles à la polarisation du fond diffus cosmologique et à l'effet de lentilles gravitationnelles. Le premier chapître se veut une introduction à la polarisation du rayonnement de fond et aux expériences à venir dédiées à sa mesure. Ensuite, je présente l'expérience Planck et décris la chaîne de simulations rapides de signaux temporels que j'ai développé pour faciliter l'élaboration et le test des algorythmes d'analyse des données Planck. Les deux derniers chapitres sont consacrés à l'effet de lentille gravitationnelle sur le rayonnement de fond. Tout d'abord, j'évalue la capacité des futures expériences précédemment décrites à mesurer le spectre de puissance des Grandes Structures à partir d'une estimation de l'effet de lentille. J'en déduis leur sensibilité à une masse non-nulle des neutrinos -- suggérée par les expériences d'oscillation -- supprimant les petites échelles angulaires au sein du spectre angulaire de la matière. Enfin, je développe une méthode pour caractériser les effets délétères des avant-plans sur l'estimation de l'effet de lentille. Je valide cette méthode, mettant en oeuvre le meilleur estimateur linéaire de lentilles décrit dans la littérature, grâce à une simulation numérique de cartes du rayonnement de fond diffus affecté par les lentilles et de l'émission des sources radio extra-galactiques. Je trouve que la présence de sources amoindris la sensibilité des expériences au potentiel gravitationnel de la Matière Noire et entraîne la surestimation de son spectre de puissance angulaire.

L'objectif de ce travail est la détection conjointe d'ondes gravitationnelles et de neutrinos cosmique de haute énergie à travers une approche multi-messagers. Les astronomies "neutrinos" et "ondes gravitationnelles" sont encore en phase de développement, mais elles sont appelées à jouer un rôle fondamental dans le futur. En effet, ces "messagers" peuvent parcourir de grandes distances grâce à leur faible interaction avec la matière (contrairement aux photons qui, à haute énergie, sont rapidement absorbés), sans être affectés par les champs magnétiques (contrairement aux rayons cosmiques chargés). Ils peuvent également s' échapper de milieux denses et fournir des informations sur les processus qui ont lieu au coeur des sources astrophysique (les photons s' échappent des couches périphériques des objets célestes). En un mot, ces astronomies sont susceptibles d'ouvrir une nouvelle fenêtre d'observation sur le cosmos. La collaboration ANTARES a construit en Méditerranée un télescope sous-marin de neutrino de haute énergie d'une surface de détection proche de 0.1 km². C'est le télescope le plus sensible pour la partie du ciel observée. Les interféromètres VIRGO et LIGO sont des détecteurs terrestres pour l'observation directe d'ondes gravitationnelles, instalés en Europe et aux états-Unis d'Amérique respectivement. Les instruments ANTARES, VIRGO et LIGO offrent une sensibilité inégalée dans la zone de recherche commune. Le premier chapitre de cette thèse introduit les motivations théoriques pour une recherche jointe d'ondes gravitationnelles et de neutrinos de haute énergies en développant les différents scénarios d'émission. Le deuxième et troisième chapitres sont consacrés à l'étude des techniques de détection avec les interféromètres VIRGO-LIGO et le télescope à neutrinos ANTARES. Les quatriéme et cinquième chapitres de ce travail présentent les résultats d'analyses de données combinées d'ANTARES, VIRGO et LIGO prises séparement pendant les années 2007 et 2009-2010.

