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Journal articles on the topic 'Nucleosynthesis'

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Author: Grafiati

Published: 4 June 2021

Last updated: 31 July 2024

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1

Sprouse, Trevor M., Kelsey A. Lund, Jonah M. Miller, Gail C. McLaughlin, and Matthew R. Mumpower. "Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk." Astrophysical Journal 962, no. 1 (February 1, 2024): 79. http://dx.doi.org/10.3847/1538-4357/ad1819.

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Abstract We simulate a black hole accretion disk system with full-transport general relativistic neutrino radiation magnetohydrodynamics for 1.2 s. This system is likely to form after the merger of two compact objects and is thought to be a robust site of r-process nucleosynthesis. We consider the case of a black hole accretion disk arising from the merger of two neutron stars. Our simulation time coincides with the nucleosynthesis timescale of the r-process (∼1 s). Because these simulations are time-consuming, it is common practice to run for a “short” duration of approximately 0.1–0.3 s. We analyze the nucleosynthetic outflow from this system and compare the results of stopping at 0.12 and 1.2 s. We find that the addition of mass ejected in the longer simulation as well as more favorable thermodynamic conditions from emergent viscous ejecta greatly impacts the nucleosynthetic outcome. We quantify the error in nucleosynthetic outcomes between short and long cuts.

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2

Yao, Xingqun, Motohiko Kusakabe, Toshitaka Kajino, Silvio Cherubini, Seiya Hayakawa, and Hidetoshi Yamaguchi. "Supernova Nucleosynthesis, Radioactive Nuclear Reactions and Neutrino-Mass Hierarchy." EPJ Web of Conferences 260 (2022): 01007. http://dx.doi.org/10.1051/epjconf/202226001007.

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The ν-process nucleosynthesis in core-collapse supernovae is a sensitive probe of unknown neutrino mass hierarchy through the MSW effect. We carefully studied the uncertainties of almost one hundred ν-induced and nuclear reactions associated with the nucleosynthesis and found that the ν-16O and 11C(α,p)14N reactions among them have the biggest effect on the final 7Li/11B isotopic abundance ratio. The neutrino mass hierarchy is constrained in our nucleosynthetic method with measured 7Li/11B value in SiC-X presolar grains. The inverted hierarchy is statistically more favored at the 2-σ C.L. [1].

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3

Ji, Alexander P., Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, et al. "Spectacular Nucleosynthesis from Early Massive Stars." Astrophysical Journal Letters 961, no. 2 (January 31, 2024): L41. http://dx.doi.org/10.3847/2041-8213/ad19c4.

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Abstract Stars that formed with an initial mass of over 50 M ⊙ are very rare today, but they are thought to be more common in the early Universe. The fates of those early, metal-poor, massive stars are highly uncertain. Most are expected to directly collapse to black holes, while some may explode as a result of rotationally powered engines or the pair-creation instability. We present the chemical abundances of J0931+0038, a nearby low-mass star identified in early follow-up of the SDSS-V Milky Way Mapper, which preserves the signature of unusual nucleosynthesis from a massive star in the early Universe. J0931+0038 has a relatively high metallicity ([Fe/H] = −1.76 ± 0.13) but an extreme odd–even abundance pattern, with some of the lowest known abundance ratios of [N/Fe], [Na/Fe], [K/Fe], [Sc/Fe], and [Ba/Fe]. The implication is that a majority of its metals originated in a single extremely metal-poor nucleosynthetic source. An extensive search through nucleosynthesis predictions finds a clear preference for progenitors with initial mass >50 M ⊙, making J0931+0038 one of the first observational constraints on nucleosynthesis in this mass range. However, the full abundance pattern is not matched by any models in the literature. J0931+0038 thus presents a challenge for the next generation of nucleosynthesis models and motivates the study of high-mass progenitor stars impacted by convection, rotation, jets, and/or binary companions. Though rare, more examples of unusual early nucleosynthesis in metal-poor stars should be found in upcoming large spectroscopic surveys.

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4

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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5

Mathews, G. J. "Nucleosynthesis and After: Supernovae and Nucleosynthesis." Science 274, no. 5291 (November 22, 1996): 1320b—1321b. http://dx.doi.org/10.1126/science.274.5291.1320b.

