Multiple coherent supernova explosions (SNe) in an OB association can produce a strong shock that moves through the interstellar medium (ISM). These shocks fronts carve out hot and tenuous regions in the ISM known as superbubbles. The density contour plot at three different times (0.5 Myr (left panel), 4 Myr (middle panel), 9.5 Myr (right panel)) showing different stages of superbubble evolution for n0 = 0.5 cm−3, z0 = 300 pc, and for NOB = 104. This density contour plot is produced using ZEUS-MP 2D hydrodynamic simulation with a resolution of 512 × 512 with a logarithmic grid extending from 2 pc to 2.5 kpc. For a detailed description of this figure, see Roy et. al., 2015. The evolution of a superbubble is marked by different phases, as it moves through the ISM. Consider an OB association at the center of a disk galaxy. Initially the distance of the shock front is much smaller than the disk scale height. The superbubble shell sweeps up the ISM material, and once the amount of swept up material becomes comparable to the ejected material during SNe, the superbubble enters a self-similar phase (analogous to the Sedov-Taylor phase of individual SNe). As the superbubble shell sweeps up material, its velocity decreases, and thus the corresponding post-shock temperature drops. At a temperature of ∼ 2 × 105 K (where the cooling function peaks), the superbubble shell becomes radiative and starts losing energy via radiative cooling. This radiative phase is shown in the left panel of Figure 1. The superbubble shell starts fragmenting into clumps and channels due to Rayleigh-Taylor instabilities (RTI) (which is seeded by the thermal instability; for details see Roy et. al., 2013) when the superbubble shell crosses a few times the scale height. This is represented in the middle panel of the same figure. At a much later epoch, RTI has a strong effect on the shell fragmentation and the top of the bubble is completely blown off (the right panel). In the first chapter of the thesis (reported in Sharma et. al., 2014), we show using ZEUS-MP hydrodynamic simulations that an isolated supernova loses almost all its mechanical energy within a Myr whereas superbubbles can retain up to ∼ 40% of the input energy over the lifetime of the starcluster (∼ few tens of Myr), consistent with the analytic estimate of the second chapter. We also compare different recipes (constant luminosity driven model (LD model), kinetic energy driven model (KE model) to implement SNe feedback in numerical simulations. We determine the constraints on the injection radius (within which the SNe input energy is injected) so that the supernova explosion energy realistically couples to the interstellar medium (ISM). We show that all models produce similar results if the SNe energy is injected within a very small volume ( typically 1–2 pc for typical disk parameters). The second chapter concentrates on the conditions for galactic disks to produce superbubbles which can give rise to galactic winds after breaking out of the disk. The Kompaneets formalism provides an analytic expression for the adiabatic evolution of a superbubble. In our calculation, we include radiative cooling, and implement the supernova explosion energy in terms of constant luminosity through out the life-time of the OB stars in an exponentially stratified medium (Roy et. al., 2013). We use hydrodynamic simulations (ZEUS-MP) to determine the evolution of the superbubble shell. The main result of our calculation is a clear demarcation between the energy scales of sources causing two different astrophysical phenomenon: (i) An energy injection rate of ∼ 10−4 erg cm−2 s−1 (corresponding Mach number ∼ 2–3, produced by large OB associations) is relevant for disk galaxies with synchrotron emitting gas in the extra-planar regions. (ii) A larger energy injection scale ∼ 10−3 erg cm−2 s−1, or equivalently a surface density of star formation rate ∼ 0.1 M⊙ yr−1 kpc−2 corresponding to superbubbles with high Mach number (∼ 5–10) produces galactic-scale superwinds (requires superstar clusters to evolve coherently in space and time). The stronger energy injection case also satisfies the requirements to create and maintain a multiphase