While the single core accretion model for low mass star formation is well developed, it cannot simply be extended into the high mass star formation regime where clustered star formation dominates. The study of intermediate-mass star formation should provide us with insights into how the process of star formation changes for high mass stars. In this thesis observations of H2O line emission from two intermediate-mass candidate Young Stellar Objects (YSOs) made using the HIFI instrument aboard the Herschel Space Observatory are presented. Modelling of molecular line emission using the radiative transfer code RATRAN is used to put constraints on kinematics and the abundance of water throughout the region by modelling the observed water lines after decomposing them into separate Gaussian components. The medium component of the 752 GHz line from Vela IRS 17 was modelled by using a turbulent velocity of 1.7 km s^-1 and an outer abundance of 6x10^-8. The narrow component of the 752 GHz line from Vela IRS 19 could be modelled using a turbulent velocity of 0.6 km s^-1 and an outer abundance of 6x 10^-8, while the medium component required an outer abundance of 4 x 10^-7 with a turbulent velocity of 2.5 km s^-1. The constraints on water abundance in these star-forming regions are to be used along with studies of water in low and high mass star-forming regions in the effort to improve our understanding of star formation across the entire stellar mass spectrum.

While the single core accretion model for low mass star formation is well developed, it cannot simply be extended into the high mass star formation regime where clustered star formation dominates. The study of intermediate-mass star formation should provide us with insights into how the process of star formation changes for high mass stars. In this thesis observations of H2O line emission from two intermediate-mass candidate Young Stellar Objects (YSOs) made using the HIFI instrument aboard the Herschel Space Observatory are presented. Modelling of molecular line emission using the radiative transfer code RATRAN is used to put constraints on kinematics and the abundance of water throughout the region by modelling the observed water lines after decomposing them into separate Gaussian components. The medium component of the 752 GHz line from Vela IRS 17 was modelled by using a turbulent velocity of 1.7 km s^-1 and an outer abundance of 6x10^-8. The narrow component of the 752 GHz line from Vela IRS 19 could be modelled using a turbulent velocity of 0.6 km s^-1 and an outer abundance of 6x 10^-8, while the medium component required an outer abundance of 4 x 10^-7 with a turbulent velocity of 2.5 km s^-1. The constraints on water abundance in these star-forming regions are to be used along with studies of water in low and high mass star-forming regions in the effort to improve our understanding of star formation across the entire stellar mass spectrum.

Thesis (PhD)--Stellenbosch University, 2013. / ENGLISH ABSTRACT: See full text for the abstract / AFRIKAANSE OPSOMMING: Sien volteks vir die opsomming

The heaviest fragments, recoils, have been studied in proton and deuteron induced 28Si reactions and proton-20Ne reactions at 100-300 MeV per nucleon. Inclusive charge and angular distributions and coincidences between He nuclei and recoils have been compared to two theoretical models, Dubna Cascade Model and JAERI Quantum Molecular Dynamics. The overall agreement was good for the reactions with 28Si, however the angular distributions of He fragments could not be reproduced. For the 20Ne reactions the recoil angular distributions were only reproduced for large angles. There was a significant underestimation at small angles and low recoil charge. α-clustering in the bombarding nucleus is a possible explanation for the deviations. In the 100 MeV per nucleon reactions all assumptions of the models may not be valid and the agreement was worst for these reactions. In proton-natXe reactions intermediate mass fragments have been studied from 200 to 1400 MeV. Slow ramping was used to scan the energy. Charge distributions and a caloric curve have been compared to Cascade Fragmentation Evaporation Model. Charge distributions showed good agreement for fragments with Z<8 but the heavier fragments were underestimated.

