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Journal articles on the topic 'Stellar nucleosynthesi'

Author: Grafiati

Published: 9 March 2023

Last updated: 31 July 2025

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1

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 та ін. "Monash Chemical Yields Project (Monχey) Element production in low- and intermediate-mass stars". Proceedings of the International Astronomical Union 11, A29B (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

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3

Salpeter, Edwin E. "Stellar nucleosynthesis." Reviews of Modern Physics 71, no. 2 (1999): S220—S222. http://dx.doi.org/10.1103/revmodphys.71.s220.

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4

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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5

Vescovi, Diego. "Mixing and Magnetic Fields in Asymptotic Giant Branch Stars in the Framework of FRUITY Models." Universe 8, no. 1 (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

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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 ai

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Tolasa, Diriba. "Stellar Evolution and Nucleosynthesis: Investigating the Life Cycles of Massive Stars and Their Role in Galactic Chemical Enrichment." Engineering Physics 8, no. 1 (2025): 24–40. https://doi.org/10.11648/j.ep.20250801.13.

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Stellar evolution and nucleosynthesis are fundamental processes that govern the life cycles of massive stars, significantly influencing the chemical enrichment of galaxies. This study aims to elucidate the intricate mechanisms underlying the evolution of massive stars, from their formation in molecular clouds to their explosive demise as supernovae. Massive stars, defined as those with initial masses exceeding approximately eight solar masses, undergo a series of complex nuclear fusion reactions that synthesize heavier elements, thereby contributing to the cosmic abundance of elements beyond h

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Monpribat, E., A. Choplin, S. Martinet, et al. "A new ¹²C+¹²C reaction rate: Impact on stellar evolution." EPJ Web of Conferences 279 (2023): 11016. http://dx.doi.org/10.1051/epjconf/202327911016.

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Among the reactions driving stellar evolution during carbon burning, 12C + 12C fusion provides the key ingredients. This system reveals many resonances, but also regions with suppressed fusion cross-sections. The reaction was recently measured by the STELLA collaboration utilizing the gammaparticle coincidence technique for precise cross-section measurements reaching down to the Gamow window of massive stars. From the experimental data, reaction rates were determined by approximating a hindrance parametrization and by adding on top a resonance at the lowest measured energy. The impact of these

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9

Karinkuzhi, D., S. Van Eck, A. Jorissen, et al. "When binaries keep track of recent nucleosynthesis." Proceedings of the International Astronomical Union 14, S343 (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 ou

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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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11

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

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12

Fok, Hung Kwan, Marco Pignatari, Benoît Côté, and Reto Trappitsch. "Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties." Astrophysical Journal Letters 977, no. 1 (2024): L24. https://doi.org/10.3847/2041-8213/ad91ab.

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Abstract Presolar grains are stardust particles that condensed in the ejecta or in the outflows of dying stars and can today be extracted from meteorites. They recorded the nucleosynthetic fingerprint of their parent stars and thus serve as valuable probes of these astrophysical sites. The most common types of presolar silicon carbide grains (called mainstream SiC grains) condensed in the outflows of asymptotic giant branch stars. Their measured silicon isotopic abundances are not significantly influenced by nucleosynthesis within the parent star but rather represent the pristine stellar compo

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13

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

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14

Benjamin Wehmeyer, Andr´es Yag¨ue L´opez, Benoit Cˆot´e, Maria K. Pet˝o, Chiaki Kobayashi, and Maria Lugaro. "Galactic Chemical Evolution with the short lived radioisotopes \(^{53}\textbf{Mn}\), \(^{60}\textbf{Fe}\), \(^{182}\textbf{Hf}\), and \(^{244}\textbf{Pu}\)." Communications in Physics 32, no. 4S (2023): 453. http://dx.doi.org/10.15625/0868-3166/17727.

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Modelling the Galactic chemical evolution (GCE) of short-lived radioisotopes (SLRs, with half-lives of the order of million years) can provide timing information on recent nucleosynthesis. The knowledge of their spatial distribution throughout the interstellar medium (ISM) is crucial. We are using a three-dimensional GCE model to investigate the evolution of four SLRs: \(^{53}\)Mn from supernovae of type Ia (SNeIa), \(^{60}\)Fe from core-collapse supernovae (CCSNe), \(^{182}\)Hf from stellar winds from intermediate mass stars (IMSs), and \(^{244}\)Pu from neutron star mergers (NSMs) to explain

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15

Aliotta, M., R. Buompane, M. Couder, et al. "The status and future of direct nuclear reaction measurements for stellar burning." Journal of Physics G: Nuclear and Particle Physics 49, no. 1 (2021): 010501. http://dx.doi.org/10.1088/1361-6471/ac2b0f.