halo (matches with observations). Roy et. al., 2013 also points out that Rayleigh-Taylor instability (RTI) plays an important role in the fragmentation of superbubble shell when the shell reaches a distance approximately 2–3 times the scale-height; and before the initiation of RTI, thermal instability helps to corrugate the shell and seed the RTI. Another important finding of this chapter is the analytic estimation of the energetics of superbubble shell. The shell retains almost ∼ 30% of the thermal energy after the radiative losses at the end of the lifetime of OB associations. The third chapter considers the escape of hydrogen ionizing (Lyc) photons arising from the central OB-association that depends on the superbubble shell dynamics. The escape fraction of Lyc photons is expected to decrease at an initial stage (when the superbubble is buried in the disk) as the dense shell absorbs most of the ionizing photons, whereas the subsequently formed channels (created by RTI and thermal instabilities) in the shell creates optically thin pathways at a later time (∼ 2–3 dynamical times) which help the ionizing photons to escape. We determine an escape fraction (fesc) of Lyc photons of ∼ 10 ± 5% from typical disk galaxies (within 0 ≤ z (redshift) ≤ 2) with a weak variation with disk masses (reported in Roy et. al., 2015). This is consistent with observations of local galaxies as well as constraints from the epoch of reionization. Our work connects the fesc with the fundamental disk parameters (mid-plane density (n0), scale-height (z0)) via a relation that fescαn20z03 (with a ≈ 2.2) is a constant. In the fourth chapter, we have considered a simple model of molecule formation in the superbubble shells produced in starburst nuclei. We determine the threshold conditions on the disk parameters (gas density and scale height) for the formation of molecules in superbubble shells breaking out of disk galaxies. This threshold condition implies a gas surface density of ≥ 2000 M⊙ pc−2, which translates to a SFR of ≥ 5 M⊙ yr−1 within the nuclear region of radius ∼ 100 pc, consistent with the observed SFR of galaxies hosting molecular outflows. Consideration of molecule formation in these expanding superbubble shells predicts molecular outflows with velocities ∼ 30–40 km s−1 at distances ∼ 100–200 pc with a molecular mass ∼ 106–107 M⊙, which tally with the recent ALMA observations of NGC 253. We also consider different combinations of disk parameters and predict velocities of molecule bearing shells in the range of ∼ 30–100 km s−1 with length scales of ≥ 100 pc, in rough agreement with the observations of molecules in NGC 3628 and M82 (Roy et. al., 2016, submitted to MNRAS).

New high-K isomers have been populated in Ta and W by bombarding thick targets with pulsed 238U beams at 1600 MeV. The new inelastically excited multi-quasiparticle states include Kpi = 21/2- and 29/2- 3-quasiparticle isomers in 181Ta and Kpi = 7- and (16+) isomers in 186W. The Kpi = (16+) state in 186w has t1/2≥3 ms and extends the 4-quasiparticle isomer systematics beyond the limit accessible with fusion-evaporation reactions, using stable beams and targets, for the first time. In addition, a t1/2≥1 ms 3-quasiparticle isomeric state feeding a strongly coupled rotational band has been populated in Ta by nucleon transfer. The excitation energies of the intrinsic states are compared to predictions of blocked BCS calculations. A different study of high-K states used a radioactive 14C beam at 67 MeV to investigate the high-spin structure of Os. New rotational bands built on multi-quasiparticle states with Kpi = 5-, 7-, 9-, 10+ and 15+ are observed. The first crossing of the ground-state band at I = 14 h, is interpreted as involving a high-K t-band structure and explained using a two-band mixing model. The structure at higher angular momentum is dominated by intrinsic states, that exhibit a dramatic loss of isomerism. Potential-energy-surface calculations, with Lipkin-Nogami pairing, show these configurations to be triaxial, accounting for the breakdown in K conservation. The relation between the K projection and the total angular momentum is investigated for these non-axial states.

