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s-process Heavy-element Nucleosynthesis in Low-mass Rotating AGB Stars 认领 引用
1
作者 Xin-Yue Qu Han-Feng Song +4 位作者 Rui-Yu Zhang Ying Qin Shi-Tao Qi Zhuo Han Wen-Li Zhong 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第7期205-214,共10页
While the qualitative aspects of the slow neutron-capture process(s-process)are understood,its quantitative treatment in stellar evolution models remains a major source of uncertainty.Rotation’s role in stellar struc... While the qualitative aspects of the slow neutron-capture process(s-process)are understood,its quantitative treatment in stellar evolution models remains a major source of uncertainty.Rotation’s role in stellar structure,mixing,and s-process nucleosynthesis is actively being researched,with recent studies showing it can significantly influence s-process yields,but the precise effects and uncertainties in these models still require further investigation.To study the impact of rotation on the s-process,we implemented an extended and flexible reaction network within the Geneva Stellar Evolution Code.Rotation exerts a dual influence:first,it modifies the stellar structure equations to include centrifugal forces,which provide structural support and consequently lower central temperatures but high densities.Second,rotation increases helium core size and central temperature,enhancing s-process efficiency.The emergence of shear instabilities represents a significant rotational effect impacting s-process nucleosynthesis.Rotationally driven mixing transports 12C beyond the core into proton-rich radiative zones.These regions enable efficient 12C(p,)13N(+)13C reactions.Subsequent beta-decay 13N(+)13C yields gradual 13C accumulation reaching mass fractions of∼0.1%.Rotationally induced mixing returns portions of this 13C to the core,while outward core expansion slowly ingests additional 13C.Upon entering the convective region,13C advects inward to higher-temperature zones,where rapid burning occurs via 13C(α,n)16O with abundant helium,producing neutrons.Therefore,rotationally induced mixing boosts s-process nucleosynthesis. 展开更多
关键词 stars:rotation nuclear reactions,nucleosynthesis,abundances stars:evolution stars:AGB and post AGB
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Nucleosynthesis in Advection-Dominated Accretion Flow onto a Black Hole 认领 引用
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作者 Jiang Zhang Ren-Yi Ma +1 位作者 Hong-Jie Li Bo Zhang 《Chinese Physics Letters》 SCIE EI CAS CSCD 2017年第4期128-131,共4页
Nucleosynthesis in advection-dominated accretion flow （ADAF） onto a black hole is proposed to be an important role in chemical evolution around compact stars. We investigate the nucleosynthesis in ADAF relevant for ... Nucleosynthesis in advection-dominated accretion flow （ADAF） onto a black hole is proposed to be an important role in chemical evolution around compact stars. We investigate the nucleosynthesis in ADAF relevant for a black hole of low mass, different from that of the self-similar solution. In particular, the presence of supersolar metal mass fractions of some isotopes seems to be associated with the known black hole nucleosynthesis in ADAF, which offers further evidence of diversity of the chemical enrichment. 展开更多
关键词 Nucleosynthesis in Advection-Dominated Accretion Flow onto a Black Hole
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Study of primordial deuterium abundance in Big Bang nucleosynthesis 认领 引用 被引量：4
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作者 Zhi-Lin Shen Jian-Jun He 《Nuclear Science and Techniques》 SCIE EI CAS CSCD 2024年第3期208-215,共8页
Big Bang nucleosynthesis(BBN)theory predicts the primordial abundances of the light elements2 H(referred to as deuterium,or D for short),3He,4He,and7 Li produced in the early universe.Among these,deuterium... Big Bang nucleosynthesis(BBN)theory predicts the primordial abundances of the light elements2 H(referred to as deuterium,or D for short),3He,4He,and7 Li produced in the early universe.Among these,deuterium,the first nuclide produced by BBN,is a key primordial material for subsequent reactions.To date,the uncertainty in predicted deuterium abundance(D/H)remains larger than the observational precision.In this study,the Monte Carlo simulation code PRIMAT was used to investigate the sensitivity of 11 important BBN reactions to deuterium abundance.We found that the reaction rate uncertainties of the four reactions d(d,n)3He,d(d,p)t,d(p,γ)3He,and p(n,γ)d had the largest influence on the calculated D/H uncertainty.Currently,the calculated D/H uncertainty cannot reach observational precision even with the recent LUNA precise d(p,γ)3 He rate.From the nuclear physics aspect,there is still room to largely reduce the reaction-rate uncertainties;hence,further measurements of the important reactions involved in BBN are still necessary.A photodisintegration experiment will be conducted at the Shanghai Laser Electron Gamma Source Facility to precisely study the deuterium production reaction of p(n,γ)d. 展开更多
