XTE J1550-564 2001年“迷你爆发”的X射线能谱研究

黑洞X射线暂现源的迷你爆发是一类峰值光度较低、持续时间较短的爆发.由于观测数据较少,其物理机制仍不清楚.利用RXTE (Rossi X-ray Timing Explorer)卫星从2001年1月28日到3月14日的数据,研究了黑洞X射线暂现源XTE J1550–564 2001年迷你爆发的X射线能谱特性.发现在本次迷你爆发中, XTE J1550–564的X射线能谱可以用幂律谱很好地拟合.整个爆发的硬度强度图不是标准的q型,而是一直保持在最右侧.此外,还分析了此次爆发谱指数Γ与未吸收的2–10 keV能段的X射线流量F_(2–10 keV)的相关性,发现Γ-F_(2–10 keV)呈反相关关系,且谱指数Γ∈[1.35, 1.72].上述结果表明2001年这次爆发一直处于低/硬态,它的X射线辐射主要来自于辐射低效的吸积模式,如ADAF(Advection-Dominated Accretion Flow).     

公用机房的硬盘保护措施

在深入分析硬盘结构及硬盘工作原理的基础上,详细阐述了用软件实现对公用机房硬盘的保护原理和方法,并给出了编程思路。     

甘肃北山造山带类型及基本特征

北山造山带经历多期次、多阶段的板块裂解－俯冲－碰撞－拼合的复杂地质演化历程，具多旋回复合造山的特色。通过对造山带构造单元的建立、古板块重建、原型盆地恢复、造山带结构、构造特征及造山机制和模式的研究，确定北山造山带类型为陆－增生弧碰撞造山带。     

中国东南沿海及邻近海区一种独特的大陆增生方式——转换断层向俯冲体系的转变

闽东沿海构造带—东海陆架西缘断裂、钓鱼岛隆起带(台湾—宍道褶皱带)以及帛琉—九州洋脊在中生代期间先后经历了自转换断层向俯冲系统的转变,这种转变构成了中国东南及毗邻海区独特的大陆增生方式,它表明特提斯和古太平洋的演化对这一地区的中、新生代构造格局起着重要的制约作用。     

海平面升降变化对贵州紫云礁体生长的控制

以贵州紫晚二叠世碳酸盐台地边缘礁为例,运用高频层序地层学原理和方法,精细地划分了紫云礁层序的各级单元,并对其内部沉积构成进行了详细研究,探讨海平面和变化对礁体生长的控制,研究结果表明,晚二叠世紫云礁 合体为发育在台地边缘坡折带的一个三级层序,由１３个准层序组成,并可识别出低位、海侵、高位３个体系域,低位期的下切谷 边缘坡折带碳酸盐台地的暴露、海侵期和高位期礁的３种生长方式的增生及每种生长方式的特定     

The fraction of galaxies that contain active nuclei and their accretion rates

We investigate the relationship between the present-day optical luminosity function of galaxies and the X-ray luminosity function of Seyfert 1s to determine the fraction of galaxies that host Seyfert 1 nuclei and their Eddington ratios. The local type 1 active galactic nuclei (AGN) X-ray luminosity function is well reproduced if ∼1 per cent of all galaxies are type 1 Seyferts which have Eddington ratios of ∼10⁻³. However, in such a model the X-ray luminosity function is completely dominated by AGN in E and S0 galaxies, contrary to the observed mix of Seyfert host galaxies. To obtain a plausible mix of AGN host galaxy morphologies requires that the most massive black holes in E and S0 galaxies accrete with lower Eddington ratios, or have a lower incidence of Seyfert activity, than the central black holes of later-type galaxies.     

Peculiarities of the UV continuum energy distribution for T Tauri stars

In the UV spectra of BP Tau, GW Ori, T Tau, and RY Tau obtained with the Hubble Space Telescope, we detected an inflection near 2000 Å in the F _λ ^c (λ) curve that describes the continuum energy distribution. The inflection probably stems from the fact that the UV continuum in these stars consists of two components: the emission from an optically thick gas with T<8000 K and the emission from a gas with a much higher temperature. The total luminosity of the hot component is much lower than that of the cool component, but the hot-gas radiation dominates at λ<1800 Å. Previously, other authors have drawn a similar conclusion for several young stars from low-resolution IUE spectra. However, we show that the short-wavelength continuum is determined from these spectra with large errors. We also show that, for three of the stars studied (BP Tau, GW Ori, and T Tau), the accretion-shock radiation cannot account for the observed dependence F _λ ^c (λ) in the ultraviolet. We argue that more than 90% of the emission continuum in BP Tau at λ>2000 Å originates not in the accretion shock but in the inner accretion disk. Previously, a similar conclusion was reached for six more classical T Tau stars. Therefore, we believe that the high-temperature continuum can be associated with the radiation from the disk chromosphere. However, it may well be that the stellar chromosphere is its source.     