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6

KAJINO, TOSHITAKA, TAKAHIRO SASAQUI, TAKASHI YOSHIDA, and WAKO AOKI. "NEUTRINO OSCILLATION IN SUPERNOVA AND GRB NUCLEOSYNTHESIS." Modern Physics Letters A 23, no. 17n20 (June 28, 2008): 1409–18. http://dx.doi.org/10.1142/s0217732308027783.

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Neutrinos play the critical roles in nucleosyntheses of light-to-heavy mass elements in core-collapse supernovae (SNe). The light element synthesis is affected strongly by neutrino oscillations (MSW effect) through the ν-process in outer layers of supernova explosions. Specifically the 7 Li and 11 B yields increase by factors of 1.9 and 1.3 respectively in the case of large mixing angle solution, normal mass hierarchy, and sin 2 2θ13 = 2 × 10−3 compared to those without the oscillations. In the case of inverted mass hierarchy or nonadiabatic 13-mixing resonance, the increment of their yields is much smaller. We thus propose that precise constraint on mass hierarchy and sin 2 2θ13 is given by future observations of Li / B ratio or Li abundance in stars and presolar grains which are made from supernova ejecta. Gamma ray burst (GRB) nucleosynthesis in contrast is not affected strongly by thermal neutrinos from the central core which culminates in black hole (BH), although the effect of neutrinos from proto-neutron star prior to black hole formation is still unknown. We calculate GRB nucleosynthesis by turning off the thermal neutrinos and find that the abundance pattern is totally different from ordinary SN nucleosynthesis which satisfies the universality to the solar abundance pattern.

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7

Nie, Nicole X., Da Wang, Zachary A. Torrano, Richard W. Carlson, Conel M. O’D. Alexander, and Anat Shahar. "Meteorites have inherited nucleosynthetic anomalies of potassium-40 produced in supernovae." Science 379, no. 6630 (January 27, 2023): 372–76. http://dx.doi.org/10.1126/science.abn1783.

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Meteorites record processes that occurred before and during the formation of the Solar System in the form of nucleosynthetic anomalies: isotopic compositions that differ from the Solar System patterns. Nucleosynthetic anomalies are rarely seen in volatile elements such as potassium at bulk meteorite scale. We measured potassium isotope ratios in 32 meteorites and identified nucleosynthetic anomalies in the isotope potassium-40. The anomalies are larger and more variable in carbonaceous chondrite (CC) meteorites than in noncarbonaceous (NC) meteorites, indicating that CCs inherited more material produced in supernova nucleosynthesis. The potassium-40 anomaly of Earth is close to that of the NCs, implying that Earth’s potassium was mostly delivered by NCs.

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8

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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9

Coc, A. "Primordial Nucleosynthesis." Acta Physica Polonica B 44, no. 3 (2013): 521. http://dx.doi.org/10.5506/aphyspolb.44.521.

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10

Coc, Alain. "Primordial Nucleosynthesis." Journal of Physics: Conference Series 420 (March 25, 2013): 012136. http://dx.doi.org/10.1088/1742-6596/420/1/012136.

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11

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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12

Coc, A. "Primordial Nucleosynthesis." Journal of Physics: Conference Series 665 (January 5, 2016): 012001. http://dx.doi.org/10.1088/1742-6596/665/1/012001.

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13

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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14

Coc, Alain, and Elisabeth Vangioni. "Primordial nucleosynthesis." International Journal of Modern Physics E 26, no. 08 (August 2017): 1741002. http://dx.doi.org/10.1142/s0218301317410026.

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Primordial nucleosynthesis, or big bang nucleosynthesis (BBN), is one of the three evidences for the big bang model, together with the expansion of the universe and the cosmic microwave background. There is a good global agreement over a range of nine orders of magnitude between abundances of 4He, D, 3He and 7Li deduced from observations, and calculated in primordial nucleosynthesis. However, there remains a yet-unexplained discrepancy of a factor [Formula: see text], between the calculated and observed lithium primordial abundances, that has not been reduced, neither by recent nuclear physics experiments, nor by new observations. The precision in deuterium observations in cosmological clouds has recently improved dramatically, so that nuclear cross-sections involved in deuterium BBN needs to be known with similar precision. We will briefly discuss nuclear aspects related to the BBN of Li and D, BBN with nonstandard neutron sources, and finally, improved sensitivity studies using a Monte Carlo method that can be used in other sites of nucleosynthesis.

