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Academic literature on the topic 'Stellar nucleosynthesi'

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Published: 9 March 2023
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Journal articles on the topic "Stellar nucleosynthesi"

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Ryan, Sean G. "Big Bang Nucleosynthesis, Population III, and Stellar Genetics in the Galactic Halo." Publications of the Astronomical Society of Australia 19, no. 2 (2002): 238–45. http://dx.doi.org/10.1071/as01067.

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AbstractThe diverse isotopic and elemental signatures produced in different nucleosynthetic sites are passed on to successive generations of stars. By tracing these chemical signatures back through the stellar populations of the Galaxy, it is possible to unravel its nucleosynthetic history and even to study stars which are now extinct. This review considers recent applications of ‘stellar genetics’ to examine the earliest episodes of nucleosynthesis in the universe, in Population iii stars and the Big Bang.
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Doherty, Carolyn, John Lattanzio, George Angelou, Simon W. Campbell, Ross Church, Thomas Constantino, Sergio Cristallo, et al. "Monash Chemical Yields Project (Monχey) Element production in low- and intermediate-mass stars." Proceedings of the International Astronomical Union 11, A29B (August 2015): 164–65. http://dx.doi.org/10.1017/s1743921316004725.

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AbstractThe Monχey project will provide a large and homogeneous set of stellar yields for the low- and intermediate- mass stars and has applications particularly to galactic chemical evolution modelling. We describe our detailed grid of stellar evolutionary models and corresponding nucleosynthetic yields for stars of initial mass 0.8 M⊙ up to the limit for core collapse supernova (CC-SN) ≈ 10 M⊙. Our study covers a broad range of metallicities, ranging from the first, primordial stars (Z = 0) to those of super-solar metallicity (Z = 0.04). The models are evolved from the zero-age main-sequence until the end of the asymptotic giant branch (AGB) and the nucleosynthesis calculations include all elements from H to Bi. A major innovation of our work is the first complete grid of heavy element nucleosynthetic predictions for primordial AGB stars as well as the inclusion of extra-mixing processes (in this case thermohaline) during the red giant branch. We provide a broad overview of our results with implications for galactic chemical evolution as well as highlight interesting results such as heavy element production in dredge-out events of super-AGB stars. We briefly introduce our forthcoming web-based database which provides the evolutionary tracks, structural properties, internal/surface nucleosynthetic compositions and stellar yields. Our web interface includes user- driven plotting capabilities with output available in a range of formats. Our nucleosynthetic results will be available for further use in post processing calculations for dust production yields.
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Salpeter, Edwin E. "Stellar nucleosynthesis." Reviews of Modern Physics 71, no. 2 (March 1, 1999): S220—S222. http://dx.doi.org/10.1103/revmodphys.71.s220.

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Weiss, A. "Stellar nucleosynthesis." Physica Scripta T133 (January 1, 2008): 014025. http://dx.doi.org/10.1088/0031-8949/2008/t133/014025.

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Vescovi, Diego. "Mixing and Magnetic Fields in Asymptotic Giant Branch Stars in the Framework of FRUITY Models." Universe 8, no. 1 (December 28, 2021): 16. http://dx.doi.org/10.3390/universe8010016.

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In the last few years, the modeling of asymptotic giant branch (AGB) stars has been much investigated, both focusing on nucleosynthesis and stellar evolution aspects. Recent advances in the input physics required for stellar computations made it possible to construct more accurate evolutionary models, which are an essential tool to interpret the wealth of available observational and nucleosynthetic data. Motivated by such improvements, the FUNS stellar evolutionary code has been updated. Nonetheless, mixing processes occurring in AGB stars’ interiors are currently not well-understood. This is especially true for the physical mechanism leading to the formation of the 13C pocket, the major neutron source in low-mass AGB stars. In this regard, post-processing s-process models assuming that partial mixing of protons is induced by magneto-hydrodynamics processes were shown to reproduce many observations. Such mixing prescriptions have now been implemented in the FUNS code to compute stellar models with fully coupled nucleosynthesis. Here, we review the new generation of FRUITY models that include the effects of mixing triggered by magnetic fields by comparing theoretical findings with observational constraints available either from the isotopic analysis of trace-heavy elements in presolar grains or from carbon AGB stars and Galactic open clusters.
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Gil-Pons, P., C. L. Doherty, J. Gutiérrez, S. W. Campbell, L. Siess, and J. C. Lattanzio. "Nucleosynthetic yields of Z = 10−5 intermediate-mass stars." Astronomy & Astrophysics 645 (December 21, 2020): A10. http://dx.doi.org/10.1051/0004-6361/201937264.