The Equation of State (EoS) of asymmetric nuclear matter has been explored through the study of mid-rapidity fragment dynamics from the 35 MeV/u $^{70}$Zn $^{70}$Zn, $^{64}$Zn $^{64}$Zn, and $^{64}$Ni $^{64}$Ni systems. The experimental data was collected at the Texas A and M Cyclotron Institute using the 4 NIMROD-ISiS array, which provided both event characterization and excellent isotopic resolution of charged particles. The transverse collective flow was extracted for proton, deuteron, triton, 3He, alpha, and 6He particles. Isotopic and isobaric effects were observed in the transverse flow of the fragments. In both cases, the transverse flow was shown to decrease with an increasing neutron content in the fragments. The (N/Z)sys dependence of the transverse flow and the difference betwen the triton and 3He flow were shown to be sensitive to the density dependence of the symmetry energy using the stochastic mean-field model. A stiff parameterization of Esym(p) was found to provide better agreement with the experimental data. The transverse flow for intermediate mass fragments (IMFs) was investigated, providing a new probe to study the nuclear EoS. A transition from the IMF flow strongly depending on the mass of the system, in the most violent collisions, to a dependence on the charge of the system, for the peripheral reactions, was observed. Theoretical simulations were used to show that the relative differences in the IMF flow are sensitive to the density dependence of the symmetry energy. The best agreement between the experiment and theory was achieved with a stiff Esym(p). A new method was developed in which correlations between the projectile-like and mid-rapidity fragments were examined using a scaled flow. Theoretical simulations were used to show that the scaled flow of the particles was connected to their average order of emission. The experimental results suggest that the mid-rapidity region is preferentially populated with neutron-rich light charged particles and the Z=3-4 IMFs at a relatively early stage in the collision. This work presents additional constraints on the nuclear EoS and insight into the mid-rapidity dynamics observed in Fermi energy heavy-ion collisions.

Les protoétoiles de masse intermédiaire (IM) (2 ≤ M* ≤ 8 Msun) sont le lien entre les étoiles de faible et haute masse car elles couvrent également un intervalle intermédiaire de luminosités, de densités et de températures [Fuente et al., 2012]. Même si les « IM-YSOs » jouent un rôle important dans l'étude de la formation des étoiles, on a très peu de connaissances sur la formation et l'évolution des premières étapes des protoétoiles de masse intermédiaire. Les études systématiques spectrales sont un outil puissant pour caractériser la composition chimique d'un objet astrophysique, et la seule façon d'obtenir un recensement complet des espèces chimiques. Une étude spectrale fournit également des lignes multiples de la même molécule, donnant la possibilité d'une analyse multifréquences ainsi que d'une modélisation. En outre, grâce aux profils des raies, nous pouvons obtenir des informations sur la cinématique, et identifier les structures au long de la ligne de vue, en tant que sources multiples, des jets ou des cavités, par exemple, [Caux et al., 2011]. Les phénomènes d'éjection (jets, des vents et des « outflows » bipolaires moléculaires), sont une phase inhérente au processus de formation d'étoiles observées dans les YSOs de toutes masses dans des longueurs d'onde millimétriques. Cependant, il n'y a pas d'études systématiques dans l'intervalle de masse intermédiaire comme dans le cas des protoétoiles de faible et haute masse. Compte tenu de l'absence d'une étude systématique de la partie mm/submillimétrique dans le spectre des protoétoiles de masse intermédiaire, au cours de ma thèse, j'ai mené une étude systématique spectrale vers la protoétoile de masse intermédiaire de classe 0 Cep E et de son « outflow » moléculaire. / Intermediate-mass (IM) protostars (2 ≤ M∗ ≤8 Msun) are the link between low and the high mass stars as they cover also an intermediate range of luminosities, densities and temperatures [Fuente et al., 2012]. Even though the IM-YSOs are important in the study of star formation, very little is known about the formation and first evolutionary stages of IM protostars. Unbiased spectral surveys are a powerful tool to characterize the chemical composition of an astrophysical object, and the only way to obtain a complete census of the chemical species. A spectral survey provides also multiple lines from the same molecule, giving the possibility of a multi-frequency analysis and modeling. Also, through line profiles, we can obtain kinematic information, and identify structures along the line of sight, as multiple sources, outflows, jets or cavities, e.g. [Caux et al., 2011]. The outflow phenomena (jets, winds and bipolar molecular outflows), are an inherent phase in the process of star formation observed in YSOs of all range of masses at millimeter wavelengths. However, there are not systematic studies in IM range as in the case of of low- and high-mass protostars. Given the lack of a systematic study of the mm/submm spectrum of IM protostars, during my thesis I carried out an unbiased spectral survey towards IM Class 0 Cep E protostar and its molecular outflow.