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15

Knödlseder, J. "Supernova Nucleosynthesis." EAS Publications Series 7 (2003): 177. http://dx.doi.org/10.1051/eas:2003041.

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16

Schramm, D. N. "Primordial nucleosynthesis." Proceedings of the National Academy of Sciences 95, no. 1 (January 6, 1998): 42–46. http://dx.doi.org/10.1073/pnas.95.1.42.

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17

Audouze, J. "Primordial Nucleosynthesis." Transactions of the International Astronomical Union 20, no. 1 (1988): 658–60. http://dx.doi.org/10.1017/s0251107x00007501.

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Primordial nucleosynthesis which is responsible for the formation of the lightest elements (D, 3He, 4HE and 7Li) might be as important as the overall expansion of the Universe and the cosmic background radiation to prove the occurrence of a dense and hot phase for the Unvierse about 15 billion years ago. As recalled in many reviews (e.g. refs. 1, 2) the standard Big Bang nucleosynthesis leads to two important conclusions regarding (i) a limitation of the baryonic density such that the corresponding cosmological parameter ΩB ≤ 0.1; (ii) a limitation of the number of neutrino flavours to 3-4 consistent with the results concerning the widths of the Z0 and W± particles3.

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18

Matzner, Richard A. "Cosmic nucleosynthesis." Publications of the Astronomical Society of the Pacific 98 (October 1986): 1049. http://dx.doi.org/10.1086/131871.

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19

Signore, Monique, and Denis Puy. "Primordial nucleosynthesis." New Astronomy Reviews 43, no. 2-4 (July 1999): 185–200. http://dx.doi.org/10.1016/s1387-6473(99)00011-1.

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20

Starrfield, S., J. W. Truran, M. Wiescher, and W. M. Sparks. "Nova nucleosynthesis." Nuclear Physics A 621, no. 1-2 (August 1997): 495–98. http://dx.doi.org/10.1016/s0375-9474(97)00296-0.

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21

Heger, A., E. Kolbe, W. C. Haxton, K. Langanke, G. Martínez-Pinedo, and S. E. Woosley. "Neutrino nucleosynthesis." Physics Letters B 606, no. 3-4 (January 2005): 258–64. http://dx.doi.org/10.1016/j.physletb.2004.12.017.

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22

Scherrer, R. J. "Primordial nucleosynthesis." Astronomical & Astrophysical Transactions 19, no. 3-4 (December 2000): 367–73. http://dx.doi.org/10.1080/10556790008238583.

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23

Mishinsky, Gennady V., Vladimir D. Kuznetsov, and Victor I. Starostin. "Natural Nucleosynthesis." Radioelectronics. Nanosystems. Information Technologies. 14, no. 4 (December 29, 2022): 473–96. http://dx.doi.org/10.17725/rensit.2022.14.473.

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The possibility of generating strong and ultrastrong magnetic fields in condensed ionized media in the presence of unidirectional motion of an ensemble of free electrons with a density > 1021 e/cm3 is demonstrated. It is shown that atomic and nuclear matter in strong and ultrastrong magnetic fields is transformed into a new state of matter - into transatom, in which atomic electrons and nuclear protons and neutrons are bound in pairs into orthobosons with a spin equal to unity S = 1ћ. Examples of radiationless, low-energy nuclear reactions of transatoms, including those without the Coulomb barrier between identical atomic nuclei, are presented. The mechanism of natural nucleosynthesis, based on the results of the low-energy nuclear reactions registered in various experiments in many laboratories of the world and on the creation of the theory of those reactions, at different stages of the development of the Universe, stars and planets is presented.

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24

Maciel, W. J., R. D. D. Costa, and T. E. P. Idiart. "Helium abundances in planetary nebulae: Nucleosynthesis and chemical evolution." Proceedings of the International Astronomical Union 5, S268 (November 2009): 181–82. http://dx.doi.org/10.1017/s1743921310004084.