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Context. Observed abundances of extremely metal-poor stars in the Galactic halo hold clues for understanding the ancient universe. Interpreting these clues requires theoretical stellar models in a wide range of masses in the low-metallicity regime. The existing literature is relatively rich with extremely metal-poor massive and low-mass stellar models. However, relatively little information is available on the evolution of intermediate-mass stars of Z ≲ 10−5, and the impact of the uncertain input physics on the evolution and nucleosynthesis has not yet been systematically analysed. Aims. We aim to provide the nucleosynthetic yields of intermediate-mass Z = 10−5 stars between 3 and 7.5 M⊙, and quantify the effects of the uncertain wind rates. We expect these yields could eventually be used to assess the contribution to the chemical inventory of the early universe, and to help interpret abundances of selected C-enhanced extremely metal-poor (CEMP) stars. Methods. We compute and analyse the evolution of surface abundances and nucleosynthetic yields of Z = 10−5 intermediate-mass stars from their main sequence up to the late stages of their thermally pulsing (Super) AGB phase, with different prescriptions for stellar winds. We use the postprocessing code MONSOON to compute the nucleosynthesis based on the evolution structure obtained with the Monash-Mount Stromlo stellar evolution code MONSTAR. By comparing our models and others from the literature, we explore evolutionary and nucleosynthetic trends with wind prescriptions and with initial metallicity (in the very low-Z regime). We also compare our nucleosynthetic yields to observations of CEMP-s stars belonging to the Galactic halo. Results. The yields of intermediate-mass extremely metal-poor stars reflect the effects of very deep or corrosive second dredge-up (for the most massive models), superimposed with the combined signatures of hot-bottom burning and third dredge-up. Specifically, we confirm the reported trend that models with initial metallicity Zini ≲ 10−3 give positive yields of 12C, 15N, 16O, and 26Mg. The 20Ne, 21Ne, and 24Mg yields, which were reported to be negative at Zini ≳ 10−4, become positive for Z = 10−5. The results using two different prescriptions for mass-loss rates differ widely in terms of the duration of the thermally pulsing (Super) AGB phase, overall efficiency of the third dredge-up episode, and nucleosynthetic yields. We find that the most efficient of the standard wind rates frequently used in the literature seems to favour agreement between our yield results and observational data. Regardless of the wind prescription, all our models become N-enhanced EMP stars.
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Karinkuzhi, D., S. Van Eck, A. Jorissen, S. Goriely, L. Siess, T. Merle, A. Escorza, et al. "When binaries keep track of recent nucleosynthesis." Proceedings of the International Astronomical Union 14, S343 (August 2018): 438–40. http://dx.doi.org/10.1017/s1743921318006567.

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AbstractWe determine Zr and Nb elemental abundances in barium stars to probe the operation temperature of the s-process that occurred in the companion asymptotic giant branch (AGB) stars. Along with Zr and Nb, we derive the abundances of a large number of heavy elements. They provide constraints on the s-process operation temperature and therefore on the s-process neutron source. The results are then compared with stellar evolution and nucleosynthesis models. We compare the nucleosynthetic profile of the present sample stars with those of CEMP-s, CEMP-rs and CEMP-r stars. One barium star of our sample is potentially identified as the highest-metallicity CEMP-rs star yet discovered.
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AOKI, Wako, and Nobuyuki IWAMOTO. "Stellar Evolution and Nucleosynthesis." Journal of Plasma and Fusion Research 79, no. 9 (2003): 871–77. http://dx.doi.org/10.1585/jspf.79.871.

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Ryde, Nils, and Graham Harper. "Observing early stellar nucleosynthesis." Nature Astronomy 5, no. 12 (November 15, 2021): 1212–13. http://dx.doi.org/10.1038/s41550-021-01510-0.

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Truran, James W. "The Oldest Stars as Tracers of Heavy Element Formation at Early Epochs." Symposium - International Astronomical Union 204 (2001): 333–34. http://dx.doi.org/10.1017/s0074180900226247.