关键词 Big Bang nucleosynthesis Abundance of deuterium Reaction cross section Reaction rate Monte Carlo method
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Big Bang Nucleosynthesis in Carmeli Cosmology—Mass Density, Temperature and Expansion Rate of the Early Universe 认领 引用
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作者 Firmin J. Oliveira 《Journal of High Energy Physics, Gravitation and Cosmology》 CAS 2021年第1期333-343,共11页
The Carmeli Cosmological Special Relativity theory (CSR) is used to study the universe at early times after the big bang. The universe temperature vs. time relation is developed from the mass density relation. It is s... The Carmeli Cosmological Special Relativity theory (CSR) is used to study the universe at early times after the big bang. The universe temperature vs. time relation is developed from the mass density relation. It is shown that CSR is well suited to analyze the nucleosynthesis of the light elements up to beryllium, equivalent to the standard model. 展开更多
关键词 Big Bang Nucleosynthesis Carmeli Cosmology Nucleosynthesis
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Nucleosynthesis in the accretion disks of Type Ⅱ collapsars 认领 引用
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作者 Indrani Banerjee Banibrata Mukhopadhyay 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2013年第9期1063-1074,共12页
We investigate nucleosynthesis inside the gamma-ray burst （GRB） accre- tion disks formed by the Type II collapsars. In these collapsars, the core collapse of massive stars first leads to the formation of a proto-neu... We investigate nucleosynthesis inside the gamma-ray burst （GRB） accre- tion disks formed by the Type II collapsars. In these collapsars, the core collapse of massive stars first leads to the formation of a proto-neutron star. After that, an out- ward moving shock triggers a successful supernova. However, the supernova ejecta lacks momentum and within a few seconds the newly formed neutron star gets trans- formed to a stellar mass black hole via massive fallback. The hydrodynamics of such an accretion disk formed from the fallback material of the supernova ejecta has been studied extensively in the past. We use these well-established hydrodynamic models for our accretion disk in order to understand nucleosynthesis, which is mainly ad- vection dominated in the outer regions. Neutrino cooling becomes important in the inner disk where the temperature and density are higher. The higher the accretion rate （M） is, the higher the density and temperature are in the disks. We deal with accre- tion disks with relatively low accretion rates： 0.001 Mo s-1 ~ 3）/~ 0.01 Mo S--1 and hence these disks are predominantly advection dominated. We use He-rich and Si- rich abundances as the initial condition of nucleosynthesis at the outer disk, and being equipped with the disk hydrodynamics and the nuclear network code, we study the abundance evolution as matter inflows and falls into the central object. We investigate the variation in the nucleosynthesis products in the disk with the change in the initial abundance at the outer disk and also with the change in the mass accretion rate. We report the synthesis of several unusual nuclei like 31p, 39K, 43Sc＇ 35C1 and various isotopes of titanium, vanadium, chromium, manganese and copper. We also confirm that isotopes of iron, cobalt, nickel, argon, calcium, sulphur and silicon get synthe- sized in the disk, as shown by previous authors. Much of these heavy elements thus synthesized are ejected from the disk via outflows and hence they should leave their signature in observed data. 展开更多
关键词 accretion accretion disks -- gamma rays： bursts -- black hole physics-- nuclear reactions nucleosynthesis abundances
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The Origin of Cosmic Structures Part 4—Nucleosynthesis 认领 引用 被引量：3