The discovery of the Higgs boson by the LHC provided the last piece of the puzzle neces- sary for the Standard Model (SM) to be a successful theory of electroweak scale physics. However there exist various phenomenological reasons which serve as pointer towards the existence of physics beyond the Standard Model. For example the explanation for the smallness of the neutrino mass, baryon asymmetry of the universe, the presence of dark matter and dark energy etc. are not within purview of the Standard Model. Con- ceptual issues like the gauge hierarchy problem, weakness of gravity provide some of the theoretical motivation to pursue theories beyond the SM. We consider scenarios with warped extra-dimensions (Randall-Sundrum (RS) Model ) as our preferred candidate to answer some of the questions raised above. RS model gives an elegant geometric solution to address the hierarchy between the two fundamental scales of nature i.e. Planck scale and electroweak scale. In addition to this, the geometry of RS serves as a useful setup wherein the fermion mass hierarchy problem can also be solved. The goal of this thesis is to investigate whether RS model can be an acceptable theory of avour while at the same time serving as a solution to the hierarchy problem. In Chapter[1] we begin with a brief introduction of the SM, highlighting issues which pro- vides the necessary motivation for constructing new physics models. Various candidates of Beyond Standard Model (BSM) physics are introduced and a few preliminaries es- sential to understand frameworks with additional spatial-dimensions ( at and warped) is provided. In Chapter[2] we specialize to the case of warped extra-dimensions and motivate the need to have the SM elds in the bulk. Mathematical details related to the analysis of various spin elds (0; 12; 1 and 2) in a warped background necessary to understand relevant phenomenology is provided. The lack of knowledge of Dirac or Majorana nature of the neutrino leads to a wide variety of possibilities as far as neutrino mass generation is concerned. In Chapter[3] we focus on the leptonic sector where three cases of neutrino mass generation are consid- ered: a)Planck Scale lepton number violation (LLHH case) b) Dirac neutrinos c) Bulk Majorana mass terms. We then study the implications of each case on the charged lepton mass tting. The case with Planck scale lepton number violation in normal RS scenario requires large and negative values for the bulk mass parameters for the charged singlets cE. Dirac neutrinos and the case with Bulk Majorana mass terms give good t to data. For completeness, the ts for the hadronic sector is provided in the appendix. In Chapter[4] avour violation for each of three cases introduced in Chapter[3] is studied. For the case with Planck scale lepton number violation, the non-perturbative Yukawa coupling between the SM singlets and the KK states render the higher order diagrams incalculable. Lepton avour violation (LFV) is particularly large for the Dirac case and the bulk Majorana case for low Kaluza-Klein(KK) mass scales. We then invoke the ansatz of Minimal Flavour violation to suppress LFV with low lying KK scales and examples of avour group is provided for both cases. In Chapter[5] we present an example with a type II two Higgs doublet model applied to the LLHH case. The setup o ers a solution where LLHH scenario can be consistently realized in RS model, where the masses and mixing angles in the leptonic sector can bet with O(1) choice of bulk parameters. Assumption of global lepton number conservation (like in Dirac neutrinos) could lead to problems in theories of quantum gravity where it does not hold. This leads us to the question whether Dirac neutrinos can be naturally realized in nature. In Chapter[6] we consider the special case of bulk Majorana mass encountered in Chapter[3] where the bulk Dirac mass terms for the right handed neutrino is set to zero. We nd that this leads to a case where the e ective zero mode neutrino mass is of Dirac type with negligible e ects from the tower of Majorana states. In Chapter[7] we consider RS at the GUT scale which no longer serves as a solution to the hierarchy problem. SUSY is introduced in the bulk and the low energy SUSY serves as a solution to the hierarchy problem. Such models serve as a useful alternative to SUSY models with family symmetries (e.g. Froggatt-Nielsen Model). However the solutions to the Yukawa hierarchy problem are constrained due to anomaly cancellation conditions. In Chapter[8] supersymmetry breaking due to radion mediation in addition to brane localized sources is considered and detailed analysis of the running of soft masses and the low energy avour observables is considered for both cases separately. In Chapter[9] we conclude and present future directions.

Ces dernières années, une série d' expériences utilisant des sources naturelles et artificielles de neutrinos ont prouvé que ces particules oscillent; la mesure des paramètres de leur matrice de mélange est en cours et elle guide la conception de futures appareillages et expériences. Théoriquement, cette découverte prouve que les neutrinos sont massives et qu' au moins une extension minimale du Modèle Standard de la physique des particules est nécessaire. Nous décrivons quelques conséquences que cette nouvelle connaissance a sur des systèmes cosmologiques et astrophysiques. En particulier, nous discutons: i) les implications pour les propriétés du fond de neutrinos cosmiques, à la fois dans le scénario minimal et dans certaines extensions non standard; ii) les contraintes cosmologiques actuelles et futures sur la durée de vie des neutrinos; iii) les implications fascinantes de la non-linéairité due à l' auto-réfraction dans l' évolution de la saveur des flux de neutrinos émis par la proto-étoile à neutrons produite lors d' un phénomène de supernova à effondrement de coeur. Enfin, nous décrivons certaines des orientations de recherche possibles pour les années à venir.