No presente trabalho é apresentado um conjunto de medidas de seção de choque do processo de fusão nuclear nos sistemas ANTPOT. 12 C + ANTPOT. 63, 65 CU, em um intervalo de energia correspondente à 0.91.8 vezes a barreira coulombiana. O método experimental utilizado foi a detecção dos resíduos de evaporação através da técnica de tempo de vôo, acoplado à um defletor eletrostático para separar as partículas provenientes do espalhamento elástico dos produtos de fusão. As vantagens e limitações do método são discutidas em detalhes. As funções de excitação de fusão dos sistemas citados foram analisadas via modelo de penetração de barreira unidimensional , utilizando vários potenciais nucleares. Dessa análise comprovou-se que a secção de choque de fusão é subestimada em energias em torno e abaixo da barreira coulombiana. Nesse sentido foi feito um cálculo, utilizando o código computacional CCFUS, que simula o acoplamento de canais, com a finalidade de descobrir quais canais contribuem para o processo de fusão nuclear em baixas energias. As seções de choque de fusão obtidas foram comparadas com outros sistemas - ANTPOT. 12 C + ANTPOT. 63, 65 CU.- que utilizam os mesmos núcleos-alvo. A comparação revelou que os sistemas ANTPOT. 12 C + ANTPOT. 63, 65 CU possuem o maior aumento de seção de choque de fusão subcoulombiana e esse fato pode estar relacionado à deformação estática do projétil. A comparação das distribuições da velocidade dos resíduos de evaporação para os dois de sistemas revelou um canal intenso para o sistema ANTPOT. 12 C + ANTPOT. 63 CU que não está presente para o outro sistema. / In this work we present cross-section measurements for nuclear fusion in the 12C+ 63,65 Cu system, at 12C energy range from 0.9 to 1.8 times the Coulomb barrier. In order to detect and to obtain the mass identification of the evaporation residues following the fusion process, the time of flight method was adopted in conjunction with an eletrostatic deflector capable of separating the evaporation residues from the beam particles. The limitation and advantadges of this method of measurement are discussed. The excitation functions for the above systems were analysed using the unidimensional barrier penetration model with different nuclear potentials. Theoretical fusion cross-section values obtained from this analysis were systematically smaller than our measured values, in the energy region below the Coulomb barrier. In order to discover which channel enhances the fusion cross-section in this region, a coupled channel calculation was performed, with the aid of CCFUS code. The experimental data for the above reactions were compared with the systems 12C+ 63,65 Cu, measured by our group. In this comparison, It was noted that the systems 12C+ 63,65 Cu have greater fusion cross section below the Coulomb barrier. This fact can be related to the static deformation of 12C. The comparison of velocity spectra of the evaporated residues for the two systems shows that 12C+63Cu has a strong reaction channel that was not present in the 12C+ 65Cu system.

