Phase and Polarization State of High-Frequency Relic Gravitational Waves

The displaying condition of strength, phase and polarization states of high-frequency relic gravitational waves （HFRGWs） in electromagnetic （EM） detecting systems is studied. It is shown that the displaying condition depends not only on the sensitivity of EM detecting systems and the amplitudes of HFRGWs, but also on the phase, the polarization states of HFRGWs and their matching to the EM detecting systems. In order to display simultaneously the strength, phase and polarization states of the resonant ＂monochromatic component＂ of HFRGWs, an important necessary condition is the utilization of two or more different EM detectors.     

New initial condition of the new agegraphic dark energy model

The initial condition Ω_de(z_ini)=n²(1+z_ini)^-2/4 at z_ini=2000 widely used to solve the differential equation of the density of the new agegraphic dark energy (NADE) Ω_de, makes the NADE model be a single-parameter dark-energy cosmological model. However, we find that this initial condition is only applicable in a flat universe with only dark energy and pressureless matter. In fact, in order to obtain more information from current observational data, such as the cosmic microwave background (CMB) and the baryon acoustic oscillations (BAO), we need to consider the contribution of radiation. For this situation, the initial condition mentioned above becomes invalid. To overcome this shortage, we investigate the evolutions of dark energy in the matter-dominated and the radiation-dominated epochs, and obtain a new initial condition Ω_de(z_ini)=n²(1+z_ini)^-2(1+√F(z_ini)²/4 at z_ini=2000, where F(z)≡Ω_r0(1+z)/[Ω_m0+Ω_r0(1+z)] with Ω_r0 and Ω_m0 being the current density parameters of radiation and pressureless matter, respectively. This revised initial condition is applicable for the differential equation of Ω_de obtained in the standard Friedmann-Robertson-Walker (FRW) universe with dark energy, pressureless matter, radiation, and even spatial curvature, and can still keep the NADE model being a single-parameter model. With the revised initial condition and the observational data of type Ia supernova (SNIa), CMB, and BAO, we finally constrain the NADE model. The results show that the single free parameter n of the NADE model can be constrained tightly.     

Hadronic Scenarios for Gamma-Ray Emission from Three Supernova Remnants Interacting with Molecular Clouds

GeV γ-rays detected with the large area telescope on board the Fermi Gamma-ray space telescope in the direc- tion of HB21, MSH 17-39 and G337.0-0.1 have been recently reported. The three supernova remnants （SNRs） show interactions with molecular clouds, and they are effective gamma-ray emitters as the relativistic protons accelerated by the SNR shocks inelastically colliding with the dense gas in the clouds. The origin of the observed γ-rays for the three remnants is investigated in the scenario of the diffusive shock acceleration. In the model, a part of the SNR shock transmits into the nearby molecular clouds, and the shock velocity is greatly reduced. As a result, a shock with a relatively low Alfven Mach number is generated, and the spectra of the accelerated protons and thee＇γ-ray photons produced via proton-proton interaction can be obtained. The results show that the observed γ-ray spectra for the three SNRs interacting with the molecular clouds can be reproduced. It can be concluded that the hadronic origin of the γ-rays for the three SNRs is approved, and the ability of SNR shocks to accelerate protons is also supported.     

SKLOF:一种新的超新星候选范围约减算法

超新星是宇宙学中的“标准烛光”, 其在星系中爆发的概率很低, 是一种特殊、稀少的天体, 只有在大量观测的星系数据中才有机会遇到, 而正处于爆发期的超新星会照亮其整个星系从而在观测获得的星系光谱中具有较明显的特征。但是, 目前已发现的超新星数量相对于大量的天体而言又是非常稀少的, 搜寻它们所用的计算时间成为能否进行后续观测的关键, 因此需要寻找高效率的超新星搜寻方法。对超新星候选范围进行约减的LOF算法的时间复杂度较高, 计算量大, 不适用于大规模数据集。为此通过对LOF算法进行改进, 提出了一种在海量星系光谱中快速约减超新星候范围的新方法(SKLOF)。首先对光谱数据集中离中心点近的数据点进行数据剪枝, 剪掉那些肯定不是超新星候选体的光谱数据对象, 然后利用改进的LOF算法计算剩余的光谱数据的孤立性因子并降序排列进行离群搜索, 最后获得超新星候选体的较小的搜索范围以便进行后续的证认。实验结果表明, 该算法十分有效, 不仅在精确度上有所提高, 而且相比于LOF算法还进一步缩短了算法的运行时间, 提高了算法的执行效率。     

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.     

In-Medium K^＋ and K^- Production and K^- Condensation in Supernova Matter

In-medium effects and neutrino trapping on K^ and K^- production and K^- condensation in supernova matter are investigated in a chiral hadronic model. Our results show that neutrino trapping shifts the critical density for K^- condensation to higher density, the Q values for K^ and K^- production are not sensitive to neutrino trapping, in-medium effects decrease the Q values for NN→NNK^ K^- and AN→NNK^- and increase those for NN→NAK^ , K^- p→Aπ^0 and K^-n→Aπ^- as the density of supernova matter increases. Moreover, it is shown that neutrino trapping decreases the maximum masses of protoneutron stars compared with the neutrino-free case.     

超新星爆发与原初云的质量流失

本文着重研究了超新星爆发对矮星系演化的反馈作用。指出,单个超新星在外壳层中爆发,导致气体的逐渐丢失,可能是反馈的主要形式,现在观测到的矮星系可能是由较高密度的原初云在丢失了大量气体后形成的。     

Effects of Electron Screening on Electron Capture Rates in High Density Presupernova Core

Considering that the electron capture rate can be greatly reduced by the electron screening effect in the regime of high temperature and high density,we calculate the effect of electron screening on the electron capture rate for two important elements ^56 Ni and ^55Co in the high density condition of a pre-supernova star.The effect of electron screening is so effective that the electron capture rate may be reduced to about 20%.     

星际26Al核合成的研究进展

介绍了星际 26Al衰变所发射1 809 keV γ射线的最新空间探测结果， 综述了目前关于星际 26Al起源的各种天体模型的研究进展。最后， 简要阐述了14N(p,γ)15O反应截面的最新测量结果及其对 26Al起源研究的影响， 探讨了一种星际 26Al合成的可能新途径。The recently detection outcome about interstellar 26Al is introduced, as well as the investigation progresses of interstellar 26Al nucleosynthesis in all models are reviewed. Finally, the new nuclear physics experimental results for the14N(p,γ)15O reaction effect on sources of interstellar 26Al and an alternative new way for nucleosynthesis 26Al in SNIa are discussed.     

矿业遗迹旅游开发监管的演化博弈与稳定性分析

矿业遗迹旅游开发涉及主体众多，均衡各方主体利益对兼顾矿业遗迹保护和开发具有重要意义。文章搭建企业、政府和矿区居民三方核心利益主体的静态演化博弈模型，并在静态演化博弈基础上引入动态变量，利用系统动力学仿真分析三方在一般惩罚、动态惩罚与优化动态奖惩三种方案下的行为策略及稳定情况，并采用李雅普诺夫稳定性理论进行双重论证。研究发现：一般惩罚与动态惩罚方案下三方行为均不稳定，但动态惩罚方案在一定程度上能够抑制三方行为的波动情况；优化动态奖惩方案能够有效抑制三方行为的反复波动并达到理想的稳定状态。基于研究结论，文章提出政府应采取综合优化动态奖惩方案规制矿业遗迹再开发；设计各类政府监管工具组合拳、构建矿业遗迹开发生态文化体系与培育生态文化框架等建议。