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Abstract The study of stellar burning began just over 100 years ago. Nonetheless, we do not yet have a detailed picture of the nucleosynthesis within stars and how nucleosynthesis impacts stellar structure and the remnants of stellar evolution. Achieving this understanding will require precise direct measurements of the nuclear reactions involved. This report summarizes the status of direct measurements for stellar burning, focusing on developments of the last couple of decades, and offering a prospectus of near-future developments.

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Vescovi, Diego. "News on the slow neutron capture process in AGB stars." EPJ Web of Conferences 279 (2023): 06001. http://dx.doi.org/10.1051/epjconf/202327906001.

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Asymptotic giant branch (AGB) stars are responsible for the production of the main component of the solar s-process distribution. Despite enormous progress in the theoretical modeling of these objects over the last few decades, many uncertainties remain. The still-unknown mechanism leading to the production of 13C neutron source is one example. The nucleosynthetic signature of AGB stars can be examined in a number of stellar sources, from spectroscopic observations of intrinsic and extrinsic stars to the heavy-element isotopic composition of presolar grains found in meteorites. The wealth of a

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17

Rizzuti, Federico, Raphael Hirschi, Vishnu Varma, et al. "Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase." Galaxies 12, no. 6 (2024): 87. https://doi.org/10.3390/galaxies12060087.

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Our understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models can improve this knowledge by studying multi-D processes, but only for a short time range (minutes or hours). Recent advances in computing resources have enabled 3D stellar models to reproduce longer time scales and include nuclear reactions, making the simulations more accurate and allowing to study explicit nucleosynthesis. Here, we present results from 3D s

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18

Norris, John E. "Stellar chemical evolution." Symposium - International Astronomical Union 189 (1997): 407–16. http://dx.doi.org/10.1017/s007418090011695x.

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One of the major achievements of astrophysics has been the demonstration that most of the chemical elements have been synthesized in stars: nucleosynthesis calculations of homogeneous and inhomogeneous big bang cosmologies show that, in comparison with the most metal-poor stars currently known, essentially no elements heavier than B existed at the era of decoupling (see e.g. Wagoner, Fowler, & Hoyle 1967; Kajino, Mathews, & Fuller 1990). Following the pioneering work on stellar nucleosynthesis by Hoyle (1946), the basic precepts and the role of stars was set down in the classic papers

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19

Spite, Monique, and François Spite. "Li isotopes in metal-poor halo dwarfs: a more and more complicated story." Proceedings of the International Astronomical Union 5, S268 (2009): 201–10. http://dx.doi.org/10.1017/s1743921310004138.

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AbstractThe nuclei of the lithium isotopes are fragile, easily destroyed, so that, at variance with most of the other elements, they cannot be formed in stars through steady hydrostatic nucleosynthesis.The 7Li isotope is synthesized during primordial nucleosynthesis in the first minutes after the Big Bang and later by cosmic rays, by novae and in pulsations of AGB stars (possibly also by the ν process). 6Li is mainly formed by cosmic rays. The oldest (most metal-deficient) warm galactic stars should retain the signature of these processes if, (as it had been often expected) lithium is not depl

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20

Sneden, Christopher, James E. Lawler, Elizabeth A. Den Hartog, and Michael E. Wood. "Atomic Data for Stellar Nucleosynthesis." Proceedings of the International Astronomical Union 11, A29A (2015): 287–90. http://dx.doi.org/10.1017/s1743921316003069.

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AbstractStellar chemical composition analyses can only yield reliable abundances if the atomic transition parameters are accurately determined. During the last couple of decades a renewed emphasis on laboratory spectroscopy has produced large sets of useful atomic transition probabilities for species of interest to stellar spectroscopists. In many cases the transition data are of such high quality that they play little part in the abundance uncertainties. We summarize the current state of atomic parameters, highlighting the areas of satisfactory progress and noting places, where further labora

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21

Cristallo, Sergio. "Neutron captures in stellar nucleosynthesis." EPJ Web of Conferences 275 (2023): 01006. http://dx.doi.org/10.1051/epjconf/202327501006.

