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Dissertations / Theses on the topic 'Stellar nucleosynthesi'

Author: Grafiati

Published: 9 March 2023

Last updated: 31 July 2025

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1

MASHA, ELIANA. "ASTROPHYSICAL NUCLEAR REACTIONS ON NEON ISOTOPES AT LUNA." Doctoral thesis, Università degli Studi di Milano, 2022. http://hdl.handle.net/2434/899089.

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This thesis reports the direct measurements of the 22Ne(α,γ)26Mg and 20Ne(p,γ)21Na reactions at astrophysical energies of interest. The 22Ne(α,γ)26Mg reaction competes with the 22Ne(α,n)25Mg reaction which is the main source of neutrons for the s-process in low-mass Asymptotic Giant Branch and massive stars. At temperatures T < 300 MK where the (α,γ) channel becomes dominant, the rate of the 22Ne(α,γ)26Mg reaction is influenced by several resonances studied only indirectly. The first part of this thesis concerns the direct measurement of one of these resonances, Er = 334 keV, which so f

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2

Joseph, Craig L. "Q-nucleosynthesis : implications for stellar evolution /." The Ohio State University, 1985. http://rave.ohiolink.edu/etdc/view?acc_num=osu1487260531956577.

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3

Scholz, Philipp [Verfasser]. "Exploring statistical properties of nuclei for explosive stellar nucleosynthesis / Philipp Scholz." München : Verlag Dr. Hut, 2018. http://d-nb.info/1170473377/34.

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4

Margerin, Vincent. "Transfer reaction measurements and the stellar nucleosynthesis of 26A1 and 44Ti." Thesis, University of Edinburgh, 2016. http://hdl.handle.net/1842/25428.

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Progress in the description of stellar evolution is driven by the collaborative effort of nuclear physics, astrophysics and astronomy. Using those developments, the theory of the origin of elements in the Universe is challenged. This thesis addresses the problem behind the abundance of 44Ti and the origin of 26Al. The mismatch between the predicted abundance of 44Ti as produced by the only sites known to be able to create 44Ti, core collapse supernovae (CCSNe), and the observations, highlight the current uncertainty that exists in the physics of these stars. Several satellite based γ-ray obser

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5

Mountford, David James. "Investigations of nuclear reactions relevant to stellar γ-ray emission". Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/8238.

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The detection of γ-rays from explosive astrophysical scenarios such as novae provides an excellent opportunity for the study of on-going nucleosynthesis in the Universe. Within this context, this work has addressed an uncertainty in the destruction rate of the 18F nucleus, thought to be the primary source of 511 keV γ-rays from novae. A direct measurement of the 18F(p,α )15O cross section has provided the opportunity to extract resonance parameters through the R-Matrix formalism. The inferred parameters of populated states in 19Ne include the observation of a broad 1/2+ state, consistent with

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6

Arzhanov, Alexander. "Gogny-Hartree-Fock-Bogolyubov Nuclear Mass Models with Application to r-Process Stellar Nucleosynthesis." Thesis, KTH, Kärnfysik, 2013. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-139303.

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7

Lombardo, Linda. "Explorer l'histoire de la Galaxie grâce à la spectroscopie stellaire." Electronic Thesis or Diss., Université Paris sciences et lettres, 2022. http://www.theses.fr/2022UPSLO011.

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Ce travail de thèse présente plusieurs études qui utilisent la spectroscopie à haute résolution pour déterminer les propriétés chimiques des différentes populations stellaires de la Voie Lactée. Le document est structuré comme suit : Le premier chapitre de la thèse, divisée en 3 sections, est une introduction générale à la structure de la Voie lactée et à ses populations stellaires, suivie d'une partie décrivant les différentes méthodes utilisées pour mesurer les abondances chimiques des étoiles. La première section décrit les différents scénarios concernant la structure et la formation de la

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8

Meakin, Casey Adam. "Hydrodynamic Modeling of Massive Star Interiors." Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/194035.

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In this thesis, the hydrodynamics of massive star interiors are explored. Our primary theoretical tool is multi-dimensional hydrodynamic simulation using realistic initial conditions calculated with the one-dimensional stellar evolution code, TYCHO. The convective shells accompanying oxygen and carbon burning are examined, including models with single as well as multiple, simultaneously burning shells. A convective core during hydrogen burning is also studied in order to test the generality of the flow characteristics. Two and three dimensional models are calculated. We analyze the properties

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9

KIOUS, MALEK. "Determination de taux de reactions nucleaires conduisant a la nucleosynthese stellaire du fluor." Paris 11, 1990. http://www.theses.fr/1990PA112371.

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La nucleosynthese stellaire du fluor reste a ce jour inexpliquee. Si l'on en croit les taux de reaction admis actuellement, le fluor synthetise au cours de la combustion de l'hydrogene ou de l'helium est immediatement detruit. Nous avons entrepris l'etude spectroscopique des niveaux du neon vingt (participant a la combustion du fluor) situes pres du seuil proton. Nous avons en particulier mis en evidence l'importance d'un niveau proche du seuil proton, qui par des effets d'interferences qu'il induit avec les autres niveaux de meme spin-parite, modifie de facon importante le taux de destruction

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10

Wagner, Louis. "Precise nuclear data of the 14N(p,gamma)15O reaction for solar neutrino predictions." Helmholtz-Zentrum Dresden-Rossendorf, 2018. https://tud.qucosa.de/id/qucosa%3A31122.