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作者 J. C. Botke 《Journal of High Energy Physics, Gravitation and Cosmology》 CAS 2022年第3期768-799,共32页
In our original paper, we outlined a new model of nucleosynthesis which began when a small percentage of the vacuum energy was converted primarily into neutron-antineutron pairs but with a very small excess of neutron... In our original paper, we outlined a new model of nucleosynthesis which began when a small percentage of the vacuum energy was converted primarily into neutron-antineutron pairs but with a very small excess of neutrons. In this paper, we present a detailed study of that original idea. We show that immediately after their inception, annihilation and charge exchange reactions proceeded at a very high rate and after an interval of no more than 10-12 s, the matter/antimatter asymmetry of the universe and the present-day abundance of baryons had been established. The annihilations produced the high density of leptons critical for the weak interactions and the photons that make up the CMB. The model predicts a photon temperature in agreement with the present-day CMB value and also explains the origin of the CMB anisotropy spectrum. We also show how the nucleosynthesis density variations needed to explain all cosmic structures can resolve the difficulties that arise when trying to explain observed primordial element abundances in terms of a single-density universal model of nucleosynthesis. 展开更多
关键词 Nucleosynthesis Early Universe Time-Varying Curvature
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Nucleosynthesis in Hot and Dense Media 认领 引用 被引量：1
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作者 Samina S. Masood 《Journal of Modern Physics》 2014年第5期296-308,共13页
We study the finite temperature and density effects on beta decay rates to compute their contributions to nucleosynthesis. QED type corrections to beta decay from the hot and dense background are estimated in terms of... We study the finite temperature and density effects on beta decay rates to compute their contributions to nucleosynthesis. QED type corrections to beta decay from the hot and dense background are estimated in terms of the statistical corrections to the self-mass of an electron. For this purpose, we re-examine the hot and dense background contributions to the electron mass and compute its effect to the beta decay rate, helium yield, energy density of the universe as well as the change in neutrino temperature from the first order contribution to the self-mass of electrons during these processes. We explicitly show that the thermal contribution to the helium abundance at T = m of a cooling universe (0.045 percent) is higher than the corresponding contribution to helium abundance of a heating universe (0.031 percent) due to the existence of hot fermions before the beginning of nucleosynthesis and their absence after the nucleosynthesis, in the early universe. Thermal contribution to helium abundance was a simple quadratic function of temperature, before and after the nucleosynthesis. However, this quadratic behavior was not the same before the decoupling temperature due to weak interactions;so the nucleosynthesis did not even start before the universe had cooled down to the neutrino decoupling temperatures and QED became a dominant theory in the presence of a high concentration of charged fermions. It is also explicitly shown that the chemical potential in the core of supermassive and superdense stars affect beta decay and their helium abundance but the background contributions depend on the ratio between temperature and chemical potential and not the chemical potential or temperature only. We calculate the hot and dense background contributions for m = T = μ. It has been noticed that temperature plays a role in regulating parameter in an extremely dense systems. Therefore, for extremely dense systems, temperature has to be large enough to get the expected value of helium production in the stellar cores. 展开更多
关键词 Nucleosynthesis Beta Decay Compact Stars Hot and Dense Media
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Impact of mass uncertainties of 83,84Mo,82Nb and 80Zr on the rp-process nucleosynthesis 认领 引用
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作者 Jia-Hao Lv Yuan-Ming Xing +1 位作者 Meng Wang Yu-Hu Zhang 《Chinese Physics C》 SCIE CAS CSCD 2026年第8期265-268,共4页