Lorsque l’on veut sonder les structures internes de sources astronomiques non résolues par nos instruments modernes, la technique de la spectropolarimétrie a démontré etre une méthode à la fois indépendante et complémentaire des analyses spectrales et temporelles. Dans cette thèse, j’explore de façon théorique le signal de polarisation résultant des Noyaux Actifs de Galaxies (NAG en français, AGN en anglais), dans lesquels on suppose que l’énergie radiative principale est crée paraccrétion autour d’un trou noir super-massif et qu’une partie importante des échappements de matère se fait sous la forme de vents d’éjection. Selon le Schéma Unifié des NAG, l’émission radiative résultante est fortement anisotrope, due au confinement des photons par un corps de poussère obscurcissant situé au niveau du plan équatorial. Les radiations sont donc forcées de s’échapper dans les directions polaires, photo-ionisant au passage les vents d’éjection coniques. Cette configuration asymétrique permet de justifier la dichotomie observationnelle des NAG en fonction de leur inclinaison spatiale; cependant, leurs propriétés difèrent aussi en fonction de la bande énergétique d’observation. Donc, afin de vérifier la stabilité du moèle unifié, il est nécessaire de le tester sur de multiples échelles de longueur d’onde afin d’en déduire de fortes contraintes morphologiques. / When probing the inner structures of unresolved astrophysical sources, spectropolarimetry has proven to be a solid tool, both independent and complementary to spectral and timing analyses. In this thesis, I theoretically explore the polarization of Active Galactic Nuclei (AGN), which are powered by accretion onto supermassive black holes and often reveal significant mass outflows. Their emission is strongly anisotropic and the standard model of AGN postulates that the anisotropy is caused by a confinement of the radiation in the funnel of an obscuring body of circumnuclear dust; the radiation is thus forced to escape along the funnel where it photo-ionizes conically shaped outflows. The asymmetrical configuration explains an observational dichotomy where AGN properties are characterized according to the observer’s line-of-sight. However, AGN observations differ significantly from one waveband to another and the broadband validity of the unified model has to be tested by a method that gives strong constraints on the AGN morphology. In this thesis, I subsequently investigate how morphological and composition constraints on the different substructures in thermal, radio-quiet Active Galactic Nuclei can be deduced from optical, UV and X-ray polarization properties.

Le tableau périodique est connu jusqu'à l'élément Z=118, situé dans une région difficile d'accès. Un ultime Îlot de stabilité y est prédit par les théories mais n'a pas encore été mis en évidence. Les noyaux de Z=100 à 106 sont produits en nombre suffisant pour en faire la spectroscopie fine. J'ai ainsi étudié le noyau de 256Rf (Z=104). Pour cela, un faisceau isotopique intense d'ions de 50Ti a été conçu et réalisé avec la méthode MIVOC pour la première fois à Jyväskylä (Finlande).Grâce à l'association de JUROGAM II, RITU et GREAT, j'ai étudié le 256Rf en spectroscopies prompte et retardée. J'ai mis en évidence la première bande de rotation dans un noyau superlourd s'étendant jusqu'à un spin de 20+ et confirmé les trois états isomériques connus. Après la présentation des méthodes de sélection, la caractérisation de ces transitions et les moments d'inertie associés sont discutés et comparés avec ceux de la région. Les informations sur la structure quantique sont aussi sont discutées. / The periodic table is known up to the element Z=118, in a region very difficult to access. An ultimate superheavy Island of Stability is predicted by various theories but was never discovered. The nuclei from Z=100 to 106 can be produced in suffisant number to be studied by spectroscopic techniques. Within this framework, I studied in particular the 256Rf (Z=104) nuclei. For this purpose, an isotopic intense 50Ti ion beam was established with the MIVOC method for the first time at Jyväskylä (Finland).Thanks to the JUROGAM II, RITU and GREAT association, I studied the 256Rf with in prompt and delayed spectroscopy. I highlighted the first rotational band in a superheavy nuclei extending up to 20+ and confirmed its three khown isomers. After the presentation of the selections methods, the characterization of these transitions and the associated moments of inertia are discussed and compared to those of the region. The informations on the quantum structure are also discussed.

