A homogeneous sample of sub-damped Lyman     systems – IV. Global metallicity evolution     

Céline Péroux  Miroslava Dessauges-Zavadsky  Sandro D'Odorico  Tae-Sun Kim  Richard G. McMahon 《Monthly notices of the Royal Astronomical Society》2007,382(1):177-193

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A possible EGRET source with a two-sided radio jet structure on a parsec scale – 3EG J0808+5114     

Yongjun Chen  Minfeng Gu  Zhi-Qiang Shen  Zhonghui Fan 《Monthly notices of the Royal Astronomical Society》2006,370(4):1885-1892

Recent observations have revealed that damped Lyα clouds (DLAs) host star formation activity. In order to examine if such star formation activity can be triggered by ionization fronts, we perform high-resolution hydrodynamics and radiative transfer simulations of the effect of radiative feedback from propagating ionization fronts on high-density clumps. We examine two sources of ultraviolet (UV) radiation field to which high-redshift ( z ∼ 3) galaxies could be exposed: one corresponding to the UV radiation originating from stars within the DLA, itself, and the other corresponding to the UV background radiation. We find that, for larger clouds, the propagating I-fronts created by local stellar sources can trigger cooling instability and collapse of significant part, up to 85 per cent, of the cloud, creating conditions for star formation in a time-scale of a few Myr. The passage of the I-front also triggers collapse of smaller clumps (with radii below ∼4 pc), but in these cases the resulting cold and dense gas does not reach conditions conducive to star formation. Assuming that 85 per cent of the gas initially in the clump is converted into stars, we obtain a star formation rate of  ∼0.25 M_⊙ yr⁻¹ kpc⁻²  . This is somewhat higher than the value derived from recent observations. On the other hand, the background UV radiation which has harder spectrum fails to trigger cooling and collapse. Instead, the hard photons which have long mean free-path heat the dense clumps, which as a result expand and essentially dissolve in the ambient medium. Therefore, the star formation activity in DLAs is strongly regulated by the radiative feedback, both from the external UV background and internal stellar sources and we predict quiescent evolution of DLAs (not starburst-like evolution).  相似文献   

Key problems in cool-star astrophysics     

Isabella Pagano  Thomas R. Ayres  Alessandro C. Lanzafame  Jeffrey L. Linsky  Benjamín Montesinos  Marcello-Rodonò 《Astrophysics and Space Science》2006,303(1-4):17-31

Selected key problems in cool-star astrophysics are reviewed, with emphasis on the importance of new ultraviolet missions to tackle the unresolved issues.UV spectral signatures are an essential probe of critical physical processes related to the production and transport of magnetic energy in astrophysical plasmas ranging, for example, from stellar coronae, to the magnetospheres of magnetars, and the accretion disks of protostars and Active Galactic Nuclei. From an historical point of view, our comprehension of such processes has been closely tied to our understanding of solar/stellar magnetic activity, which has its origins in a poorly understood convection-powered internal magnetic dynamo. The evolution of the Sun's dynamo, and associated magnetic activity, affected the development of planetary atmospheres in the early solar system, and the conditions in which life arose on the primitive Earth. The gradual fading of magnetic activity as the Sun grows old likewise will have profound consequences for the future heliospheric environment. Beyond the Sun, the magnetic activity of stars can influence their close-in companions, and vice versa.Cool star outer atmospheres thus represent an important laboratory in which magnetic activity phenomena can be studied under a wide variety of conditions, allowing us to gain insight into the fundamental processes involved. The UV range is especially useful for such studies because it contains powerful diagnostics extending from warm (∼ 10⁴ K) chromospheres out to hot (1–10 MK) coronae, and very high-resolution spectroscopy in the UV has been demonstrated by the GHRS and STIS instruments on HST but has not yet been demonstrated in the higher energy EUV and X-ray bands. A recent example is the use of the hydrogen Lyα resonance line—at 110 000 resolution with HST STIS—study, for the first time, coronal winds from cool stars through their interaction with the interstellar gas. These winds cannot be detected from the ground, for lack of suitable diagnostics; or in the X-rays, because the outflowing gas is too thin.A 2m class UV space telescope with high resolution spectroscopy and monitoring capabilities would enable important new discoveries in cool-star astronomy among the stars of the solar neighborhood out to about 150 pc. A larger aperture facility (4–6 m) would reach beyond the 150 pc horizon to fainter objects including young brown dwarfs and pre-main sequence stars in star-forming regions like Orion, and magnetic active stars in distant clusters beyond the Pleiades and α Persei. This would be essential, as well, to characterize the outer atmospheres of stars with planets, that will be discovered by future space missions like COROT, Kepler, and Darwin.Deceased October 23, 2005  相似文献   