X-ray emission from accretion disks in active galactic nuclei

We constructed a grid of relativistic models for standard high-relative-luminosity accretion α-disks around supermassive Kerr black holes (BHs) and computed X-ray spectra for their hot, effectively optically thin inner parts by taking into account general-relativity effects. They are known to be heated to high (～10⁶–10⁹ K) temperatures and to cool down through the Comptonization of intrinsic thermal radiation. Their spectra are power laws with an exponential cutoff at high energies; i.e., they have the same shape as those observed in active galactic nuclei (AGNs). Fitting the observed X-ray spectra of AGNs with computed spectra allowed us to estimate the fundamental parameters of BHs (their mass and Kerr parameter) and accretion disks (luminosity and inclination to the line of sight) in 28 AGNs. We show that the Kerr parameter for BHs in AGNs is close to unity and that the disk inclination correlates with the Seyfert type of AGN, in accordance with the unification model of activity. The estimated BH masses M_x are compared with the masses M_rev determined by the reverberation mapping technique. For AGNs with luminosities close to the Eddington limit, these masses agree and the model under consideration may be valid for them. For low-relative-luminosity AGNs, the differences in masses increase with decreasing relative luminosity and their X-ray emission cannot be explained by this model.     

赣东北前寒武纪港边杂岩体的岩浆混合（和）作用及其地质意义

赣东北地区沿江绍断裂北缘和江南造山带南侧有大量的前寒武纪火山侵入杂岩呈带状分布,主要由大面积的陆相火山岩和若干长英质镁铁质火成杂岩体组成,后者中出露面积最大的港边杂岩体在填图尺度上可划分为长英质岩、镁铁质岩和过渡性岩3大组成部分,长英质岩颗粒锆石U_Pb谐和不一致曲线上交点年龄为822±4Ma,代表杂岩体中岩浆混合作用发生的时间。港边岩体中长英质岩石的Nd模式年龄为1·49~1·68Ga,镁铁质岩中玄武质岩石为1·51~2·21Ga,辉长岩的Nd模式年龄与玄武质岩石基本相同,为1·54~2·13Ga,经计算的过渡性岩石的Nd模式年龄为1·58~1·90Ga,因此认为镁铁质岩石从源区分离的时间要远早于长英质岩石,而过渡性岩石含有前两个端员岩浆相互混合(和)的信息。长英质岩石的εNd(t=822Ma)值为-0·8~-4·4,87Sr/86Sr(822)比值为0·70368~0·70549;玄武质岩石的εNd(822)值为-2·6~+2·3,87Sr/86Sr(822)比值为0·70387~0·70527,这反映了镁铁质岩浆的源区接近总地球,长英质岩浆则来自具壳幔混合性质的EMⅠ型地幔的源区。可以推测,赣东北前寒武纪也曾发生过岩浆底侵作用。底侵作用对港边火成杂岩体岩浆的形成起着重要的作用。底侵于壳幔边界的玄武质岩浆使地壳熔融形成长英质岩浆并聚集于浅部岩浆房。随着长英质岩浆房降温,长英质岩浆的结晶度和粘度增加,其物理状态发生液态→(固+液)混合态→固态的变化;当玄武质岩浆穿透下地壳并不断进入物理状态变化的长英质岩浆房时,持续地发生两种岩浆的化学混合作用或两岩浆的机械混合作用或玄武质岩浆的侵入,其混合作用的时间以长英质岩锆石的U_Pb谐和不一致曲线上交点年龄822±4Ma界定。根据Nd模式年龄(tDM)和Nd富集系数(fSm/Nd)分布特征,可以确定中元古代江南造山带为太古宙扬子古陆核的横向增生体,而新元古代陆相火山侵入杂岩带则横向增生于江南造山带南缘。至此,扬子古陆横向增生作用结束,开始与华夏古陆拼贴,包括港边火成杂岩体在内的新元古代火山侵入杂岩带则成为两古陆连结的纽带。