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Apart from cosmological hydrogen and helium, chemical elements in the Universe are produced in stars, during both quiescent and explosive phases. The Sun chemical distribution witnesses the pollution from already extinct stellar generations at different epochs before the Solar System formation. The two major nucleosynthesis processes responsible for the formation of elements heavier than iron are the slow neutron capture process (the s-process) and the rapid neutron capture process (the r-process). A third, less common, nucleosynthesis channel is related to the intermediate neutron capture pro

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22

Hollowell, David, and Icko Iben. "Nucleosynthesis and Mixing in Low- and Intermediate-Mass AGB Stars." International Astronomical Union Colloquium 108 (1988): 38–43. http://dx.doi.org/10.1017/s0252921100093374.

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AbstractThe existence of carbon stars brighter than Mbol=-4 can be understood in terms of dredge up in thermally pulsing asymptotic giant branch (AGB) stars. As a low- or intermediate-mass star evolves on the AGB, the large fluxes engendered in a helium shell flash cause the base of the convective envelope to extend into the radiative, carbon-rich region, and transport nucleosynthesis products to the stellar surface. Numerical models indicate that AGB stars with sufficiently massive stellar envelopes can become carbon stars via this standard dredge-up mechanism. AGB stars with less massive ste

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23

Karakas, Amanda I. "Stellar yields – theory and observations." Proceedings of the International Astronomical Union 11, A29B (2015): 162–63. http://dx.doi.org/10.1017/s1743921316004713.

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AbstractStellar yields are an essential tool for studies of chemical evolution. For low and intermediate-mass stars (0.8 up to 8-10M⊙) the richest nucleosynthesis occurs when the stars are on the asymptotic giant branch (AGB) of stellar evolution. We discuss the main nucleosynthesis outcomes, along with the uncertainties that affect the theoretical calculations. The uncertainties in the physics can be improved by comparing theoretical models to observations, including chemically peculiar metal-poor stars, along with AGB stars and their progeny.

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Griffith, Emily J., David W. Hogg, Julianne J. Dalcanton, et al. "KPM: A Flexible and Data-driven K-process Model for Nucleosynthesis." Astronomical Journal 167, no. 3 (2024): 98. http://dx.doi.org/10.3847/1538-3881/ad19c7.

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Abstract The element abundance pattern found in Milky Way disk stars is close to two-dimensional, dominated by production from one prompt process and one delayed process. This simplicity is remarkable, since the elements are produced by a multitude of nucleosynthesis mechanisms operating in stars with a wide range of progenitor masses. We fit the abundances of 14 elements for 48,659 red-giant stars from APOGEE Data Release 17 using a flexible, data-driven K-process model—dubbed KPM. In our fiducial model, with K = 2, each abundance in each star is described as the sum of a prompt and a delayed

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Lamia, L. "Nuclear reactions involving light elements & BBN." EPJ Web of Conferences 297 (2024): 01008. http://dx.doi.org/10.1051/epjconf/202429701008.

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Light elements play a key role in different scenario in astrophysics, ranging from primordial nucleosynthesis up to stellar nucleosynthesis and cosmic ray nucleosynthesis. The nuclear reaction cross section measurements of interest in primordial and stellar nucleosynthesis have been investigated in terrestrial laboratories via devoted experiments. However, because of the difficulties in reaching the Gamow energy windows of interest for such processes through direct approaches, the indirect Trojan Horse Method (THM) have been used in the last ’30 years for shedding light on some unsolved questi

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Vescovi, Diego. "Fundamentals of stellar evolution and nucleosynthesis." EPJ Web of Conferences 297 (2024): 01014. http://dx.doi.org/10.1051/epjconf/202429701014.

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The theory of stellar structure and evolution plays a pivotal role in modern astrophysics. Stellar evolution calculations are used to determine the ages and, to a lesser extent, distances of stars, which are critical to our knowledge of the history and structure of galaxies. Moreover, since virtually all chemical elements (except hydrogen) can be synthesized inside stars, knowing the chemical history of the Universe requires understanding stellar evolution. Here, we briefly outline the basic physical processes at work in stellar structures and examine some of the most relevant aspects of the l

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Brauer, Kaley, Andrew Emerick, Jennifer Mead, et al. "AEOS: Star-by-star Cosmological Simulations of Early Chemical Enrichment and Galaxy Formation." Astrophysical Journal 980, no. 1 (2025): 41. https://doi.org/10.3847/1538-4357/ada4a1.