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Elemental abundance patterns in very metal-poor halo field stars and globular cluster stars play a crucial role both in guiding theoretical models of nucleosynthesis and in providing constraints upon the early star formation and concomitant nucleosynthesis history of our Galaxy. The abundance patterns characterizing the oldest and most metal deficient stars ([Fe/H] ≤ −3) are entirely consistent with their being products of metal-poor massive stars of lifetimes τ ≤ 108years. This includes both the elevated abundances of thealpha-elements (O, Mg, Si, S, Ca, and Ti) relative to iron-peak elements and the dominance of r-process elements over s-process elements. The nucleosynthetic contributions of lower mass AGB stars of longer lifetimes (τ ≈ 109years) begin to appear at metallicities [Fe/H] ≈ −2.5, while clear evidence for iron-peak nuclei produced in supernovae Ia (τ ≥ 1-2x109years?) does not appear until metallicities approaching [Fe/H] ~ −1. Similar trends are also suggested by abundances determined for gas clouds at high redshifts. We review the manner in which a knowledge of the abundances of the stellar and gas components of early populations, as a function of [Fe/H], time, and/or redshift, can be used to set constraints on their star formation and nucleosynthesis histories.
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Dissertations / Theses on the topic "Stellar nucleosynthesi"

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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 far was studied only indirectly leading to six orders of magnitude range of possible values for its resonance strength. The experiment has been performed at LUNA (Laboratory for Underground Nuclear Astrophysics) using the intense alpha beam of the LUNA 400 kV accelerator and a windowless gas target combined with a high-efficiency BGO detector. In the present study, an upper limit of 4.0·10−11 eV has been determined for the resonance strength. Taking into account these results, an up-dated 22Ne(α,γ)26Mg thermonuclear reaction rate was obtained and its role on the predicted 25Mg/26Mg ratio of a 5M⊙ AGBs was investigated. The data show a decrease by a factor of 15 of the intershell 25Mg/26Mg ratio. The 20Ne(p,γ)21Na is the slowest reaction of the NeNa cycle. It determines the velocity of the cycle and defines the final abundances of the isotopes synthesized in this cycle. The uncertainties on the NeNa cycle are affected by the 20Ne(p,γ)21Na reaction rate. The main goal of the second part of this thesis was the direct measurement of the Ecm = 366 keV resonance which dominates the total rate in the temperature range between 0.2 GK and 1 GK. The measurement has been performed at LUNA using the windowless gas target and two high-purity germanium detectors placed at different positions. This measurement allowed to reduce the uncertainty on the strengths of the 366 keV resonance from 18% to 7%. These results were used to update the 20Ne(p,γ)21Na reaction rate.
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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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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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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 observations of the isotope 44Ti have been reported in recent times and confirm the disagreement. As the amount of this isotope in stellar ejecta is thought to critically depend on the explosion mechanism, the ability to accurately model the observed abundance would be a pivotal step towards validating that theory. The most influential reaction to the amount of 44Ti in supernovae is 44Ti(α, p)47V. Here we report on a direct study of this reaction conducted at the REX-ISOLDE facility, CERN. The experiment was performed at a centre of mass energy 4.15±0.23 MeV, which is, for the first time, well within the Gamow window for core collapse supernovae. The experiment employed a beam of 44Ti extracted from highly irradiated components of the SINQ spallation neutron source of the Paul Scherrer Institute. No yield above background was observed, enabling an upper limit for the rate of this reaction to be determined. This result is below expectation, suggesting that the 44Ti(α, p)47V reaction proceeds more slowly than previously thought. Implications for astrophysical events, and remnant age, are discussed. In Wolf-Rayet and asymptotic giant branch (AGB) stars, the 26gAl(p,γ)27Si reaction is expected to govern the destruction of the cosmic γ-ray emitting nucleus 26Al. The rate of this reaction, however, is highly uncertain due to the unknown properties of several resonances in the temperature regime of hydrogen burning. We present a high-resolution inverse kinematic study of the 26gAl(d, p)27Al reaction as a method for constraining the strengths of key astrophysical resonances in the 26gAl(p,γ)27Si reaction. In particular, the results indicate that the resonance at Er = 127 keV in 27Si determines the entire 26gAl(p, γ)27Si reaction rate over almost the complete temperature range of Wolf-Rayet stars and AGB stars. The measurements of spectroscopic factors for many states in 27Al and a shell model calculation of nuclear properties of rp-resonant states in 27Si also allow for testing the structure model.
