Nuclear statistical equilibrium at core-collapse supernova

A new improved nuclear partition function is employed to calculate the nuclear statistical equilibrium (NSE) in core-collapse supernova environment. The results show that the change of nucleus abundance is slight even though the temperature is higher than 10$^{11}$\,K when shock propagates, which indicates that the effect of the nuclear partition function is not so important as shown in the previous calculations, but it can also be considered in detailed simulation if it is sensitive to weak interaction rates in core-collapse supernova.     

Heavy sterile neutrinos and supernova explosions

We consider sterile neutrinos with rest masses 0.2 GeV and with vacuum flavor mixing angles θ²>10⁻⁸ for mixing with τ-neutrinos, or 10⁻⁸<θ²<10⁻⁷ for mixing with muon neutrinos. Such sterile neutrinos could augment core collapse supernova shock energies by enhancing energy transport from the core to the vicinity of the shock front. The decay of these neutrinos could produce a flux of very energetic active neutrinos, detectable by future neutrino observations from galactic supernova. The relevant range of sterile neutrino masses and mixing angles can be probed in future laboratory experiments.     

恒星演化和超生爆发理论中某些重要问题的核物理问题

首先,在第1节中我们依次介绍了各种不同质量的恒星演化进程中各个主要热核燃烧的点火条件,致密物质中自由电子系统的简并性对星体热核燃烧的主导作用以及爆炸性核燃烧条件。其次,在第2节中我们讨论了导致恒星核心不稳定坍缩的物理因素和条件。此后,在本第3节中我们评述了Ia型超新星爆发理论尚在急论中的核物理和固体物理的问题。在第4节中我们评述了Ⅱ型（以及Ib型）超新星爆发理论中的严重困难,并且介绍了我们（南京大学研究小组）就超新星中微子延缓爆发机制的关键问题（强大的中微子暴如何产生？）的物理机制提出的具体过程：这中微子暴的强大中微子流量是从刚刚坍缩的高温高密核心通过核物质－－（u,d）夸克系统－－（u,d,s)系统的相变过程在不到1微秒的时间内很快地产生出来的。而且,这个过程导致核心区域的负熵梯度,引起核心区域大规模对流,它将这强大的中微子流量很快地向外输送到中微子球的表面。在第5节中本还介绍了我们就超新星核心高密条件下电荷屏蔽对电子俘获过程的影响所作的探讨研究以及讨论了它对超新星坍缩核心质量（它对超新星瞬时爆发机制成功与否起着关键作用）的可能影响。     

恒星演化和超新星爆发理论中某些重要问题的核物理问题

首先 ,在第 1节中我们依次介绍了各种不同质量的恒星演化进程中各个主要热核燃烧的点火条件 ,致密物质中自由电子系统的简并性对星体热核燃烧的主导作用以及爆炸性核燃烧条件。其次 ,在第 2节中我们讨论了导致恒星核心不稳定坍缩的物理因素和条件。此后 ,在本文第 3节中我们评述了Ⅰa 型超新星爆发理论尚在争论中的核物理和固体物理的问题。在第 4节中我们评述了Ⅱ型 (以及Ib 型 )超新星爆发理论中的严重困难 ,并且介绍了我们 (南京大学研究小组 )就超新星中微子延缓爆发机制的关键问题 (强大的中微子暴如何产生 ?)的物理机制提出的具体过程 :这中微子暴的强大中微子流量是从刚刚坍缩的高温高密核心通过核物质——— (u ,d)夸克系统——— (u ,d ,s)系统的相变过程在不到 1微秒的时间内很快地产生出来的的。而且 ,这个过程导致核心区域的负熵梯度 ,引起核心区域大规模对流 ,它将这强大的中微子流量很快地向外输送到中微子球的表面。在第 5节中本文还介绍了我们就超新星核心高密条件下电荷屏蔽对电子俘获过程的影响所作的探讨研究以及讨论了它对超新星坍缩核心质量 (它对超新星瞬时爆发机制成功与否起着关键作用 )的可能影响。     

Possible violation of the spin-statistics relation for neutrinos: checking through future galactic supernova

We use the detection of neutrinos from a future galactic type-II supernova event in a water Cerenkov detector like Super-Kamiokande to constrain the possible violation of spin-statistics by neutrinos resulting in their obeying a mixed statistics instead of Fermi–Dirac.     