Precise nuclear mass values are key parameters for modeling astrophysical X-ray bursts.In this work,we investigate the impact of current mass uncertainties of 83,84Mo,82Nb,and 80Zr on the nucleosynthesis of t... Precise nuclear mass values are key parameters for modeling astrophysical X-ray bursts.In this work,we investigate the impact of current mass uncertainties of 83,84Mo,82Nb,and 80Zr on the nucleosynthesis of the rp-process.The results reveal that the impact of the mass uncertainties of 83,84Mo and 80Zr on the final abundances is negligible,although the large mass uncertainty of 83Mo can reach a level close to 1 MeV.In contrast,the final abundances are highly sensitive to the mass value of 82Nb.An increase in the mass of 82Nb can significantly enhance the abundance at A=81.Furthermore,the Zr-Nb cycle in the rp-process is investigated and confirmed to play a minor role in the rp-process flows. 展开更多
关键词 abundances nucleosynthesis X-ray burst(XRB) mass excess
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Constraining explosive nucleosynthesis by indirect reaction methods at storage rings using unstable beams in batch mode 认领 引用
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作者 G.de Angelis F.Recchia +53 位作者 J.Glorius J.Gerl B.Jurado Xiao-Lin Tu Jian-Ling Lou S.Carollo C.Berthelot N.Watwood B.P.Kay P.Aguilera M.L.Avila J.Benito Garcia K.Bhatt D.Brugnara K.A.Chipps A.Couture A.Demerdjiev G.D.Dimitrova S.Dutta A.Ertoprak R.Escudeiro S.J.Freeman F.Galtarossa E.Geleva B.Gongora Servin A.Gottardo A.Hall-Smith J.Henderson C.Hoffman R.O.Hughes H.Jayatissa M.La Commara G.Leckenby S.M.Lenzi D.Mengoni M.R.Mumpower W.J.Ong M.Paul J.Pellumaj C.Domingo-Pardo R.M.Perez Vidal S.Pigliapoco A.Ratkiewicz K.Rezynkina S.Rocca D.K.Sharp Yang Sun T.L.Tang D.Tonev I.A.Tolstukhin G.Wendell Misch M.Williams B.Wloch Fan-Fei Zeng 《Chinese Physics C》 SCIE CAS CSCD 2025年第9期148-152,共5页
Nuclear reaction studies on unstable isotopes can strongly help in improving our understanding of nucleosynthesis in stars.Indirect approaches to determining astrophysical reaction rates are increasingly common-place ... Nuclear reaction studies on unstable isotopes can strongly help in improving our understanding of nucleosynthesis in stars.Indirect approaches to determining astrophysical reaction rates are increasingly common-place and undergoing continuous refinement.Of particular interest is the use of such indirect techniques at storage rings,which,among other aspects,allow to recycle rare unstable beams.We propose to investigate the reaction rates of astrophysical interest using indirect methods(surrogate,Trojan horse,etc.)in reverse kinematics at the IMP-CAS storage ring.Long lived radioactive ion beams,produced remotely,can be accelerated,and made to interact with light targets.The proposed reactions are85Kr(p,p’γ),85Kr(d,pγ),constraining the neutron flux in an s-process branching point,79Se(p,p’γ),79Se(d,pγ),constraining the temperature in s-process nucleosyntheses,and59Fe(d,pγ),constraining core collapse supernovae. 展开更多
关键词 storage ringswhichamong indirect methods surrogatetrojan horsee storage rings indirect reaction methods improving our understanding nucleosynthesis unstable beams nuclear reaction studies unstable isotopes recycle rare unstable beamswe
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Implication of radioactive nuclear reaction 11C(α,p)14N in Supernovaν-process nucleosynthesis 认领 引用
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作者 Xingqun Yao Yudong Luo +5 位作者 Toshitaka Kajino Seiya Hayakawa Hidetoshi Yamaguchi Xiaodong Tang Bingshui Gao Fulong Liu 《Chinese Physics C》 SCIE CAS CSCD 2025年第8期159-170,共12页
The origin of boron in the solar system has not yet been clearly understood.We studied the light mass nuclear reactions and neutrino-induced reactions that play important roles in the nucleosynthesis of A=11 nuclei in... The origin of boron in the solar system has not yet been clearly understood.We studied the light mass nuclear reactions and neutrino-induced reactions that play important roles in the nucleosynthesis of A=11 nuclei in the core-collapse supernova(CCSN).We found that the production of A=11 nuclei,particularly11C,is sensitive to the radioactive nuclear reaction11C(α,p)14N among many others.We calculated the upper and lower limits of the11C(α,p)14N rate by taking account of the low energy resonances above the threshold,which have not been included in