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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 a recent theoretical prediction, which will have a significant impact on the rate of destruction of this γ-ray producing radioisotope. The 18O(p,α )15N reaction follows similar nuclear and kinematic processes and is expected to occur in the hydrogen burning layers of AGB stars. Resonance widths have been extracted from a direct measurement in the region around a poorly constrained broad state close to the Gamow window. This has produced a new parameter set for future reference and provides new information on the reaction rate. The complex R-Matrix formalism used in these analyses is a crucial tool in the study of nuclear astrophysics reactions, and many codes have been written to implement the complex mathematics. This thesis presents a comparison of two publicly available codes from the JINA collaboration and a code used extensively by the University of Edinburgh. For this, the recent results of the 18F destruction reaction, presented here, have been used. A minor error was found within one of the codes, and corrected. The final parameters extracted, and the resulting cross sections calculations, are shown to be consistent between the three codes. A further γ-ray line of interest at 1.809 MeV, characteristic of 26Al decay, has been observed throughout the interstellar medium. If, however, this isotope is formed in a known isomeric state, its decay bypasses the emission of this γ-ray, thus complicating the interpretation of observed γ-ray fluxes. To this end, an experiment has been carried out, providing proof of principle of a direct measurement of the 26mAl(p,γ)27Si reaction. The calculation of the isomeric intensity is presented here.
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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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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 of turbulent convection, the generation of internal waves in stably stratified layers, and the rate and character of compositional mixing at convective boundaries.
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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 du fluor au cours de la combustion hydrostatique de l'hydrogene. Les consequences quant a la nucleosynthese du fluor dans les etoiles massives sont examinees. Une nouvelle evaluation du taux de format du fluor au cours de la phase de combustion de l'helium a ete effectuee a la lumiere de mesures recentes de largeur alpha. Les nouveaux taux de reaction que nous proposons permettent d'esperer trouver les conditions de la nucleosynthese du fluor
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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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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 disagreement, if the 14N(p,gamma)15O reaction rate is known with high precision. After a review of several measurements its cross section was revised downward due to a much lower contribution by one particular transition, capture to the ground state in 15O. The evaluated total relative uncertainty is still 7.5%, in part due to an unsatisfactory knowledge of the excitation function over a wide energy range. The present work reports experimentally determined cross sections as astrophysical S-factor data at twelve energies between 0.357 - 1.292 MeV for the strongest transition, capture to the 6.79 MeV excited state in 15O with lower uncertainties than before and at ten energies between 0.479 - 1.202 MeV for the second strongest transition, capture to the ground state in 15O. In addition, an R-matrix fit is performed to estimate the impact of the new data on the astrophysical relevant energy range. The recently suggested slight S-factor enhancement at the Gamow window could not be confirmed and differences to previous measurements at energies around 1 MeV were observed. The present extrapolated zero-energy S-factors are S_6.79(0) = (1.19+-0.10) keV b and S_GS(0) = (0.25+-0.05) keV b and they are within the uncertainties consistent with values recommended by the latest review.
Die 14N(p,gamma)15O Reaktion ist die langsamste Phase im Bethe-Weizsäcker-Zyklus des Wasserstoffbrennens und bestimmt deshalb die Reaktionsrate des gesamten Zyklus. Präzise Werte für die Reaktionsrate sind notwendig um das Wasserstoffbrennen in unserer Sonne besser zu verstehen. Besonders das Problem widersprüchlicher Ergebnisse aus Vorhersagen des aktuellen Sonnenmodells und helioseismologischen Experimenten könnte durch genauer bekannte 14N(p,gamma)15O Reaktionsraten aufgelöst werden. Dafür soll der solare 13N und 15O Neutrinofluss von den beta+-Zerfällen als direkter Informationsträger über die Häufigkeit von Stickstoff und Kohlenstoff im Sonneninneren genutzt werden. Der für die Berechnung der Häufigkeiten benötigte Wirkungsquerschnitt der 14N(p,gamma)15O Reaktion wurde in einer Evaluation verschiedener Messungen reduziert, da der Anteil des direkten Protoneneinfang mit Übergang in den Grundzustand deutlich weniger zum gesamten Wirkungsquerschnitt beiträgt als zuvor angenommen. Die evaluierte relative Gesamtunsicherheit ist mit 7.5% dennoch hoch, was zu einem großen Teil an ungenügendem Wissen über die Anregungsfunktion in einem weiten Energiebereich liegt. In der vorliegenden Arbeit werden experimentell ermittelte Wirkungsquerschnitte in Form von astrophysikalischen S-Faktoren für zwei Übergänge vorgestellt. Für den stärksten Übergang, den Protoneneinfang zum angeregten Zustand bei 6.79 MeV in 15O, wurden zwölf S-Faktoren bei Energien zwischen 0.357 – 1.292 MeV mit geringeren Unsicherheiten als zuvor ermittelt und für den direkten Übergang in den Grundzustand zehn Werte zwischen 0.479 – 1.202 MeV. Außerdem wurde ein R-Matrix Fit durchgeführt um den Einfluss der neuen Daten auf Extrapolationen zum astrophysikalisch relevanten Energiebereich zu prüfen. Die kürzlich vorgeschlagene Erhöhung des S-Faktors im Gamow-Fenster konnte nicht bestätigt werden und es wurden auch Unterschiede zu bisherigen Messungen im Energiebereich um 1 MeV deutlich. Die neuen extrapolierten S-Faktoren sind S679(0) = (1.19±0.10) keV b und SGS(0) = (0.25 ± 0.05) keV b und sie stimmen mit den von der Evaluation empfohlenen Werten im Rahmen ihrer Unsicherheiten überein.
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Books on the topic "Stellar nucleosynthesi"