Title: Microscopic nuclear models for open-shell nuclei Author: Jakub Herko Institute: Institute of Particle and Nuclear Physics Supervisor: Mgr. František Knapp, Ph.D., Institute of Particle and Nuclear Physics Abstract: Since the nucleus is a quantum many-body system consisting of con- stituents whose mutual interaction is not satisfactorily known, it is necessary to use approximate methods when describing the nucleus. Basic approximate approaches in the microscopic theory of the nucleus are the Hartree-Fock the- ory, Tamm-Dancoff approximation and random phase approximation. They are described in the first chapter of this thesis. The main aim was to develop mi- croscopic models for open-shell nuclei with two valence particles or holes. They are described in the second chapter, which contains detailed derivations of the relevant formulae. These methods have been numerically implemented. The re- sults of the calculations of the nuclear spectra and the electromagnetic transition probabilities are presented in the third chapter. Keywords: Tamm-Dancoff approximation, random phase approximation, open- shell nuclei, nuclear spectra, electromagnetic transition probabilities ii

This dissertation attempts to extend the classes of halogen-containing systems which may be studied using solid-state nuclear magnetic resonance (SSNMR). As line shape broadening due to the quadrupolar interaction (QI) scales inversely with the applied field, high-field magnet technology is indispensable for this research. Combining advanced radiofrequency pulse sequences with high-field wideline data acquisition allowed for the collection of very broad SSNMR signals of all quadrupolar halogen nuclei (i.e., 35/37Cl, 79/81Br and 127I) within a reasonable amount of experimental time. The initial systems for study were of the MX2 variety (M = Mg, Ca, Sr, Ba; X = Cl, Br, I). In total, 9 anhydrous compounds were tested. The effects of hydrate formation were tested on 7 additional compounds. Systematic trends in the observed δiso values (and to a lesser extent, Ω and CQ) were found to be diagnostic of the extent of hydration in these materials. Resolving power was successfully tested using SrBr2, which possesses 4 magnetically unique sites. The composition of CaBr2•xH2O was convincingly determined using SSNMR data and the hydration trends noted above. The sensitivity of the QI to the local bonding environment (e.g., bond distance changes of less than 0.05 Å) was used to refine (when coupled with gauge-including projector augmented-wave density functional theory (GIPAW DFT) quantum chemical computations) the structure of MgBr2, and was used to correct prior NMR data for CaCl2 (earlier accounts had been performed upon a CaCl2 hydrate). During NMR data analysis of certain iodine-containing materials, it was found that standard fitting software (which uses perturbation theory) could not reproduce the observations. Proper analysis required the use of exact simulation software and allowed for the observation of high-order quadrupole-induced effects (HOQIE). This motivated further studies using rhenium-185/187 nuclei, where it was expected that HOQIE would be more dramatic. The observed rhenium SSNMR spectra possessed additional fine structure that had never been observed before experimentally, nor would be expected from currently-available perturbation theory analysis software. Lastly, preliminary results are shown where 127I SSNMR is used to study important supramolecular systems, and the composition of the popular synthetic reagent ‘GaI’ is elucidated.

Neste trabalho estudamos a dinâmica de discos torcidos finos e espessos para compreender melhor a propagação da deformação nestes discos. No caso dos discos finos, estudamos a física do efeito Bardeen-Petterson e aplicamos este modelo para explicar o jato em escalas de parsec e kilo-parsec da galáxia NGC 1275. Encotramos que o efeito Bardeen-Petterson reproduziu muito bem a forma do jato e com isto derivamos os parâmetros do disco como raio, valores das viscosidades azimutal e vertical, lei de potência da densidade superficial e spin do buraco negro. Para uma melhor compreensão da física destes discos, realizamos simulações GRMHD de discos moderadamente finos tanto planos como inclinados para estudar a evolução do ângulo de inclinação entre os momentos angular do buraco negro e do disco de acresção assim como o ângulo de torção que está associado com a precessão do disco. Encontramos que quando o disco de acresção e o buraco negro rotacionam no mesmo sentido, o ângulo de inclinação entre os momentos angular apresentou um comportamento oscilatório na parte interna do disco e permaneceu constante na parte externa em acordo com as previsões teóricas. Já quando o buraco negro rotacina no sentido oposto ao disco de acresção, encontramos pela primeira vez numa simulação GRMHD evidências de alinhamento, ocorrendo um alinhamento de 10\\% do angulo entre os momentos angulares do disco e buraco negro. Além disso, comprovamos pela primeira vez numa simulação GRMHD a não isotropia do stress. Utilizando um modelo semi-analítico, comparamos os resultados de nossas simulações com este modelo, utilizando os dados da simulações de disco plano como entrada e obitivemos os mesmos comportamentos das simulações tanto no caso prógrado quanto no caso retrógrado mostrando que o alinhamento é devido ao regime onda. / In this work we studied the dynamics of twisted thin and thick disks to better understand how the warp propagates in these discs. In the case of thin discs, we studied the physics of the Bardeen-Petterson effect and we applied this model to explain the shape of the jet in both parsec and kilo-parsec scales of the galaxy NGC 1275. We found that the Bardeen-Petterson effect could explain very well the shape of the jet and with that we derived the disc parameters such as its radius, the values of the kinematic azimutal and vertical viscosities, the power-law of the surface density and the spin of the black hole. To better understand the physics of such discs, we have performed GRMHD simulations of moderatelly thin tilted disks to study the evolution of the tilt angle between the angular momentum of the accretion disk and black hole and also the twist angle which is associated with the precession of the disc. We found that when the accretion disc and the black hole are rotating in the same direction, the tilt angle showed an oscillatory behavior in the inner parts of the disk while in the outer parts it remained constant in agreement with the theorical modelos. However, when both rotate in the opposite direction, we found for the very first time in a GRMHD simulation, evidences of alignment of 10\\% of the tilt angle. Besides that, we prove for the first time in a GRMHD simulation that the stress is far from being isotropic. Using a semi-analitic model, we compared the results of our simulations with this model, using the datas of the untilted simulations as inputs and we found the same behaviors found in the simulations even in prograde case as in the retrograde case showing that the alignment is due to bending waves.