the previous SN nucleosynthesis calculations.These resonance contributions significantly change the11C abundance,which decays to11B with a half-life of 20.34 m,and affects the resultant isotopic abundance ratio of11B/10B at Mr=3.78-4.4M⊙from which the presolar X grains could form.The11B/10B isotopic ratio measured in X grains can help to understand the origin of solar system boron and constrain still unknown neutrino mass hierarchy if the observational and theoretical uncertainties associated with these abundances are reduced.We emphasize that the further precise experiment of measuring the11C(α,p)14N reaction cross sections at the astrophysically interesting energies of Gamow window 0.23-1.24 MeV,which corresponds to the effective temperature T=0.2-1 GK,could clarify CCSN contribution to the solar11B/10B ratio. 展开更多
关键词 Core-collapse supernova explosive nucleosynthesis reaction rates nuclear physics
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The impact of new(α,n)reaction rates on the weak s‑process in metal‑poor massive stars 认领 引用
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作者 Wen‑Yu Xin Chun‑Ming Yip +2 位作者 Ken’ichi Nomoto Xian‑Fei Zhang Shao‑Lan Bi 《Nuclear Science and Techniques》 SCIE EI CAS CSCD 2026年第8期216-232,共17页
Massive stars are significant sites for the weak s-process(ws-process).In metal-rich stars,22Ne and16O are,respectively,the main neutron source and poison for the ws-process.In metal-poor stars,however,the abund... Massive stars are significant sites for the weak s-process(ws-process).In metal-rich stars,22Ne and16O are,respectively,the main neutron source and poison for the ws-process.In metal-poor stars,however,the abundance of 22Ne is limited by metallicity,so the contribution of 22Ne(α,n)25Mg reaction on the s-process is smaller.Conversely,the 17O(α,n)20Ne reaction becomes more prominent in these stars because of the most abundant 16O at all metallicities.In this study,we calculated the evolution of four metal-poor stars(Z=10-3)for the zero-age main-sequence(ZAMS)masses of M(ZAMS)=15,20,25,and30 M⊙to investigate the effect of reaction rates on the ws-process.We adopt the new 17O(α,n)20Ne and 17O(α,γ)21Ne reaction rates suggested by Best et al.(2013)and 22Ne(α,n)25Mg and 22Ne(α,γ)26Mg reaction rates from Wiescher et al.(2023).The yields of the s-process isotopes with the updated reaction rates are compared with the results using the default reaction rates from JINA REACLIB.We found that the new 17O+αreaction rates enhance the ws-process in all stages,whereas the new 22Ne+αreaction rates enhance the ws-process only in the C and Ne burning stages.Updating these new reaction rates would increase the production of ws-process isotopes by tens of times.We also note that for more massive stars,the enhancement by the new 17O+αreaction rates becomes more significant. 展开更多
关键词 Massive stars Supernovae S-process Nuclear reactions Nucleosynthesis
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In-Target Energy Loss Compensation for Nuclear Astrophysical Studies 认领 引用
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作者 Huangkai Wu Kai Zhao +11 位作者 Youjing Wang Yixin Li Yisong Zhou Ding Yue Zhengkun Li Jize Tan Lisong Bai Weiping Liu Bing Guo Changbo Fu Guoqiang Zhang Yu-Gang Ma 《Chinese Physics Letters》 SCIE EI CAS CSCD 2026年第3期1-9,共9页
Measuring cross sections of nuclear reactions,such as the so-called“Holy Grail”reaction,12C(σ,γ)16O,is essential for understanding stellar nucleosynthesis but presents significant challenges due to extremely... Measuring cross sections of nuclear reactions,such as the so-called“Holy Grail”reaction,12C(σ,γ)16O,is essential for understanding stellar nucleosynthesis but presents significant challenges due to extremely low cross sections.Key challenges include significant energy loss as ions penetrate the target material,limiting measurements to thin target layers.To overcome these obstacles,we propose a novel method,the in-target energy loss compensating(eLOC)method,specifically designed for gas targets,which utilizes a gas-filled magnetic field and accelerating electric fields to compensate for ion energy loss in the target.Simulations show that this approach significantly enhances the effective target thickness by over 140 times in the case of the“Holy Grail”reaction with an inverse-kinematics setup.This eLOC method may provide a powerful new tool for obtaining critical data in nuclear astrophysics,thereby advancing our understanding of stellar nucleosynthesis and the origins of elements in the universe,as well as benefiting other related fields such as isotope production. 展开更多