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Abstract The Aeos project introduces a series of high-resolution cosmological simulations that model star-by-star chemical enrichment and galaxy formation in the early Universe, achieving 1 pc resolution. These simulations capture the complexities of galaxy evolution within the first ~300 Myr by modeling individual stars and their feedback processes. By incorporating chemical yields from individual stars, Aeos generates galaxies with diverse stellar chemical abundances, linking them to hierarchical galaxy formation and early nucleosynthetic events. These simulations underscore the importance o

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Woosley, S. E., A. Heger, L. Roberts, and R. D. Hoffman. "Nucleosynthesis Now and Then." Proceedings of the International Astronomical Union 5, S265 (2009): 3–11. http://dx.doi.org/10.1017/s1743921310000086.

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AbstractToday we understand, to reasonable accuracy, the origin of most of the abundant elements in the sun and similar Population I stars. Given our relatively primitive ability to model supernova explosion mechanisms, stellar mass loss, and stellar mixing, this is a remarkable achievement. This understanding is possible, in part, because supernovae are highly constrained by their spectra, light curves and the sorts of remnants they leave. This same understanding extends to the major abundances seen in primitive metal-poor stars down to [Fe/H] > −4. In particular, one finds no compelling e

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29

Cahoone, Lawrence E. "Is Stellar Nucleosynthesis a Good Thing?" Environmental Ethics 38, no. 4 (2016): 421–39. http://dx.doi.org/10.5840/enviroethics201638436.

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30

Stasińska, G. "Planetary Nebulae, Tracers of Stellar Nucleosynthesis." EAS Publications Series 32 (2008): 173–85. http://dx.doi.org/10.1051/eas:0832005.

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Gustafsson, B. "Nucleosynthesis and future stellar abundance determinations." EAS Publications Series 11 (2004): 21–50. http://dx.doi.org/10.1051/eas:2004002.

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32

Käppeler, F. "Reaction rates, nucleosynthesis, and stellar structure." Nuclear Instruments and Methods in Physics Research Section B: Beam Interactions with Materials and Atoms 259, no. 1 (2007): 663–68. http://dx.doi.org/10.1016/j.nimb.2007.01.296.

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Schatz, Gerd. "The s-process of stellar nucleosynthesis." Progress in Particle and Nuclear Physics 17 (January 1986): 393–417. http://dx.doi.org/10.1016/0146-6410(86)90027-x.

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34

Wannier, Peter G. "Abundances in the Galactic Center." Symposium - International Astronomical Union 136 (1989): 107–19. http://dx.doi.org/10.1017/s0074180900186395.

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Abundance measurements in the Galactic Center (GC) probe material with a nucleosynthetic history unique in our Galaxy. The measurements are of two types: probing interstellar and stellar material. Measurements of gas-phase abundances are mostly toward SgrB2 and SgrA. They reflect the current state of nuclear evolution in the GC and include several important isotope abundance ratios. The isotope ratios provide the most accurate information and allow for comparison with results elsewhere in the interstellar medium. The second type of measurement is of abundances in (and around) stars, yielding c

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Sergi, Maria Letizia, Giuseppe D’Agata, Giovanni Luca Guardo, et al. "Trojan Horse Investigation for AGB Stellar Nucleosynthesis." Universe 8, no. 2 (2022): 128. http://dx.doi.org/10.3390/universe8020128.

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Asymptotic Giant Branch (AGB) stars are among the most important astrophysical sites influencing the nucleosynthesis and the chemical abundances in the Universe. From a pure nuclear point of view, several processes take part during this peculiar stage of stellar evolution thus requiring detailed experimental cross section measurements. Here, we report on the most recent results achieved via the application of the Trojan Horse Method (THM) and Asymptotic Normalization Coefficient (ANC) indirect techniques, discussing the details of the experimental procedure and the deduced reaction rates. In a

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Holmbeck, Erika M., and Jeff J. Andrews. "Total r-process Yields of Milky Way Neutron Star Mergers." Astrophysical Journal 963, no. 2 (2024): 110. http://dx.doi.org/10.3847/1538-4357/ad1e52.