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The 14N(p,gamma)15O reaction is the slowest stage of the carbon-nitrogen-oxygen cycle of hydrogen burning and thus determines its reaction rate. Precise knowledge of its rate is required to improve the model of hydrogen burning in our sun. The reaction rate is a necessary ingredient for a possible solution of the solar abundance problem that led to discrepancies between predictions of the solar standard model and helioseismology. The solar 13N and 15O neutrino fluxes are used as independent observables that probe the carbon and nitrogen abundances in the solar core. This could settle the disag

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11

Herwig, Falk. "Evolution of late stages of intermediate mass stars : mixing processes and their consequences for stellar evolution and nucleosynthesis /." Aachen : Shaker, 1998. http://catalogue.bnf.fr/ark:/12148/cb37322724p.

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Texte traduit de: Dissertation--Mathematisch-Naturwissenschaftliche Fakultät--Kiel--Christian-Albrechts-Universität, 1998. Titre de soutenance : Spätphasen der Entwicklung von Sternen mittlerer Masse : Mischprozesse und ihre Bedeutung für Sternentwicklung und Elementsynthese.

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12

Neyskens, Pieter. "Exploring S stars: stellar parameters, abundances and constraints on the s-process from a new grid of model atmospheres." Doctoral thesis, Universite Libre de Bruxelles, 2014. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209358.

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More than 80% of the stars in the Universe are expected to have initial masses below eight to ten times the mass of our sun. These low mass stars, including our sun, become cool red giants during one of the final evolutionary stages of their life: the Asymptotic Giant Branch (or AGB) phase. AGB stars are among the main producers of carbon and heavy (s-process) elements in the Universe. These elements are synthesized inside the star and mixed to the stellar atmosphere where stellar winds are responsible for the loss of more than 50% of the stellar mass, hence, AGB stars are strong polluters of

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13

Slemer, Alessandra. "Chemical ejecta and final fates of intermediate-mass and massive stars." Doctoral thesis, Università degli studi di Padova, 2017. http://hdl.handle.net/11577/3422388.

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In my PhD work I carried out a detailed investigation on the final fates and chemical ejecta produced by intermediate-mass and massive stars. The first part of the thesis is focused on massive and very massive stars. We derive the ejecta for a large number of elemental species (H, He, C, N, O, F, Ne, Na, Mg, Al, Si, S Ar, K, Ca, Sc, Ti, Cr, Mn, Fe, Ni, Zn) during the pre-supernova evolution and after the explosion or collapse event. We use a set of stellar tracks computed with PAdova and TRieste Stellar Evolution Code (PARSEC), with initial masses in the range between 8 M to 350 M , for thirt

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14

Hosford, A. "Temperature scales and the "lithium problem"." Thesis, University of Hertfordshire, 2010. http://hdl.handle.net/2299/4401.

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The discovery of the Spite plateau in the abundances of 7Li for metal-poor stars led to the determination of an observationally deduced primordial lithium abundance. However, with the determination of the baryon density, Omega_B_h^2, from the Wilkinson Microwave Anisotropy Probe (WMAP) data, a discrepancy arose between observationally determined and theoretically determined abundances of 7Li. This is what has become known as the “lithium problem”. Of all the uncertain factors in determining a stellar Li abundance, the effective temperature is the most important. This thesis is concerned with d

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15

Mattsson, Lars. "On the Winds of Carbon Stars and the Origin of Carbon : A Theoretical Study." Doctoral thesis, Uppsala universitet, Astronomi och rymdfysik, 2009. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-99593.

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Carbon is the basis for life, as we know it, but its origin is still largely unclear. Carbon-rich Asymptotic Giant Branch (AGB) stars (carbon stars) play an important rôle in the cosmic matter cycle and may contribute most of the carbon in the Galaxy. In this thesis it is explored how the dust-driven mass loss of these stars depends on the basic stellar parameters by computing a large grid of wind models. The existence of a critical wind regime and mass-loss thresholds for dust-driven winds are confirmed. Furthermore, a steep dependence of mass loss on carbon excess is found. Exploratory work

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16

Kahane, Claudine. "Observations millimétriques de molécules circumstellaires : de la recherche de nouvelles espèces, à la mesure d'abondances isotopiques." Phd thesis, Grenoble 1, 1989. http://tel.archives-ouvertes.fr/tel-00724537.

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La première partie de ce travail concerne la recherche de nouvelles molécules interstellaires et circumstellaires. Après une description des divers hamiltoniens utilisés pour le calcul des fréquences des spectres moléculaires dans le domaine des ondes millimétriques,elle expose la recherche et la détection de nouvelles molécules, à l'aide d'observations réalisées avec le radiotélescope de 30m de l 'IRAM, ainsi que la couverture spectrale, effectuée à 2mm et 3mm, de l'émission de l'enveloppe circumstellaire IRC+ 10216. La deuxième partie de ce travail est consacrée à la détermination de rapport

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17

Ritter, Christian Heiko. "Nucleosynthesis in stellar models across initial masses and metallicities and implications for chemical evolution." Thesis, 2017. http://hdl.handle.net/1828/7983.