关键词 measuring cross sections nuclear astrophysics gas targets understanding stellar nucleosynthesis magnetic field target materiallimiting target energy loss compensation gas targetswhich
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Constraints on the 12C(α,γ)16Oand16O+16OReaction Rates from Binary Black Holes Detected via Gravitational Wave Signals 认领 引用
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作者 Wenyu Xin Xiaokun Hou +2 位作者 Xianfei Zhang Shaolan Bi Gang Zhao 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第7期139-146,共8页
Gravitational-wave observations of binary black hole(BH)mergers provide a novel avenue for testing massivestar evolution and the resulting BH mass spectrum.Recent population analyses under the hierarchical-merger hypo... Gravitational-wave observations of binary black hole(BH)mergers provide a novel avenue for testing massivestar evolution and the resulting BH mass spectrum.Recent population analyses under the hierarchical-merger hypothesis have provided evidence for the BH mass gap and inferred its lower edge to∼44–68M⊙.Motivated by these findings,we compute low-metallicity(Z=10−5)helium star models with MESA and systematically explore the effect of uncertainties in the 12C(α,γ)16O and 16O+16O reaction rates on the final fate of these massive stars.Varying the 12C(α,γ)16O reaction rate from−3σto+3σ,we find that the predicted BH mass gap shifts from∼104–184 M⊙to∼45–135 M⊙.In contrast,scaling the 16O+16O reaction rate by global factors of 0.1,1,and 10 has only a modest effect on the lower edge of the BH mass gap(less than 5 M⊙),and shifts the upper edge by more than 10 M⊙.Using the predictions of our models together with the literature estimates for the lower edge of the BH mass gap,we constrain the astrophysical S factor of 12C(α,γ)16O reaction at 300 keV of S300≃137.6–263.4 keV barn. 展开更多
关键词 stars:black holes (stars:)supernovae:general nuclear reactions,nucleosynthesis,abundances
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Toward precision mass measurements of neutron-rich nuclei relevant to r-process nucleosynthesis 认领 引用 被引量：9
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作者 B. H. Sun Yu. A. Litvinov +1 位作者 I. Tanihata Y. H. Zhang 《Frontiers of physics》 SCIE CSCD 2015年第4期1-25,共25页
The open question of where, when, and how the heavy elements beyond iron enrich our Universe has triggered a new era in nuclear physics studies. Of all the relevant nuclear physics inputs, the mass of very neutron-ric... The open question of where, when, and how the heavy elements beyond iron enrich our Universe has triggered a new era in nuclear physics studies. Of all the relevant nuclear physics inputs, the mass of very neutron-rich nuclides is a key quantity for revealing the origin of heavy elements beyond iron. Although the precise determination of this property is a great challenge, enormous progress has been made in recent decades, and it has contributed significantly to both nuclear structure and astrophysical nucleosynthesis studies. In this review, we first survey our present knowledge of the nuclear mass surface, emphasizing the importance of nuclear mass precision in r-process calculations. We then discuss recent progress in various methods of nuclear mass measurement with a few selected examples. For each method, we focus on recent breakthroughs and discuss possible ways of improving the weighing of r-process nuclides. 展开更多
关键词 binding energy r-process nucleosynthesis nuclear mass spectrometry
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BIG-BANG NUCLEOSYNTHESIS 认领 引用 被引量：1
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作者 K.A.Olive K.Agashe +208 位作者 C.Amsler M.Antonelli J.-F.Arguin D.M.Asner H.Baer H.R.Band R.M.Barnett T.Basaglia C.W.Bauer J.J.Beatty V.I.Belousov J.Beringer G.Bernardi S.Bethke H.Bichsel O.Biebe E.Blucher S.Blusk G.Brooijmans O.Buchmueller V.Burkert M.A.Bychkov R.N.Cahn M.Carena A.Ceccucci A.Cerr D.Chakraborty M.-C.Chen R.S.Chivukula K.Copic G.Cowan O.Dahl G.D'Ambrosio T.Damour D.de Florian A.de Gouvea T.DeGrand P.de Jong G.Dissertor B.A.Dobrescu M.Doser M.Drees H.K.Dreiner D.A.Edwards S.Eidelman J.Erler V.V.Ezhela W.Fetscher B.D.Fields B.Foster A.Freitas T.K.Gaisser H.Gallagher L.Garren H.