No presente trabalho é apresentado um conjunto de medidas de seção de choque do processo de fusão nuclear nos sistemas ANTPOT. 12 C + ANTPOT. 63, 65 CU, em um intervalo de energia correspondente à 0.91.8 vezes a barreira coulombiana. O método experimental utilizado foi a detecção dos resíduos de evaporação através da técnica de tempo de vôo, acoplado à um defletor eletrostático para separar as partículas provenientes do espalhamento elástico dos produtos de fusão. As vantagens e limitações do método são discutidas em detalhes. As funções de excitação de fusão dos sistemas citados foram analisadas via modelo de penetração de barreira unidimensional , utilizando vários potenciais nucleares. Dessa análise comprovou-se que a secção de choque de fusão é subestimada em energias em torno e abaixo da barreira coulombiana. Nesse sentido foi feito um cálculo, utilizando o código computacional CCFUS, que simula o acoplamento de canais, com a finalidade de descobrir quais canais contribuem para o processo de fusão nuclear em baixas energias. As seções de choque de fusão obtidas foram comparadas com outros sistemas - ANTPOT. 12 C + ANTPOT. 63, 65 CU.- que utilizam os mesmos núcleos-alvo. A comparação revelou que os sistemas ANTPOT. 12 C + ANTPOT. 63, 65 CU possuem o maior aumento de seção de choque de fusão subcoulombiana e esse fato pode estar relacionado à deformação estática do projétil. A comparação das distribuições da velocidade dos resíduos de evaporação para os dois de sistemas revelou um canal intenso para o sistema ANTPOT. 12 C + ANTPOT. 63 CU que não está presente para o outro sistema. / In this work we present cross-section measurements for nuclear fusion in the 12C+ 63,65 Cu system, at 12C energy range from 0.9 to 1.8 times the Coulomb barrier. In order to detect and to obtain the mass identification of the evaporation residues following the fusion process, the time of flight method was adopted in conjunction with an eletrostatic deflector capable of separating the evaporation residues from the beam particles. The limitation and advantadges of this method of measurement are discussed. The excitation functions for the above systems were analysed using the unidimensional barrier penetration model with different nuclear potentials. Theoretical fusion cross-section values obtained from this analysis were systematically smaller than our measured values, in the energy region below the Coulomb barrier. In order to discover which channel enhances the fusion cross-section in this region, a coupled channel calculation was performed, with the aid of CCFUS code. The experimental data for the above reactions were compared with the systems 12C+ 63,65 Cu, measured by our group. In this comparison, It was noted that the systems 12C+ 63,65 Cu have greater fusion cross section below the Coulomb barrier. This fact can be related to the static deformation of 12C. The comparison of velocity spectra of the evaporated residues for the two systems shows that 12C+63Cu has a strong reaction channel that was not present in the 12C+ 65Cu system.

O modelo de cluster-alfa é aplicado aos núcleos de massa intermediária 90Sr, 92Zr, 94Mo, 96Ru e 98Pd com a Abordagem de Potencial Local. As bandas do estado fundamental dos respectivos sistemas alfa + caroço são calculadas com um único parâmetro variável, fornecendo uma boa descrição geral dos níveis experimentais. Mostra-se que o potencial alfa + caroço é fracamente dependente do momento angular L, e que tal dependência pode ser descrita de forma simples e padronizada para os cinco núcleos. O comportamento do parâmetro radial R do potencial alfa + caroço é discutido em relação ao raio do núcleo total e a soma dos raios do cluster-alfa e do caroço. As taxas de transição B(E2) reproduzem corretamente as ordens de grandeza de quase todos os dados experimentais sem o uso de cargas efetivas. A análise das separações intercluster rms e das larguras-alfa reduzidas nas bandas do estado fundamental sugere que há uma redução da intensidade de aglomeração-alfa com o aumento do spin. Uma análise complementar das bandas de estado fundamental dos núcleos 20Ne, 44Ti e 212Po aponta uma diminuição da intensidade de aglomeração-alfa com o aumento da massa nuclear, e mostra uma condição mais fraca de aglomeração-alfa para os núcleos da região do Mo em comparação com os núcleos leves. Bandas de paridade negativa são calculadas para os núcleos 92Zr, 94Mo, 96Ru e 98Pd e informações não relatadas anteriormente são comparadas a níveis experimentais disponíveis. A avaliação geral dos resultados indica que os núcleos com A par e N=52 na região do Mo possuem estruturas alfa + caroço com características semelhantes. / The alpha-cluster model is applied to the intermediate mass nuclei 90Sr, 92Zr, 94Mo, 96Ru and 98Pd with the Local Potential Approach. The ground state bands of the respective alpha + core systems are calculated with only one variable parameter, giving a good general description of the experimental data. It is shown that the alpha + core potential is weakly dependent on the angular momentum L and such dependence may be described in a simple and standardized form for the five nuclei. The behavior of the radial parameter R of the alpha + core potential is discussed in relation to the radius of the total nucleus and the sum of the radii of the alpha-cluster and the core. The calculated B(E2) transition rates reproduce correctly the orders of magnitude of almost all experimental data without the use of effective charges. The analysis of the rms intercluster separations and the reduced alpha-widths for the ground state bands suggests a reduction of the alpha-cluster intensity with the increasing spin. A complementary analysis of the ground state bands of the nuclei 20Ne, 44Ti and 212Po points to a decrease of the alpha-cluster intensity with the increasing nuclear mass, and shows a weaker alpha-cluster condition for the nuclei of the Mo region in comparison with the light nuclei. Negative parity bands are calculated for the nuclei 92Zr, 94Mo, 96Ru and 98Pd and previously not reported information are compared to available experimental levels. The general evaluation of the results indicates that the N=52 even-A nuclei in the Mo region have alpha + core structures with similar features.