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AbstractWe have obtained a large sample of PN with accurately determined helium abundances, as well as abundances of several heavy elements. The nebulae are located in the solar neighbourhood, in the galactic bulge, disk and anticentre, and in the Magellanic Clouds. The abundances are analyzed both in terms of the nucleosynthesis of intermediate mass stars and the chemical evolution of the host galaxies. In particular, correlations between the He/H ratio and the abundances of N and O are used as constraints of the nucleosynthetic processes occurring in the progenitor stars.

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25

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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26

Kurki-Suonio, Hannu. "Alternative Solutions to Big Bang Nucleosynthesis." Symposium - International Astronomical Union 198 (2000): 25–34. http://dx.doi.org/10.1017/s0074180900166367.

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Standard big bang nucleosynthesis (SBBN) has been remarkably successful, and it may well be the correct and sufficient account of what happened. However, interest in variations from the standard picture come from two sources: First, big bang nucleosynthesis can be used to constrain physics of the early universe. Second, there may be some discrepancy between predictions of SBBN and observations of abundances. Various alternatives to SBBN include inhomogeneous nucleosynthesis, nucleosynthesis with antimatter, and nonstandard neutrino physics.

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27

Kamath, Devika, and Hans Van Winckel. "Post-AGB Stars as Tracers of AGB Nucleosynthesis: An Update." Universe 8, no. 4 (April 11, 2022): 233. http://dx.doi.org/10.3390/universe8040233.

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The chemical evolution of galaxies is governed by the chemical yields from stars, and here we focus on the important contributions from asymptotic giant branch (AGB) stars. AGB nucleosynthesis is, however, still riddled with complexities. Observations from post-asymptotic giant branch (post-AGB) stars serve as exquisite tools to quantify and understand AGB nucleosynthesis. In this contribution, we review the invaluable constraints provided by post-AGB stars with which to study AGB nucleosynthesis, especially the slow neutron capture nucleosynthesis (i.e., the s-process).

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28

CHEOUN, Myung-Ki, and Dukjae JANG. "Big Bang Nucleosynthesis." Physics and High Technology 26, no. 4 (April 30, 2017): 22–27. http://dx.doi.org/10.3938/phit.26.015.

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29

Horowitz, C. J., and Gang Li. "Nucleosynthesis in Supernovae." Physical Review Letters 82, no. 26 (June 28, 1999): 5198–201. http://dx.doi.org/10.1103/physrevlett.82.5198.

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30

El Eid, Mounib F. "Heavy Element Nucleosynthesis." EPJ Web of Conferences 184 (2018): 01007. http://dx.doi.org/10.1051/epjconf/201818401007.

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This contribution deals with the important subject of the nucleosynthesis of heavy elements in the Galaxy. After an overview of several observational features, the physical processes responsible mainly for the formation of heavy elements will be described and linked to possible stellar sites and to galactic chemical evolution. In particular, we focus on the neutron-capture processes, namely the s-process (slow neutron capture) and the r-process (rapid neutron capture) and discuss some problems in connection with their sites and their outcome. The aim is to give a brief overview on the exciting subject of the heavy element nucleosynthesis in the Galaxy, emphasizing its importance to trace the galactic chemical evolution and illustrating the challenge of this subject.

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31

Clayton, Donald D. "Studies of nucleosynthesis." Nature 332, no. 6166 (April 1988): 683–84. http://dx.doi.org/10.1038/332683a0.

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32

Riley, S. P., and J. M. Irvine. "Primordial nucleosynthesis revisited." Journal of Physics G: Nuclear and Particle Physics 17, no. 1 (January 1, 1991): 35–48. http://dx.doi.org/10.1088/0954-3899/17/1/003.

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33

Walker, Terry P., Gary Steigman, Ho-Shik Kang, David M. Schramm, and Keith A. Olive. "Primordial nucleosynthesis redux." Astrophysical Journal 376 (July 1991): 51. http://dx.doi.org/10.1086/170255.

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34

Boyd, Richard N. "Big bang nucleosynthesis." Nuclear Physics A 693, no. 1-2 (October 2001): 249–57. http://dx.doi.org/10.1016/s0375-9474(00)00707-7.