-J.Gerber G.Gerbier T.Gershon T.Gherghetta S.Golwala M.Goodman C.Grab A.V.Gritsan C.Grojean D.E.Groom M.Grnewald A.Gurtu T.Gutsche H.E.Haber K.Hagiwara C.Hanhart S.Hashimoto Y.Hayato K.G.Hayes M.Heffner B.Heltsley J.J.Hernandez-Rey K.Hikasa A.Hocker J.Holder A.Holtkamp J.Huston J.D.Jackson K.F.Johnson T.Junk M.Kado D.Karlen U.F.Katz S.R.Klein E.Klempt R.V.Kowalewski F.Krauss M.Kreps B.Krusche Yu.V.Kuyanov Y.Kwon O.Lahav J.Laiho P.Langacker A.Liddle Z.Ligeti C.-J.Lin T.M.Liss L.Littenberg K.S.Lugovsky S.B.Lugovsky F.Maltoni T.Mannel A.V.Manohar W.J.Marciano A.D.Martin A.Masoni J.Matthews D.Milstead P.Molaro K.Monig F.Moortgat M.J.Mortonson H.Murayama K.Nakamura M.Narain P.Nason S.Navas M.Neubert P.Nevski Y.Nir L.Pape J.Parsons C.Patrignani J.A.Peacock M.Pennington S.T.Petcov Kavli IPMU A.Piepke A.Pomarol A.Quadt S.Raby J.Rademacker G.Raffel B.N.Ratcliff P.Richardson A.Ringwald S.Roesler S.Rolli A.Romaniouk L.J.Rosenberg J L.Rosner G.Rybka C.T.Sachrajda Y.Sakai G.P.Salam S.Sarkar F.Sauli O.Schneider K.Scholberg D.Scott V.Sharma S.R.Sharpe M.Silari T.Sjostrand P.Skands J.G.Smith G.F.Smoot S.Spanier H.Spieler C.Spiering A.Stahl T.Stanev S.L.Stone T.Sumiyoshi M.J.Syphers F.Takahashi M.Tanabashi J.Terning L.Tiator M.Titov N.P.Tkachenko N.A.Tornqvist D.Tovey G.Valencia G.Venanzoni M.G.Vincter P.Vogel A.Vogt S.P.Wakely W.Walkowiak C.W.Walter D.R.Ward G.Weiglein D.H.Weinberg E.J.Weinberg M.White L.R.Wiencke C.G.Wohl L.Wolfenstein J.Womersley C.L.Woody R.L.Workman A.Yamamoto W.-M.Yao G.P.Zeller O.V.Zenin J.Zhang R.-Y.Zhu F.Zimmermann P.A.Zyla G.Harper V.S.Lugovsky P.Schaffner 《Chinese Physics C》 SCIE EI CAS CSCD 2014年第9期339-344,共6页
Revised October 2013 by B.D. Fields, （Univ. of Illinois） P. Molaro （Trieste Observatory） and S. Sarkar （Univ. of Oxford ＆ Niels Bohr Institute, Copenhagen）.
关键词 BBN BIG-BANG NUCLEOSYNTHESIS Rev
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Impact of the new 12C+12C reaction rate on presupernova nucleosynthesis 认领 引用 被引量：2
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作者 辛文宇 野本憲一 +1 位作者 赵刚 吴文博 《Chinese Physics C》 SCIE CAS CSCD 2023年第3期206-217,共12页
The 12C+12C reaction rate plays an essential role in stellar evolution and nucleosynthesis.Nevertheless,the uncertainties of this reaction rate are still large.We calculate a series of stellar evolution models w... The 12C+12C reaction rate plays an essential role in stellar evolution and nucleosynthesis.Nevertheless,the uncertainties of this reaction rate are still large.We calculate a series of stellar evolution models with the near solar abundance from the zero-age main-sequence through presupernova stages for initial masses of 20 M⊙ to 40 M⊙.The 12C+12C reaction rates from two different studies are used in our investigation.One is the rate obtained using the Trojan Horse Method(THM)by Tumino et al.[Nature 557(7707),687(2018)],and the other was obtained by Mukhamedzhanov et al.[Physical Review C 99(6),064618(2019)](Muk19).Then,comparisons of the nucleosynthesis and presupernova isotopic abundances are conducted.In particular,we find that in the C burning shell,models with the THM produce a smaller amount of 23Na and some neutron-rich isotopes than Muk19.The difference in the abundance ratios of Na/Mg,S/Mg,Ar/Mg,and K/Mg between the two models are apparent.We compare Na/Mg obtained from our theoretical presupernovae models with Na/Mg in stellar atmospheres observed with high-resolution spectra as well as from the latest galactic chemical evolution model.Although Na/Mg obtained using the THM is within 2σ of the observed stellar ratio,the theoretical uncertainty on Na/Mg introduced by the uncertainty of the 12C+12C reaction rate is almost equivalent to the standard deviation of astronomical observations.Therefore,a more accurate 12C+12C reaction rate is crucial. 展开更多
关键词 reaction rate presupernova nucleosynthesis massive stars
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Nucleosynthesis in thermonuclear supernovae 认领 引用 被引量：2
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作者 Claudia Travaglio W. Raphael Hix 《Frontiers of physics》 SCIE CSCD 2013年第2期199-216,共18页
We review our understanding of the nucleosynthesis that occurs in thermonuclear supernovae and their contribution to Galactic Chemical evolution. We discuss the prospects to improve the modeling of the nucleosynthesis... We review our understanding of the nucleosynthesis that occurs in thermonuclear supernovae and their contribution to Galactic Chemical evolution. We discuss the prospects to improve the modeling of the nucleosynthesis within simulations of these events. 展开更多