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Abstract While it is now known that the mergers of double neutron star binary systems (NSMs) are copious producers of heavy elements, there remains much speculation about whether they are the sole or even principal site of rapid neutron-capture (r-process) nucleosynthesis, one of the primary ways in which heavy elements are produced. The occurrence rates, delay times, and galactic environments of NSMs hold sway over estimating their total contribution to the elemental abundances in the solar system and the Galaxy. Furthermore, the expected elemental yields of NSMs may depend on the merger para

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Schramm, D. N. "Big Bang Nucleosynthesis." Symposium - International Astronomical Union 187 (2002): 1–15. http://dx.doi.org/10.1017/s0074180900113695.

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Big Bang Nucleosynthesis (BBN) is on the verge of undergoing a transformation now that extragalactic deuterium is being measured. Previously, the emphasis was on demonstrating the concordance of the Big Bang Nucleosynthesis model with the abundances of the light isotopes extrapolated back to their primordial values using stellar and Galactic evolution theories. Once the primordial deuterium abundance is converged upon, the nature of the field will shift to using the much more precise primordial D/H to constrain the more flexible stellar and Galactic evolution models (although the question of p

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Courtin, S., M. Heine, E. Monpribat, and J. Nippert. "Carbon burning at stellar energies." Journal of Physics: Conference Series 2586, no. 1 (2023): 012114. http://dx.doi.org/10.1088/1742-6596/2586/1/012114.

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Abstract Fusion reactions with light nuclei play an essential role in understanding the energy production, the nucleosynthesis of chemical elements and the evolution of massive stars. The measurement of key fusion reactions at stellar energies is thus of interest, but highly challenging since the associated cross sections are extremely small, of the sub-nanobarn range. Among these reactions, the fusion of carbon nuclei, which drives the stellar carbon burning phase, is deeply connected with essential microscopic features such as the impact of symmetries, the access to quantum states, emerging

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Griffith, Emily J., David W. Hogg, Sten Hasselquist, et al. "Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components." Astronomical Journal 169, no. 5 (2025): 280. https://doi.org/10.3847/1538-3881/adc07f.

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Abstract Many nucleosynthetic channels create the elements, but two-parameter models characterized by α and Fe nonetheless predict stellar abundances in the Galactic disk to accuracies of 0.02–0.05 dex for most measured elements, near the level of current abundance uncertainties. It is difficult to make individual measurements more precise than this to investigate lower-amplitude nucleosynthetic effects, but population studies of mean abundance patterns can reveal more subtle abundance differences. Here, we look at the detailed abundances for 67,315 stars from the Apache Point Observatory Gala

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de los Reyes, Mithi A. C., Evan N. Kirby, Alexander P. Ji, and Evan H. Nuñez. "Simultaneous Constraints on the Star Formation History and Nucleosynthesis of Sculptor dSph." Astrophysical Journal 925, no. 1 (2022): 66. http://dx.doi.org/10.3847/1538-4357/ac332b.

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Abstract We demonstrate that using up to seven stellar abundance ratios can place observational constraints on the star formation histories (SFHs) of Local Group dSphs, using Sculptor dSph as a test case. We use a one-zone chemical evolution model to fit the overall abundance patterns of α elements (which probe the core-collapse supernovae that occur shortly after star formation), s-process elements (which probe AGB nucleosynthesis at intermediate delay times), and iron-peak elements (which probe delayed Type Ia supernovae). Our best-fit model indicates that Sculptor dSph has an ancient SFH, c

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Weiss, Achim. "Round table discussion on session D: stellar evolution, nucleosynthesis and convective mixing." Proceedings of the International Astronomical Union 2, S239 (2006): 294–95. http://dx.doi.org/10.1017/s1743921307000579.

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Meynet, Georges. "Rotation, mass loss and nucleosynthesis." Proceedings of the International Astronomical Union 2, no. 14 (2006): 209. http://dx.doi.org/10.1017/s1743921307010216.

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Giannaka, P. G., and T. S. Kosmas. "Electron Capture Cross Sections for Stellar Nucleosynthesis." Advances in High Energy Physics 2015 (2015): 1–11. http://dx.doi.org/10.1155/2015/398796.

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In the first stage of this work, we perform detailed calculations for the cross sections of the electron capture on nuclei under laboratory conditions. Towards this aim we exploit the advantages of a refined version of the proton-neutron quasiparticle random-phase approximation (pn-QRPA) and carry out state-by-state evaluations of the rates of exclusive processes that lead to any of the accessible transitions within the chosen model space. In the second stage of our present study, we translate the abovementionede--capture cross sections to the stellar environment ones by inserting the temperat

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Chiosi, C. "Stellar Nucleosynthesis and Chemical Evolution of Galaxies." EAS Publications Series 27 (2007): 25–39. http://dx.doi.org/10.1051/eas:2007142.