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J, Norton Andrew, ed. Stellar evolution and nucleosynthesis. Cambridge: Cambridge University Press, 2010.

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N, Schramm David, Truran James W, Fermi National Accelerator Laboratory, and United States. National Aeronautics and Space Administration., eds. On relative supernova rates and nucleosynthesis roles. [Batavia, Ill.]: Fermi National Accelerator Laboratory, 1988.

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G, Barnes Thomas, Bash Frank N, and Lambert David L, eds. Cosmic abundances as records of stellar evolution and nucleosynthesis in honor of David L. Lambert: Proceedings of a symposium held in Austin, Texas, USA, 17-19 June 2004. San Francisco, Calif: Astronomical Society of the Pacific, 2005.

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Green, James A. Galactic Evolution and Stellar Nucleosynthesis. Greenwood Research, 1999.

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Stellar Explosions: Nucleosynthesis and Cosmochemistry. Taylor & Francis Group, 2015.

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Jose, Jordi. Stellar Explosions: Hydrodynamics and Nucleosynthesis. Taylor & Francis Group, 2016.

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Jose, Jordi. Stellar Explosions: Hydrodynamics and Nucleosynthesis. Taylor & Francis Group, 2016.

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Close, Frank. 5. Making and breaking nuclei. Oxford University Press, 2015. http://dx.doi.org/10.1093/actrade/9780198718635.003.0005.

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‘Making and breaking nuclei’ describes the process by which the atomic elements came to be in the early universe. The heat energy in the big bang, some 13.7 billion years ago, converted into counterbalanced particles of matter and antimatter. The seeds of atomic nuclei were initially the simplest constituents: quarks. During the last 5 billion years, the majority of elements found on earth were formed inside a long-dead star, where they were all cooked from protons, which were synthesised within the first second of the universe. The processes of stellar nucleosynthesis, the CNO cycle, supernovae nucleosynthesis, and cosmic spallation are explained along with the dating of the age of the Earth.
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Chiosi, C., and Alvio Renzini. Stellar Nucleosynthesis: Proceedings of the Third Workshop of the Advanced School of Astronomy of the Ettore Majorana Centre for Scientific Culture, Erice, Italy, May 11-21 1983. Springer, 2012.

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Renzini, Alvio, and Cesare Chiosi. Stellar Nucleosynthesis: Proceedings of the Third Workshop of the Advanced School of Astronomy of the Ettore Majorana Centre for Scientific Culture, Erice, Italy, May 11-21 1983. Springer, 2011.

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Book chapters on the topic "Stellar nucleosynthesi"

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Prantzos, Nikos, and Sylvia Ekström. "Stellar Nucleosynthesis." In Encyclopedia of Astrobiology, 1584–92. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1084.

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Prantzos, Nikos, and Sylvia Ekström. "Nucleosynthesis, Stellar." In Encyclopedia of Astrobiology, 1725–36. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_1084.