大爆炸核合成与宇宙背景中微子

文章基于大爆炸宇宙学描述了发生于宇宙早期的中微子退耦与轻核素合成事件。退耦后的中微子形成宇宙的背景之一。文章介绍了几种探测宇宙背景中微子的方法,侧重于利用b衰变核俘获超低动能的中微子。     

大爆炸核合成与宇宙背景中微子

文章基于大爆炸宇宙学描述了发生于宇宙早期的中微子退耦与轻核素合成事件。退耦后的中微子形成宇宙的背景之一。文章介绍了几种探测宇宙背景中微子的方法,侧重于利用β衰变核俘获超低动能的中微子。     

Nuclear Masses and the r- and p-Processes of Nucleosynthesis

Although important efforts have been devoted in the last decades to measure atomic masses, the modelling of the r- and p-processes of nucleosynthesis still requires the use of theoretical predictions to estimate experimentally unknown masses in the neutron-rich and neutron-deficient regions. Different mass models are available to extrapolate nuclear masses far away from the experimentally known region. These models are compared and used to estimate the reaction rates of relevance in the r- and p-processes. The impact of the different mass models on the astrophysics predictions are discussed. This revised version was published online in July 2006 with corrections to the Cover Date.     

Beta decay rates for nuclei with 115<A<140 for r-process nucleosynthesis

For r-process nucleosynthesis the β-decay rates for a number of neutron-rich intermediate heavy nuclei are calculated. The model for the β-strength function is able to reproduce the observed half-lives quite well.     

Nuclear reactions and the double beta decay

Charge-exchange reactions of (n,p) and (p,n) types at intermediate energies are introduced as a tool for the study of nuclear matrix element in ββ decay. Here, the (n,p) type reactions are realized through , where ²He refers to two protons in a singlet ¹S₀ state and where both of these are momentum analyzed and detected by the same spectrometer and detector. These reactions have been developed and performed exclusively at KVI, Groningen (NL), using an incident deuteron energy of 183 MeV. The  reaction is of (p,n) type and was developed at the RCNP facility in Osaka (JP) at incident energies of 420 MeV. Using both reaction types one can extract the Gamow-Teller transition strengths B(GT⁺) and , which define the two “legs” of the ββ decay matrix elements for the 2νββ decay. The high resolution available in both reactions allows a detailed insight into the excitations of the intermediate odd-odd nuclei and, as will be shown, some unexpected features are being unveiled.     

Beta-transition properties for neutron-rich Sn and Te isotopes by Pyatov method

Based on Pyatov’s method, the low-lying Gamow-Teller (GT) 1⁺ state energies and log(ft) values for ^128,130,132Sb and ^132,134,136I isotopes have been calculated. In this method, the strength parameter of the effective spin-isospin interaction is found by providing the commutativity of the GT operator with the central part of the nuclear Hamiltonian. The problem has been solved within the framework of RPA. The calculation results have been compared with the corresponding experimental data.      

Photo-induced nucleosynthesis: Current problems and experimental approaches

Photon-induced reactions play a key role in the nucleosynthesis of rare neutron-deficient p -nuclei. The paper focuses on , , and reactions which define the corresponding p -process path. The relation between stellar reaction rates and laboratory cross-sections is analyzed for photon-induced reactions and their inverse capture reactions to evaluate various experimental approaches. An improved version S _C(E) of the astrophysical S -factor is suggested which is based on the Coulomb wave functions. S _C(E) avoids the apparent energy dependence which is otherwise obtained for capture reactions on heavy nuclei. It is found that a special type of synchrotron radiation available at SPring-8 that mimics stellar blackbody radiation at billions of kelvins is a promising tool for future experiments. By using the blackbody synchrotron radiation, sufficient event rates for and reactions in the p -process path can be expected. These experiments will provide data to improve the nuclear parameters involved in the statistical model and thus reduce the uncertainties of nucleosynthesis calculations.     