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Schuler, Simon C., Jeremy R. King, and Lih-Sin The. "STELLAR NUCLEOSYNTHESIS IN THE HYADES OPEN CLUSTER." Astrophysical Journal 701, no. 1 (2009): 837–49. http://dx.doi.org/10.1088/0004-637x/701/1/837.

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Reifarth, René, Stefan Fiebiger, Kathrin Göbel, et al. "Treatment of isomers in nucleosynthesis codes." International Journal of Modern Physics A 33, no. 09 (2018): 1843011. http://dx.doi.org/10.1142/s0217751x1843011x.

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The decay properties of long-lived excited states (isomers) can have a significant impact on the destruction channels of isotopes under stellar conditions. In sufficiently hot environments, the population of isomers can be altered via thermal excitation or de-excitation. If the corresponding lifetimes are of the same order of magnitude as the typical time scales of the environment, the isomers have to be treated explicitly. We present a general approach to the treatment of isomers in stellar nucleosynthesis codes and discuss a few illustrative examples. The corresponding code is available onli

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Bandyopadhyay, Avrajit, and Timothy C. Beers. "Recent Advances in Understanding R-Process Nucleosynthesis in Metal-Poor Stars and Stellar Systems." Universe 11, no. 7 (2025): 229. https://doi.org/10.3390/universe11070229.

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The rapid neutron-capture process (r-process) is responsible for the creation of roughly half of the elements heavier than iron, including precious metals like silver, gold, and platinum, as well as radioactive elements such as thorium and uranium. Despite its importance, the nature of the astrophysical sites where the r-process occurs, and the detailed mechanisms of its formation, remain elusive. The key to resolving these mysteries lies in the study of chemical signatures preserved in ancient, metal-poor stars. These stars, which formed in the early Universe, retain the chemical fingerprints

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Shetye, S., S. Goriely, L. Siess, S. Van Eck, A. Jorissen, and H. Van Winckel. "Observational evidence of third dredge-up occurrence in S-type stars with initial masses around 1 M⊙." Astronomy & Astrophysics 625 (April 30, 2019): L1. http://dx.doi.org/10.1051/0004-6361/201935296.

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Context. S stars are late-type giants with spectra showing characteristic molecular bands of ZrO in addition to the TiO bands typical of M stars. Their overabundance pattern shows the signature of s-process nucleosynthesis. Intrinsic, technetium (Tc)-rich S stars are the first objects on the asymptotic giant branch (AGB) to undergo third dredge-up (TDU) events. Exquisite Gaia parallaxes now allow for these stars to be precisely located in the Hertzsprung–Russell (HR) diagram. Here we report on a population of low-mass, Tc-rich S stars previously unaccounted for by stellar evolution models. Aim

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Gustafsson, Bengt, and Nils Ryde. "Carbon Stars and Nucleosynthesis in Galaxies." Symposium - International Astronomical Union 177 (2000): 481–96. http://dx.doi.org/10.1017/s007418090000276x.

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The role of carbon stars in the build-up of chemical elements in galaxies is discussed on the basis of stellar evolution calculations and estimated stellar yields, abundance analyses of AGB stars, galactic-evolution models and abundance trends among solar-type disk stars. We conclude that the AGB stars in general, and carbon stars in particular, probably are main contributors of s-elements, that their contributions of flourine and carbon are quite significant, and that possibly their contributions of lithium, 13C and 22Ne are of some importance. Also contributions of N, Na and Al are discussed

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Matteucci, F. "The Galactic Chemical Evolution of Lithium." Highlights of Astronomy 10 (1995): 457. http://dx.doi.org/10.1017/s1539299600011734.

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Under the assumption that the abundance of 7Li in Population II stars represents the primordial Li abundance (with perhaps a small contribution from GCR spallation) and that GCR spallation/fusion processes cannot contribute to more than ≃ 10 − 20% of the Li abundance observed in Pop. I stars and in the solar system, one must conclude that most of Li in Pop. I stars has a stellar origin.Possible stellar Li producers are discussed: low mass AGB stars (2−5M⊙) (C-stars), high mass AGB stars (5 - 8M⊙), supernovae of type II (M > 10M⊙) and novae. The various problems connected with all of these s

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