O modelo de cluster-alfa é aplicado aos núcleos de massa intermediária 90Sr, 92Zr, 94Mo, 96Ru e 98Pd com a Abordagem de Potencial Local. As bandas do estado fundamental dos respectivos sistemas alfa + caroço são calculadas com um único parâmetro variável, fornecendo uma boa descrição geral dos níveis experimentais. Mostra-se que o potencial alfa + caroço é fracamente dependente do momento angular L, e que tal dependência pode ser descrita de forma simples e padronizada para os cinco núcleos. O comportamento do parâmetro radial R do potencial alfa + caroço é discutido em relação ao raio do núcleo total e a soma dos raios do cluster-alfa e do caroço. As taxas de transição B(E2) reproduzem corretamente as ordens de grandeza de quase todos os dados experimentais sem o uso de cargas efetivas. A análise das separações intercluster rms e das larguras-alfa reduzidas nas bandas do estado fundamental sugere que há uma redução da intensidade de aglomeração-alfa com o aumento do spin. Uma análise complementar das bandas de estado fundamental dos núcleos 20Ne, 44Ti e 212Po aponta uma diminuição da intensidade de aglomeração-alfa com o aumento da massa nuclear, e mostra uma condição mais fraca de aglomeração-alfa para os núcleos da região do Mo em comparação com os núcleos leves. Bandas de paridade negativa são calculadas para os núcleos 92Zr, 94Mo, 96Ru e 98Pd e informações não relatadas anteriormente são comparadas a níveis experimentais disponíveis. A avaliação geral dos resultados indica que os núcleos com A par e N=52 na região do Mo possuem estruturas alfa + caroço com características semelhantes. / The alpha-cluster model is applied to the intermediate mass nuclei 90Sr, 92Zr, 94Mo, 96Ru and 98Pd with the Local Potential Approach. The ground state bands of the respective alpha + core systems are calculated with only one variable parameter, giving a good general description of the experimental data. It is shown that the alpha + core potential is weakly dependent on the angular momentum L and such dependence may be described in a simple and standardized form for the five nuclei. The behavior of the radial parameter R of the alpha + core potential is discussed in relation to the radius of the total nucleus and the sum of the radii of the alpha-cluster and the core. The calculated B(E2) transition rates reproduce correctly the orders of magnitude of almost all experimental data without the use of effective charges. The analysis of the rms intercluster separations and the reduced alpha-widths for the ground state bands suggests a reduction of the alpha-cluster intensity with the increasing spin. A complementary analysis of the ground state bands of the nuclei 20Ne, 44Ti and 212Po points to a decrease of the alpha-cluster intensity with the increasing nuclear mass, and shows a weaker alpha-cluster condition for the nuclei of the Mo region in comparison with the light nuclei. Negative parity bands are calculated for the nuclei 92Zr, 94Mo, 96Ru and 98Pd and previously not reported information are compared to available experimental levels. The general evaluation of the results indicates that the N=52 even-A nuclei in the Mo region have alpha + core structures with similar features.