On the link between disc-galaxies and Damped Lyman-α systems

We model the chemical and spectrophotometric evolution of the Milky Way, spiral galaxies and Low Surface Brightness Galaxies in a consistent way. Some consequences with respect to the nature of Damped Lyman-α systems (DLAs) are investigated. This revised version was published online in September 2006 with corrections to the Cover Date.     

Absorption features in the quasar HS 1603 + 3820 II. Distance to the absorber obtained from photoionisation modelling

We present the photoionisation modelling of the intrinsic absorber in the bright quasar HS 1603 + 3820. We constructed the broad-band spectral energy distribution using the optical/UV/X-ray observations from different instruments as inputs for the photoionisation calculations. The spectra from the Keck telescope show extremely high Civ to Hi ratios, for the first absorber in system A, named A1. This value, together with high column density of Civ ion, place strong constraints on the photoionisation model. We used two photoionisation codes to derive the hydrogen number density at the cloud illuminated surface. By estimating bolometric luminosity of HS 1603 + 3820 using the typical formula for quasars, we calculated the distance to A1. We could find one photoionization solution, by assuming either a constant density cloud (which was modelled using cloudy), or a stratified cloud (which was modelled using titan), as well as the solar abundances. This model explained both the ionic column density of Civ and the high Civ to Hi ratio. The location of A1 is 0.1 pc, and it is situated even closer to the nucleus than the possible location of the Broad Line Region in this object. The upper limit of the distance is sensitive to the adopted covering factor and the carbon abundance. Photoionisation modelling always prefers dense clouds with the number density n₀ = 10¹⁰ − 10¹² cm⁻³, which explains intrinsic absorption in HS 1603 + 3820. This number density is of the same order as that in the disk atmosphere at the implied distance of A1. Therefore, our results show that the disk wind that escapes from the outermost accretion disk atmosphere can build up dense absorber in quasars.     

精确的频率空间域黏声波有限差分数值模拟

在时间空间域,模拟吸收衰减效应时对计算机内存需求大,计算效率不高、非常难以进行模拟吸收衰减;频率空间域通过引入品质因子和复值速度,使用经验物理、数学公式进行数值模拟吸收衰减就容易多了。笔者使用十分节省计算机内存需求的嵌套剖分法,使用Kjartansson模型高效率地进行模拟吸收衰减。数值试验证实吸收衰减影响地震场的所有频率、对高频的影响最为明显,降低了地震记录的质量;频率空间域非常容易模拟吸收衰减效应,为黏声波全波形反演实际地震资料而奠定很好的基础。     

基于动态子波估计的吸收系数提取方法

在基于褶积模型的子波提取中,大多假设地震子波为最小相位性质。虽然在地震资料处理中进行了相位转换和Q补偿处理,但从实际地震记录中提取的地震子波,大多也表现为混合相位性质。提取吸收系数大多采用地震记录谱模拟方法,即用地震记录振幅谱平滑代替子波振幅谱,这样就会存在一个误差项,给以常规方法提取的吸收系数地震剖面属性解释带来更多的不确定性。针对以上问题,在地震叠偏剖面上,动态计算地震子波的振幅谱和相位谱,可得到任意相位性质的地震子波,采用谱比法并应用相位项提取较准确的吸收系数。利用动态子波提取的吸收系数剖面,精细显示出储层中含油气和未含油气区域的明显差异,结合嘉陵江组一段动态吸收系数平面图分析,为工区储层的精细解释提供了一种精确的方法。     

水分子对硝酸根分子振动的影响

利用第一性原理计算硝酸根与1～3个水分子形成的水合物(NO3-.nH2O,n=1～3)的红外吸收谱,并与测量的硝酸钠水溶液的红外吸收谱进行了比较分析。计算结果表明硝酸根与水分子所形成的水合物具有多种稳定的结构,其中硝酸根与1个水分子结合的亚稳定结构,其硝酸根反对称伸缩振动的劈裂与硝酸钠水溶液中硝酸根的红外吸收谱结果一致,表明硝酸盐溶液中每一硝酸根与附近水分子的作用效果等效为NO3-.1H2O。     

Spatial fluctuations in the spectral shape of the ultraviolet background at 2 < z < 3 and the reionization of helium