Electron dynamics and spatial characteristics of emission from electron oscillation driven by femtosecond laser pulses

The dynamics and characteristics of spatial distribution of emission are analyzed with a single electron model in the cases of different intensities and different polarized femtosecond laser pulses. It is discovered that with the increase of laser intensity, for circularly polarized laser pulse, the angular distribution is tipped forward more and more; for linearly polarized laser pulse, the radiation pattern is changed from the fourfold rotational symmetry bifoliate pattern same as that from a dipole antenna to twofold rotational symmetry trefoil pattern.     

Neutrinos and explosive nucleosynthesis

Core-collapse supernovae produce a hot protoneutron star that cools emitting huge amounts of neutrinos of all flavors. The interaction of these neutrinos with the outer layers of the protoneutron star produces an outflow of matter whose composition is determined by the luminosities and energies of the emitted neutrinos and antineutrinos. The presence of light nuclei like deuterons and tritons can have a big impact in the average energies of the emitted antineutrinos and consequently in the neutron-richness of the ejected matter. Recent hydrodynamical models show that the ejected matter is in fact proton-rich and constitutes the site of the νp-process where antineutrino absorption reactions catalyze the nucleosynthesis of nuclei with A>64.     

Nuclear core dynamics and rearrangement energy for hypernuclei

The effect of the nuclear core dynamics on the binding energies of Λ hypernuclei is studied in the framework of variational correlated wave functions. In addition to the core energy and to a Λ single-particle contribution ϵ_ν, we exhibit a rearrangement energy E_R which in particular depends on the ΛN correlations F and on the difference δφ_N between the core wave function and its exact ground-state value. E_R is nonzero only if there are both ΛN correlations (F ≠ 1) and if δφ_N ≠ 0. The latter can result from core polarization by the Λ or from errors in the ground-state variational wave function of the core. E_R varies linearly with δφ_N for small δφ_N. Detailed numerical results for central ΛN and NN potentials with repulsive cores confirm these general features. For a give core wave function ΛN correlations reduce the radius of the core nucleons relative to their c.m.; however E_R leads to an expansion of the core rather than to a contraction with only ϵ_ν. The core polarization eneegy is quite small ⋍ 0.4 MeV. We study the effects of errors in the variational core wave function by detuning this as a function of one of the variational parameters.     

Nuclear Physics Programs for the Future RIBs Facility in Korea

We present nuclear physics programs based on the planned experiments using rare isotope beams (RIBs) for the future Korean Rare Isotope Beams Accelerator facility(KRIA). This ambitious facility has both an Isotope Separation On Line (ISOL) and fragmentation capability for producing RIBs and accelerating beams of wide range mass of nuclides with energies of a few to hundreds MeV per nucleon. Low energy RIBs at Elab = 5 to 20 MeV per nucleon are for the study of nuclear structure and nuclear astrophysics toward and beyond the drip lines while higher energy RIBs produced by inflight fragmentation with the reaccelerated ions from the ISOL enable to explore the neutron drip lines in intermediate mass regions. The planned programs have goals for investigating internal structures of the exotic nuclei toward and beyond the nucleon drip lines by addressing the following issues: how the shell structure evolves in areas of extreme proton to neutron imbalance; whether the isospin symmetry maintains in isobaric mirror nuclei at and beyond the drip lines; how two-proton radioactivity affects abundances of the elements; what the role of the continuum states including resonant states above protondecay threshold in exotic nuclei is in astrophysical nuclear reaction processes, and how the nuclear reaction rates triggered by unbound proton-rich nuclei make an effect on rapid proton capture processes in a very hot stellar plasma.     

Transfer ionization in isocharge sequence ion and Ne collisions

The dependence of the ratio R1 for transfer ionization to single capture for Cq+, Nq+, Oq+, Neq+ ions on Ne target upon the electronic structure of the projectile is studied. For Aq+-Ne collisions the ratio R1 decreases as the atomic number Z of the projectile increases for q=4,5,6,7 sequences which provides strong evidence for the increase of the binding energy of the target valence electron after single electron capture. The increase in binding energy depends both upon the atomic number of the projectile and the target atom.