La propagation des rayons Ɣ de très haute énergie (E > 100GeV) dans l'univers est affectée par les propriétés du milieu extragalactique. Ces photons à l'échelle du TeV, issus des processus d'accélération de particules dans les noyaux actifs de galaxies, peuvent en effet interagir avec des photons du fond optique et infrarouge qui baignent l'univers et produire des paires d'électrons et de positrons. Ce processus réduit la transparence de l'univers aux rayons Ɣ de très haute énergie mais permet en revanche de sonder les propriétés du milieu extragalactique de façon unique. Dans cette thèse, les données prises par le réseau de télescopes à imagerie Tcherenkov atmosphérique H.E.S.S. sont analysées et utilisées afin de caractériser la transparence de l'univers aux rayons Ɣ de très haute énergie. Une mesure indépendante de la distribution spectrale en énergie du fond cosmologique optique et infrarouge est réalisée à travers l'ajustement des modulations observées dans les spectres en énergie obtenus avec H.E.S.S. pour un échantillon de noyaux actifs de galaxies brillants dans une gamme en redshift 0.03 < z < 0.28. Les résultats obtenus sont compatibles avec les limites inférieures dérivées par comptages de galaxies et ne suggèrent pas d'anomalie de la transparence de l'univers aux rayons Ɣ vis à vis des modèles actuels du fond de lumière extragalactique. Des processus de second ordre affectant la propagation des rayons Ɣ de très haute énergie sont également explorés. Des limites sur une brisure de la symétrie de Lorentz à l'échelle de Planck sont obtenues à partir de l'analyse spectrale du noyau actif Mrk 501 observé dans un état de flux exceptionnel par H.E.S.S. en 2014, à grand angle zénithal. Enfin, des contraintes sur le champ magnétique extragalactique sont dérivées en considérant l'émission Ɣ secondaire attendue à partir de simulations des cascades électromagnétiques initiées lors du processus d'absorption pour le noyau actif distant PG 1553+113 vu par H.E.S.S. et le télescope spatial Fermi. Cette thèse a également été l'occasion d'une participation aux développements de certains aspects de la calibration et de l'analyse des données de H.E.S.S. / The propagation of very high energy Ɣ rays in the universe depends on the properties of the extragalactic medium. Such TeV-scale photons travelling cosmological distances are -emitted through particle acceleration mechanisms in active galaxy nuclei- can interact with the low-energy photons of the extragalactic background light (EBL) and produce electron-positron pairs. This effect reduces the transparency of the universe to very high energy Ɣ rays but it also provides a unique opportunity to probe the properties of the extragalactic medium. In this thesis, data taken with the H.E.S.S. array of Cherenkov telescopes are analyzed and used to characterize the transparency of the universe to very high energy Ɣ rays. A independent measurement of the spectral energy distribution of the EBL with H.E.S.S. is presented. It is obtained by extracting the EBL absorption signal from the fit of spectral modulations in the high-quality spectra of a sample of bright blazars in the redshift range 0.03 < z < 0.28. The intensity of the EBL obtained in different spectral bands is presented together with the associated Ɣ-ray horizon. The obtained results are consistent with lower limits derived from galaxy counts and do not suggest an anomaly of the transparency of the universe to Ɣ rays with respect to current models of the extragalactic background light. Second-order processes affecting the propagation of very high energy Ɣ rays in the universe are also considered. Limits on Lorentz invariance violation at Planck scale are obtained from the spectral analysis of the active galaxy nucleus Mrk 501 observed during a high-flux state by H.E.S.S. in 2014, at large zenith angle. Finally, constraints on the extragalactic magnetic field properties are derived by considering the secondary Ɣ-ray emission expected from the simulation of electromagnetic cascades initiated by the absorption process for the distant active galaxy nucleus PG 1553+113 seen by H.E.S.S. and the Fermi Ɣ-ray space telescope. In this thesis some developments related to the calibration and analysis of H.E.S.S. data are also presented.