The low-density hydrogen and helium in the intergalactic medium (IGM) probed by quasi-stellar object (QSO) absorption lines is sensitive to the amplitude and spectral shape of the metagalactic ultraviolet (UV) background. We use realistic H  i and He  ii Lyα forest spectra, constructed from state-of-the-art hydrodynamical simulations of a Λ cold dark matter (ΛCDM) universe to confirm the reliability of using line profile fitting techniques to infer the ratio of the metagalactic H  i and He  ii ionization rates. We further show that the large spatial variations and the anticorrelation with H  i absorber density observed in the ratio of the measured He  ii to H  i column densities can be explained in a model where the H  i ionization rate is dominated by the combined UV emission from young star-forming galaxies and QSOs and the He  ii ionization rate is dominated by emission from QSOs only. In such a model the large fluctuations in the column density ratio are due to the small number of QSOs expected to contribute at any given point to the He  ii ionization rate. A significant contribution to UV emission at the He  ii photoelectric edge from hot gas in galaxies and galaxy groups would decrease the expected fluctuations in the column density ratio. Consequently, this model appears difficult to reconcile with the large increase in He  ii opacity fluctuations towards higher redshift. Our results further strengthen previous suggestions that observed He  ii Lyα forest spectra at z ∼ 2–3.5 probe the tail end of the reionization of He  ii by QSOs.     

Ultraviolet spectroscopy of Comet 9P/Tempel 1 with Alice/Rosetta during the Deep Impact encounter

We report on spectroscopic observations of periodic Comet 9P/Tempel 1 by the Alice ultraviolet spectrograph on the Rosetta spacecraft in conjunction with NASA's Deep Impact mission. Our objectives were to measure an increase in atomic and molecular emissions produced by the excavation of volatile sub-surface material. We unambiguously detected atomic oxygen emission from the quiescent coma but no enhancement at the 10% (1-σ) level following the impact. We derive a quiescent H₂O production rate of 9×¹⁰²⁷ molecules s⁻¹ with an estimated uncertainty of ∼30%. Our upper limits to the volatiles produced by the impact are consistent with other estimates.     

Structure and Evolution of White Dwarfs and their Interaction with the Local Interstellar Medium

The development of far-UV astronomy has been particularly important for the study of hot white dwarf stars. A significant fraction of their emergent flux appears in the far-UV and traces of elements heavier than hydrogen or helium are, in general, only detected in this waveband or at shorter wavelengths that are also only accessible from space. Although white dwarfs have been studied in the far-UV throughout the past ∼25 years, since the launch of IUE, only a few tens of objects have been studied in great detail and a much larger sample is required to gain a detailed understanding of the evolution of hot white dwarfs and the physical processes that determine their appearance. We review here the current knowledge regarding hot white dwarfs and outline what work needs to be carried out by future far-UV observatories.     

The icy Galilean satellites: ultraviolet phase curve analysis

Ultraviolet disk-integrated solar phase curves of the icy galilean satellites Europa, Ganymede, and Callisto are presented, using combined data sets from the International Ultraviolet Explorer (IUE), Hubble Space Telescope (HST), and the Galileo Ultraviolet Spectrometer. Global, disk-integrated solar phase curves for all three satellites, in addition to disk-integrated solar phase curves for Europa's leading, trailing, jovian, and anti-jovian hemispheres, are modeled using Hapke's equations for 7 broadband UV wavelengths between 260 and 320 nm. The sparse coverage in solar phase angle, particularly for Ganymede and Callisto, and the noise in the data sets poorly constrain some of the photometric parameter values in the model. However, the results are sufficient for forming a preliminary relationship between the effects of particle bombardment on icy surfaces and photometric scattering properties at ultraviolet wavelengths. Callisto exhibits a large UV opposition surge and a surface comprised of relatively low-backward scattering particles. Europa's surface displays a dichotomy between the jovian and anti-jovian hemispheres (the anti-jovian hemisphere is more backward scattering), while a less pronounced hemispherical variation was detected between the leading and trailing hemispheres. Europa's surface, with the exception of the trailing hemisphere region, appears to have become less backscattering between the late-1970s-early-1980s and the mid-1990s. These results are commensurate with the bombardment history of these surfaces by magnetospheric charged particles.