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Tracing the element enrichment in the Universe requires to understand the element production in stellar models which is not well understood, in particular at low metallicity. In this thesis a variety of nucleosynthesis processes in stellar models across initial masses and metallicities is investigated and their relevance for chemical evolution explored. Stellar nucleosynthesis is investigated in asymptotic giant branch (AGB) models and massive star models with initial masses between 1 M⊙ and 25 M⊙ for metal fractions of Z = 0.02, 0.01, 0.006, 0.001, 0.0001. A yield grid with elements from H t

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18

Shingles, Luke Jeremy. "Neutron-Capture Nucleosynthesis and the Chemical Evolution of Globular Clusters." Phd thesis, 2015. http://hdl.handle.net/1885/16507.

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Elements heavier than iron are almost entirely produced in stars through neutron captures and radioactive decays. Of these heavy elements, roughly half are produced by the slow neutron-capture process (s-process), which takes place under extended exposure to low neutron densities. Most of the s-process production occurs in stars with initial masses between roughly 0.8 and 8 M , which evolve through the Asymptotic Giant Branch (AGB) phase. This thesis explores several topics related to AGB stars and the s-process, with a focus on comparing theoretical models to observations in the litera

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19

Clarkson, Ondrea. "The first stars and the convective-reactive regime." Thesis, 2020. http://hdl.handle.net/1828/12548.

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Due to their initially metal-free composition, the fi rst stars in the Universe, which are termed Population III (Pop III) stars, were fundamentally different than later generations of stars. As of now, we have yet to observe a truly metal-free star although much effort has been placed on this task and that of nding the second generation of stars. Given they were the first stars, Pop III stars are expected to have made the fi rst contributions to elements heavier than those produced during the Big Bang. For decades signi cant mixing between H and He burning layers has been reported in

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20

Kotachery, Devika Kamath. "Testing stellar models with observations from AGB and post-AGB stars." Phd thesis, 2013. http://hdl.handle.net/1885/149739.

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Low- to intermediate-mass stars (0.8 - 7 M{u2299}) are interesting in a broad astronomical context because they produce large amounts of electromagnetic radiation, they eject large amounts of mass, and the ejected mass contains many products of internal nucleosynthesis. However, theoretical studies of the evolution of red-giants are inhibited by uncertainties in important processes such as mass loss, convective mixing, and grain formation in stellar winds. From an observational point of view it is difficult to determine stellar parameters such as the initial mass and metallicity. This makes it

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21

Roederer, Ian Ulysses. "From heavy atoms to the outer galaxy : characterizing the chemistry of the Milky Way halo." Thesis, 2010. http://hdl.handle.net/2152/ETD-UT-2010-08-1642.

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This dissertation describes our efforts to use the assembly of matter on nuclear scales as a probe of the assembly of matter on Galactic scales. To investigate the former, we characterize the detailed abundance patterns of the heaviest elements found in ancient, metal-poor stars in the Galaxy. In particular, we place new constraints on and identify several new correlations among the nuclei produced by the rapid nucleosynthetic process, which we use to refine current models of the physical conditions of this process. To investigate the latter, we apply our knowledge of stellar nucleosynthesis t

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22

Gawlik, Aleksandra. "Radiative neutron capture cross sections measurement of 70Ge at n_TOF CERN facility and its relevance for stellar nucleosynthesis." Phd diss., 2019. http://hdl.handle.net/11089/28769.

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Stellar nucleosynthesis is the name given to the nuclear reactions taking place in stars to create the nuclei of the chemical elements. Elements heavier than iron/nickel are dominantly created by neutron capture reactions. Neutron capture reactions are responsible for forming about 99% of the elements of mass number >56. When neutron densities are rather small and radioactive decay is generally faster than subsequent neutron capture on radionuclides, it is the so called s process (slow). In environments with high neutron densities nuclei can capture many neutrons, increasing rapidly their mass

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23

Peplowski, Patrick N. "The lowest L = 0 proton resonance in Si-26 and its implications for the stellar nucleosynthesis of Al-26." 2009. http://etd.lib.fsu.edu/theses/available/etd-03182009-144142.

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Thesis (Ph. D.)--Florida State University, 2009.<br>Advisor: Ingo Wiedenhöver, Florida State University, College of Arts and Sciences, Dept. of Physics. Title and description from dissertation home page (viewed Aug.12, 2009). Document formatted into pages; contains xiii, 111 pages. Includes bibliographical references.

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24

Falahat, Sascha [Verfasser]. "Experimental investigation of the reactions 25Mg(α,n)28Si [25Mg(alpha,n)28Si], 26Mg(α,n)29Si, [25Mg(alpha,n)29Si] {18O(α,n)21Ne [18O(alpha,n)2Ne] and their impact on stellar nucleosynthesis / vorgelegt von Sascha Falahat". 2010. http://d-nb.info/1005373272/34.

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