Les travaux effectués au cours de cette thèse au sein du groupe de structure nucléaire de l’IPN d’Orsay s’articulent autour de la production, en vue d’une étude par spectroscopie gamma, de noyaux exotiques riches en neutron de la couche fp. Dans ce cadre, nous avons mis en place, auprès de l’accélérateur Tandem d’Orsay, un multi-détecteur au germanium baptisé ORGAM, destiné à la spectroscopie gamma à haute résolution. Au cours de l’année 2008-2009, les détecteurs amenés à composer ORGAM ont été testés individuellement, ainsi que le dispositif annexe de réjection Compton, en coopération avec la division instrumentation du laboratoire. Parallèlement, le système d’alimentation automatique en azote liquide, destiné au maintien des détecteurs à basse température, a été amélioré et fiabilisé. L’ensemble du dispositif a été mis en place sur une ligne de faisceau de l’accélérateur tandem avec le concours du personnel technique de l’accélérateur.La première expérience utilisant le dispositif ORGAM a été réalisée en juillet 2009. Cette expérience, dont les données ont été analysées dans le cadre de ce travail, visait à étudier les collisions profondément inélastiques entre un faisceau de 36S accéléré à 154 MeV, et une cible de 70Zn. Un dispositif permettant la détection des particules chargées émises à grand angle a été utilisé afin d’identifier les fragments de ces collisions. Il n’a pas été possible, du fait du fond important induit par la diffusion élastique du faisceau dans la cible, d’identifier directement ces fragments. L’étude des coïncidences gamma-gamma avec le détecteur ORGAM a cependant permis de mettre en évidence de nombreuses cascades de photons désexcitant des noyaux potentiellement produits par les réactions d’intérêt.Les données recueillies au cours d’une autre expérience, réalisée auprès du tandem d’Orsay en 2005, ont été analysées dans le cadre de ce travail. Cette expérience, visant à produire par fusion évaporation entre un faisceau de 14C à 25 MeV et une cible de 48Ca, les noyaux de 59Mn et de 57Cr, a permis d’établir une partie du spectre en énergie d’excitation de ces noyaux, jusqu'à une énergie d’excitation supérieure à 3 MeV.Une étude théorique des noyaux de chrome impairs de la couche fp a été tentée à l’aide d’un modèle phénoménologique de couplage intermédiaire. Ce modèle a permis une description satisfaisante du 53Cr. Les prédictions du modèle, qui ne prend pas en compte l’interaction entre nucléons de valence, se sont avérées beaucoup moins satisfaisante pour les noyaux de 55Cr et 57Cr. / This PhD thesis was prepared within the nuclear structure group of IPN Orsay. The work presented aimed to produce neutron rich fp shell nuclei through heavy ion collisions at the tandem accelerator of IPN, and to study them using gamma spectroscopy. For this purpose, a germanium gamma array called ORGAM, and dedicated to high resolution gamma spectroscopy, was set up at the tandem accelerator. During the year 2008/2009, the individual germanium detectors were tested and repaired, as well as their ancillary anti-Compton shielding. At the same time, the liquid nitrogen auto-fill system was improved for better reliability. The array was finally set up on a beam line of the accelerator.The first experiment using the ORGAM array was performed in July 2009. This experiment aimed to study fully damped deep-inelastic collisions between a 36S beam accelerated to 154 MeV, and a 70Zn target. An additional charged particle detection system was used to detect interesting fragments emitted at backward angles. It was not possible to separate these fragments from the background induced by backscattered ions from the beam. Nevertheless, the study of gamma-gamma coincidences detected with the ORGAM array allowed to identify gamma cascades de-exciting nuclei potentially produced through the mechanism of interest. Data accumulated during another experiment performed at the tandem accelerator in 2005 were analyzed. Fusion-evaporation reaction between a 25 MeV, 14C beam focused on a 48Ca target produced the 57Cr and 59Mn nuclei, whose energy spectra were established up to 3 MeV.We attempted to study theoretically odd Chromium isotopes with a simple model based on the intermediate coupling scheme. This model, which doesn’t take into account correlation between valence nucleons, described in satisfactory way the semi-magic + 1 neutron, 53Cr, but failed to do so for mid-shell nuclei 55Cr and 57Cr.