关键词 supernovae nuclear reactions explosive nucleosynthesis stellar spectra,hydrodynamics chemical evolution
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Correlativity of nucleosynthesis in low-mass AGB stars 认领 引用
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作者 刘永新 张波 彭秋和 《Science China Mathematics》 1996年第10期1112-1120,共9页
In a self-consistent treatment, an LM-AGB TP model of HHe-burning and no-branch reaction passway for s-process from Fe-Bi with correlative reaction network from C-Ne is used to reproduce the enrichment of F, C and hea... In a self-consistent treatment, an LM-AGB TP model of HHe-burning and no-branch reaction passway for s-process from Fe-Bi with correlative reaction network from C-Ne is used to reproduce the enrichment of F, C and heavy elements in the surface of MS and S stars (with Tc). The growing of the core mass and the mass loss through steller winds are also considered. Comparisons between the computed correlation: {[F/O], C/O}; {[F/O], (s/Ti)} and that of the observations are then presented. It appears that fluorine and heavy elements can be synthesized where the nucleosynthesis events occur in a fit temperature range, and then are dredged up to the surface of the star. Because F production only occurs in a narrow temperature range, the synthesis events are sensitive to temperature. The observation of this case is discussed specially. 展开更多
关键词 AGB stars nucleosynthesis correlation.
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Xenon isotope record of nucleosynthesis and the early solar system 认领 引用
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作者 Jauh-tzuoh Lee, LI Bin and Oliver ManuelDepartment of Chemistry, University of Missouri, Rolla, MO 65401, USA 《Chinese Science Bulletin》 1997年第9期752-756,共5页
ISOTOPIC abundances of Xe were determined as two FeS separates of the Allende（C3V）car-bonaceous chondrite were heated,stepwise.A tracer Xe isotope was first produced in one sam-ple by 130Te（n,γ 2β-）131rXe reacti... ISOTOPIC abundances of Xe were determined as two FeS separates of the Allende（C3V）car-bonaceous chondrite were heated,stepwise.A tracer Xe isotope was first produced in one sam-ple by 130Te（n,γ 2β-）131rXe reaction to monitor the degassing of Xe from the sample.TheFeS melted at 950℃,releasing a spike of 131rXe and terrestrial-type Xe,Xe-T.This 展开更多
关键词 xenon nucleosynthesis isotopes iron sulfide supernova.
Examination of Radiative Capture Rates of 99Tc(n,γ)100Tc and Stellarβ−Decay Rates of99Tc 认领 引用
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作者 Abdul Kabir Jameel-Un Nabi +2 位作者 Muhammad Tahir Zain Ul Abideen Isha Mudassir 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2025年第3期25-30,共6页
Within the context of the proton-neutron quasi-particle random phase approximation(pn-QRPA)model and TALYS v1.96 code,the radiative capture(99Tc(n,γ)100Tc)and stellar weak interaction(99Tc→99Ru+e−+ν_... Within the context of the proton-neutron quasi-particle random phase approximation(pn-QRPA)model and TALYS v1.96 code,the radiative capture(99Tc(n,γ)100Tc)and stellar weak interaction(99Tc→99Ru+e−+νe)rates were computed during thermal pulses operating in asymptotic giant branch stars.The Maxwellian average cross-section(MACS)and neutron capture rates for the99Tc(n,γ)100Tc process are analyzed within the context of statistical code TALYS v1.96.The effect of nuclear level density(NLD)andγ-strength functions on MACS and neutron capture rates has been examined.The model-based computations for MACS provided an insightful contrast to prior investigated findings.The sensitivity of stellar weak interaction rates to different densities and temperatures is investigated using the pn-QRPA model.The impact of thermally populated excited states on electron emission(β−)rates in99Tc is extensively examined.Additionally,a comparison is made between the study of the stellarβ−decay rates and the thermal neutron capture rates.It is found that at T9=0.26 the thermal neutron capture rates(λ(n,γ))and the temperature dependent stellarβ−decay rates( λβ-)cross each other.However,at higher temperatures,theλ(n,γ)are found to be higher than λβ-. 展开更多
关键词 astroparticle physics-nuclear reactions nucleosynthesis abundances-stars AGB and post-AGB-stars evolution
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