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Salpeter, Edwin E. "Stellar Nucleosynthesis." In More Things in Heaven and Earth, 370–74. New York, NY: Springer New York, 1999. http://dx.doi.org/10.1007/978-1-4612-1512-7_23.

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Prantzos, Nikos, and Sylvia Ekström. "Nucleosynthesis, Stellar." In Encyclopedia of Astrobiology, 1–12. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_1084-3.

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Thielemann, F. K., D. Argast, F. Brachwitz, G. Martinez-pinedo, T. Rauscher, M. Liebendörfer, A. Mezzacappa, P. Höflich, and K. Nomoto. "Nucleosynthesis and Stellar Evolution." In The Evolution of Galaxies, 25–37. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-017-3311-3_3.

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Matteucci, Francesca. "Stellar Evolution and Nucleosynthesis." In The Chemical Evolution of the Galaxy, 57–109. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0967-6_2.

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Maeda, Keiichi. "Stellar Evolution, SN Explosion, and Nucleosynthesis." In Handbook of X-ray and Gamma-ray Astrophysics, 1–41. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4544-0_85-1.

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Smith, Verne V. "Nucleosynthesis in the MS and S Stars." In Late Stages of Stellar Evolution, 241–44. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3813-7_36.

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Mathews, G. J., R. A. Ward, K. Takahashi, and W. M. Howard. "Stellar S-Process Diagnostics." In Nucleosynthesis and Its Implications on Nuclear and Particle Physics, 277–84. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4578-4_31.

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Rauscher, Thomas, Friedrich-Karl Thielemann, Robert D. Hoffman, and Stanford E. Woosley. "Nuclear Aspects of Stellar and Explosive Nucleosynthesis." In Origin of Elements in the Solar System, 143–52. Boston, MA: Springer US, 2002. http://dx.doi.org/10.1007/0-306-46927-8_12.

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Conference papers on the topic "Stellar nucleosynthesi"

1

Thielemann, F. K. "Stellar nucleosynthesis and galactic abundances." In SOLAR AND GALACTIC COMPOSITION: A Joint SOHO/ACE Workshop. AIP, 2001. http://dx.doi.org/10.1063/1.1434005.

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Hirschi, Raphael, Jacqueline den Hartogh, Andrea Cristini, Cyril Georgy, and Marco Pignatari. "Stellar structure, evolution and nucleosynthesis." In XIII Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.204.0001.

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Chieffi, Alessandro. "Element production - stellar evolution - explosive nucleosynthesis." In 11th Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.100.0296.

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El Eid, Mounib, Claudi Spitaleri, Claus Rolfs, and Rosario G. Pizzone. "Stellar Nucleosynthesis: s-Process in Massive Stars." In FIFTH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS. AIP, 2010. http://dx.doi.org/10.1063/1.3362611.

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Mengoni, A. "Neutron capture reaction rates for stellar nucleosynthesis." In CAPTURE GAMMA-RAY SPECTROSCOPY AND RELATED TOPICS: 12th International Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2187868.

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Chiosi, Cesare, Claudi Spitaleri, Claus Rolfs, and Rosario G. Pizzone. "Primordial and Stellar Nucleosynthesis Chemical Evolution of Galaxies." In FIFTH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS. AIP, 2010. http://dx.doi.org/10.1063/1.3362605.

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Zinner, Ernst. "What presolar grains tell us about stellar nucleosynthesis." In 11th Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.100.0306.

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Masseron, Thomas. "Stellar Nucleosynthesis in the Galactic History: the Carbon Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905535.

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Suzuki, Toshio, Michio Honma, Noritaka Shimizu, Yusuke Tsunoda, Takaharu Otsuka, Toshitaka Kajino, Kanji Mori, et al. "Electron-capture Rates Of Nuclei At Stellar Environments And Nucleosynthesis." In The 26th International Nuclear Physics Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.281.0155.

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Sneden, Christopher, and James E. Lawler. "An Observational Perspective on Some Aspects of Early Stellar Nucleosynthesis." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905680.

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Reports on the topic "Stellar nucleosynthesi"

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Hart, M. Boson Fermion Nuclei Stellar Nucleosynthesis: Monograph #7. Office of Scientific and Technical Information (OSTI), March 2021. http://dx.doi.org/10.2172/1773253.

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