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35

Mukhanov, V. "Nucleosynthesis Without Computer." International Journal of Theoretical Physics 43, no. 3 (March 2004): 669–93. http://dx.doi.org/10.1023/b:ijtp.0000048169.69609.77.

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36

Olive, Keith A. "Big bang nucleosynthesis." Nuclear Physics B - Proceedings Supplements 70, no. 1-3 (January 1999): 521–28. http://dx.doi.org/10.1016/s0920-5632(98)00488-5.

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37

Olive, Keith A. "Big bang nucleosynthesis." Nuclear Physics B - Proceedings Supplements 80, no. 1-3 (January 2000): 79–93. http://dx.doi.org/10.1016/s0920-5632(99)00831-2.

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38

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 potential systematic error in 4He abundance determinations remains open). The remarkable success of the theory to date in establishing the concordance has led to the very robust conclusion of BBN regarding the baryon density. The BBN constraints on the cosmological baryon density are reviewed and demonstrate that the bulk of the baryons are dark and also that the bulk of the matter in the universe is non-baryonic. Comparison of baryonic density arguments from Lyman-α clouds, x-ray gas in clusters, the Sunyaev-Zeldovich effect, and the microwave anisotropy are made and shown to be consistent with the BBN value.

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39

Tytler, David, John M. O'Meara, Nao Suzuki, and Dan Lubin. "Big Bang Nucleosynthesis." Nuclear Physics B - Proceedings Supplements 87, no. 1-3 (June 2000): 464–73. http://dx.doi.org/10.1016/s0920-5632(00)00721-0.

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40

Dolgov, A. D. "Big Bang Nucleosynthesis." Nuclear Physics B - Proceedings Supplements 110 (July 2002): 137–43. http://dx.doi.org/10.1016/s0920-5632(02)01470-6.

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41

Dolgov, A. "Big Bang Nucleosynthesis." Nuclear Physics B - Proceedings Supplements 110, no. 2 (July 2002): 137–43. http://dx.doi.org/10.1016/s0920-5632(02)80113-x.

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42

Fields, Brian D., and Keith A. Olive. "Big bang nucleosynthesis." Nuclear Physics A 777 (October 2006): 208–25. http://dx.doi.org/10.1016/j.nuclphysa.2004.10.033.

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43

Bravo, E., J. Isern, R. Canal, and J. Labay. "Nucleosynthesis in SNIa." Astrophysics and Space Science 169, no. 1-2 (July 1990): 19–24. http://dx.doi.org/10.1007/bf00640679.

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44

Cassé, Michel. "Nucleosynthesis of 26Al." Advances in Space Research 6, no. 4 (January 1986): 139–44. http://dx.doi.org/10.1016/0273-1177(86)90252-8.

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45

Meyer, Bradley S. "Entropy and nucleosynthesis." Physics Reports 227, no. 1-5 (May 1993): 257–67. http://dx.doi.org/10.1016/0370-1573(93)90071-k.

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46

Arnett, David. "Explosive nucleosynthesis: prospects." Physics Reports 333-334 (August 2000): 109–20. http://dx.doi.org/10.1016/s0370-1573(00)00018-1.

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47

Olive, K. A. "Big-bang nucleosynthesis." European Physical Journal C 15, no. 1-4 (March 2000): 133–35. http://dx.doi.org/10.1007/bf02683412.

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48

Steigman, Gary. "Big bang nucleosynthesis." Nuclear Physics B - Proceedings Supplements 37, no. 3 (January 1995): 68–73. http://dx.doi.org/10.1016/0920-5632(94)00790-3.

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49

Steigman, Gary. "Big Bang nucleosynthesis." Nuclear Physics B - Proceedings Supplements 48, no. 1-3 (May 1996): 499–507. http://dx.doi.org/10.1016/0920-5632(96)00303-9.

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50

Oberhummer, H., H. Herndl, T. Rauscher, and H. Beer. "Neutron-induced nucleosynthesis." Surveys in Geophysics 17, no. 6 (November 1996): 665–702. http://dx.doi.org/10.1007/bf01931785.

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