Les facteurs spectroscopiques nous renseignent sur l'occupation des couches nucléaires et peuvent être extraits par des réactions directes comme le transfert à basse énergie et le knockout aux énergies intermédiaires. L’étude récente de noyaux radioactifs de la couche sd ayant une large différence d'énergie de séparation, DeltaS=Sp-Sn~20 MeV, montre que les sections efficaces d’arrachage d’un nucléon très lié sont considérablement réduites par rapport aux prédictions théoriques. Cette tendance n’est pas observée pour des noyaux moins exotiques, jusqu’à DeltaS~12 MeV, par réaction de transfert (d,p).Pour comprendre l'origine de cette réduction, nous avons réalisé deux expériences complémentaires sur un noyau présentant une large différence d’énergie de séparation l’14O : (i) le knockout d'un nucléon au NSCL, 14O (53 MeV/n) et 16C (75 MeV/n), sur une cible de 9Be; (ii) le transfert d'un nucléon avec le faisceau d’14O à 18 MeV/n de SPIRAL, 14O(d,t)13O et 14O(d,3He)13N, étudié avec le dispositif MUST2. L'analyse des données présentée en détails dans ce manuscrit conduit à des facteurs spectroscopiques incompatibles entre ces deux expériences lorsqu'un neutron fortement lié est enlevé ou transféré de l'14O. Dans le cas du knockout, la section efficace mesurée est fortement réduite par rapport aux prédictions basées sur un modèle eikonal et le modèle en couches. La distribution en moment parallèle de l’13O mesurée après l’arrachage d’un neutron présente par ailleurs une forme qui n’est pas reproduite par le modèle eikonal. Dans le cas du transfert, une telle réduction n'est pas observée et le rapport entre expérience et théorie est compatible avec ce qui est obtenu pour les noyaux stables. Ces résultats suscitent de nouveaux développements théoriques pour la modélisation du mécanisme de réaction dans ces cas extrêmes où le nucléon enlevé est fortement lié. / The distribution of spectroscopic strength in nuclei can be extracted from direct-reaction cross section measurements, as one-nucleon knockout at intermediate energy or transfer at low energy. The study of deeply-bound nucleon removal from several sd-shell nuclei having a large difference of proton-neutron separation energies, DeltaS=Sp-Sn~20 MeV, exhibits experimental cross sections about four times smaller than theoretical predictions from state-of-the-art calculations. This trend is not observed from (d,p) transfer reactions with nuclei having smaller separation energy asymmetry, DeltaS~12 MeV.To investigate the origin of this reduction, we have performed two complementary experiments for the 14O case having a large energy asymmetry: (i) one-nucleon knockout from 14O (53 MeV/n) and 16C (75 MeV/n) on a 9Be target at the NSCL; (ii) one-nucleon transfer reaction using SPIRAL beam, 14O(d,t)13O and 14O(d,3He)13N at 18 MeV/n, and the MUST2 array. The analysis of the data presented in this document leads to a discrepancy between the spectroscopic factors extracted from these two experiment when a deeply-bound neutron is removed from 14O. In the neutron knockout from 14O, the cross section is strongly reduced compared to predictions based on an eikonal model and shell model spectroscopic factors. Moreover, several deviations from the eikonal prediction are observed on the shape of the parallel momentum distribution of the ejectile 13O. For the transfer 14O(d,t)13O, such a reduction is not observed and results are in agreement with stable nuclei values. These results call for new theoretical developments concerning the description of the reaction mechanism when a deeply-bound nucleon is removed from a nucleus.