The matter power spectrum from the Lyα forest: an optical depth estimate     

S. Zaroubi  M. Viel  A. Nusser  M. Haehnelt  T.-S. Kim 《Monthly notices of the Royal Astronomical Society》2006,369(2):734-750

We measure the matter power spectrum from 31 Lyα spectra spanning the redshift range of 1.6–3.6. The optical depth, τ, for Lyα absorption of the intergalactic medium is obtained from the flux using the inversion method of Nusser & Haehnelt. The optical depth is converted to density by using a simple power-law relation,  τ∝ (1 +δ)^α  . The non-linear 1D power spectrum of the gas density is then inferred with a method that makes simultaneous use of the one- and two-point statistics of the flux and compared against theoretical models with a likelihood analysis. A cold dark matter model with standard cosmological parameters fits the data well. The power-spectrum amplitude is measured to be (assuming a flat Universe),  σ₈= (0.92 ± 0.09) × (Ω_m/0.3)^−0.3  , with α varying in the range of 1.56–1.8 with redshift. Enforcing the same cosmological parameters in all four redshift bins, the likelihood analysis suggests some evolution in the temperature–density relation and the thermal smoothing length of the gas. The inferred evolution is consistent with that expected if reionization of He  ii occurred at   z ∼ 3.2  . A joint analysis with the Wilkinson Microwave Anisotropy Probe results together with a prior on the Hubble constant as suggested by the Hubble Space Telescope key project data, yields values of Ω_m and σ₈ that are consistent with the cosmological concordance model. We also perform a further inversion to obtain the linear 3D power spectrum of the matter density fluctuations.  相似文献   

Fluorescent Lyman α emission from gas near a QSO at redshift 4.28     

Paul J. Francis  Sunsanee McDonnell 《Monthly notices of the Royal Astronomical Society》2006,370(3):1372-1378

We use integral field spectroscopy with the Gemini North Telescope to detect probable fluorescent Lyman α (Lyα) emission from gas lying close to the luminous QSO PSS 2155+1358 at redshift 4.28. The emission is most likely coming not from primordial gas, but from a multiphase, chemically enriched cloud of gas lying about 50 kpc from the QSO. It appears to be associated with a highly ionized associated absorber seen in the QSO spectrum. With the exception of this gas cloud, the environment of the QSO is remarkably free of neutral hydrogen. We also marginally detect Lyα emission from a foreground subdamped Lyα absorption-line system.  相似文献   

Probing radio source environments via H i and OH absorption     

Neeraj Gupta  C. J. Salter  D. J. Saikia  T. Ghosh  S. Jeyakumar 《Monthly notices of the Royal Astronomical Society》2006,373(3):972-992

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原子吸收分光光度法测定肉类样品中微量的铜铅锌镉     

娄元礼  李明福 《河南国土资源》1997,(4)

采用原子吸收法对肉类样品微量铜铅锌镉进行测定，重点对样品的前处理进行实验，拟订测试操作规程和仪器测量最佳条件，实验证明本法操作简便，准确快速，结果满意。  相似文献   

The mysterious absence of neutral hydrogen within 1 Mpc of a luminous quasar at redshift 2.168     

Paul J. Francis  Joss Bland-Hawthorn 《Monthly notices of the Royal Astronomical Society》2004,353(1):301-309

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制作包括吸收和波散效应的VSP合成记录     

高静怀  王玉贵 《地球科学与环境学报》1991,(2)

在地球物理勘探中,岩性勘探已成为很受重视的研究课题。Q值测井是确定地下岩性的一种方法,而制做包括吸收和波散效应的VSP合成记录是利用VSP资料做Q值测井的一个重要方面。本文详细地介绍了包括吸收和波散效应的VSP合成记录的具体制作过程,附有程序框图。本文还对震源不在地表时如何修正进行了分析,在此基础上把震源在地表和震源在任意深度两种情况统一起来,用同一公式表达。  相似文献   

P-wave coda analysis of short-period array data and the scattering and absorptive properties of the lithosphere   总被引：1，自引：0，他引：1  

Michael Korn 《Geophysical Journal International》1988,93(3):437-449

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