Relative optical mass functions for air, water vapour, ozone and nitrogen dioxide in atmospheric models presenting different latitudinal and seasonal conditions     

C. Tomasi  V. Vitake  L. V. De Santis 《Meteorology and Atmospheric Physics》1998,65(1-2):11-30

Summary A study of the dependence features of the relative optical mass functions for air, water vapour, ozone and nitrogen dioxide on the apparent solar zenith angle was performed by calculating these optical parameters by means of the well-known computer code LOWTRAN 7 at several values of and for nine atmospheric models characterized by different latitudes and seasons. Moreover, other investigations were performed on the dependence features of (i) the relative optical air mass on the thermal characteristics of the low troposphere, (ii) the relative optical water vapour mass on the vertical distribution characteristics of absolute humidity in the troposphere, and (iii) the relative optical mass function for ozone and nitrogen dioxide on the shape characteristics of the vertical profiles of the two gaseous concentrations and the concentration peak altitudes. The results are compared with the values given by the two simple formulas proposed by Kasten (1966) for air and water vapour and the formulas defined by Young (1969) and Staehelin et al. (1995) for ozone and nitrogen dioxide. From this comparison, a wide set of correction factors were obtained which can be conveniently used in the analysis of multispectral sun-radiometric measurements for calculating, with a very high precision, the values of the four optical mass functions at all the angles in the 0° to 87° range, corresponding to the various latitudinal and seasonal conditions described by the nine atmospheric models.With 9 Figures  相似文献   

Validation of Ground-Based Visible Measurements of Total Ozone by Comparison with Dobson and Brewer Spectrophotometers     

M. Van Roozendael  P. Peeters  H. K. Roscoe  H. De Backer  A. E. Jones  L. Bartlett  G. Vaughan  F. Goutail  J.-P. Pommereau  E. Kyro  C. Wahlstrom  G. Braathen  P. C. Simon 《Journal of Atmospheric Chemistry》1998,29(1):55-83

Comparisons of total column ozone measurements from Dobson, Brewer and SAOZ instruments are presented for the period 1990 to 1995 at seven stations covering the mid- and the high northern latitudes, as well as the Antarctic region. The main purpose of these comparisons is to assess, by reference to the well established Dobson network, the accuracy of the zenith-sky visible spectroscopy for the measurement of total ozone. The strengths and present limitations of this latter technique are investigated. As a general result, the different instruments are found to agree within a few percent at all stations, the best agreement being obtained at mid-latitudes. On average, for the mid-latitudes, SAOZ O₃ measurements are approximately 2% higher than Dobson ones, with a scatter of about 5%. At higher latitudes, both scatter and systematic deviation tend to increase. In all cases, the relative differences between SAOZ and Dobson or Brewer column ozone are characterised by a significant seasonal signal, the amplitude of which increases from about 2.5% at mid-latitude to a maximum of 7.5% at Faraday, Antarctica. Although it introduces a significant contribution to the seasonality at high latitude, the temperature sensitivity of the O₃ absorption coefficients of the Dobson and Brewer instruments is shown to be too small to account for the observed SAOZ/Dobson differences. Except for Faraday, these differences can however be largely reduced if SAOZ AMFs are calculated with realistic climatological profiles of ozone, pressure and temperature. Other sources of uncertainties that might affect the comparison are investigated. Evidence is found that the differences in the air masses sampled by the SAOZ and the other instruments contribute significantly to the scatter, and the impact of the tropospheric clouds on SAOZ measurements is displayed.  相似文献   

Results from combining tectonic observations and SAR interferometry for the 1995 Grevena earthquake: A summary     

B. Meyer  R. Armijo  D. Massonnet  J. B. De Chabalier  C. Delacourt  J. C. Ruegg  J. Achache  D. Papanastassiou 《Journal of Geodynamics》1998,26(2-4)

Soon after the 1995 Grevena M_s = 6.6 event, we mapped the Palaeochori earthquake fault break. These tectonic observations are combined with the surface displacement field determined with the SAR interferometry to model the fault dislocation at depth.  相似文献   

Microdeformation of lacustrine laminite sequences from Late Miocene formations of SE Spain: an interpretation of loop bedding   总被引：2，自引：0，他引：2  

Jose P. Calvo  Miguel Rodriguez-Pascua  Silvia Martin-Velazquez  Sergio Jimenez  & Gerardo De Vicente 《Sedimentology》1998,45(2):279-292

Lacustrine laminated sediments (laminites) present in Late Miocene formations of the Híjar Basin, SE Spain, display well developed loop bedding, a structure consisting of bundles of laminae that are sharply constricted at intervals, giving a morphology of loops or links of a chain. The laminite sequences, which are interbedded with turbidite marlstones, were accumulated on the bottom of a permanently stratified lake developed in a rapidly subsiding basin limited by 010° and 105° normal faults. As deduced from both macro- and microdeformational analyses, the basin evolved under an extensional stress field throughout the Late Miocene. Four main types of loops, simple and complex loops with subcategories, have been recognized within the laminite sequence. Simple loops of type 1 show the best definite pattern, quite similar to ' pinch and swell structures ', a type of boudinage typical of stretching of alternating beds where the competence contrast is not strongly marked. The remaining loop types display contortion and occasional breakage of laminae (microfaulted edges) indicative of microdeformation near the boundary between the ductile-brittle deformational fields. The distribution of the various loop types across the laminite sequence reflects an interplay between progressive lithification of the laminites as sedimentation progressed and tectonic stresses which affected the sediment sequence. Accordingly, a mechanism of deformation under an extensional stress field, ultimately related to the creep movement of the main basin faults which resulted in successive seismic shocks of low magnitude, is proposed to explain the formation of loop bedding in the laminites.  相似文献   

Electronic and magnetic properties of a natural aegirine as observed from its Mössbauer spectra     

E. De Grave  A. Van Alboom  S. G. Eeckhout 《Physics and Chemistry of Minerals》1998,25(5):378-388

A natural sample of aegirine, ideally NaFeSi₂O₆, has been studied by transmission Mössbauer spectroscopy in the range 4.2–480?K. At selected temperatures, a longitudinal external field of 60?kOe was applied to the absorber. The sample was observed to order magnetically at 11±1?K. The paramagnetic Mössbauer spectra (MS) show the presence of ～10% Fe²⁺ in the M1 sites of the clinopyroxene structure. These MS have been decomposed into four quadrupole doublets: two minor ones for Fe²⁺ on M1 sites, a dominant one due to Fe³⁺ on M1 sites, and a second ferric component, with a contribution of ～3% and attributable to the tetrahedral sites. Two possibilities concerning the origin of the two distinct Fe²⁺ (M1) doublets are discussed. They are respectively based on inter-valence charge transfer and on the existence of distinct Fe²⁺ orbital configurations at the two M1 sites. Neither of the two models could be firmly excluded. The asymmetry parameter η of the electric field gradient at the Fe³⁺ (M1) sites is close to 1.0 and the quadrupole splitting within 0.34±0.01?mm/s at all temperatures. The MS at 4.2?K shows an asymmetric hyperfine-field distribution for Fe³⁺, with a maximum-probability field of 468?kOe. The maximum-probability field for Fe²⁺ is found to be 220?kOe. The shape of the applied-field MS at 4.2?K implies a static antiferromagnetic ordering and was successfully interpreted by a bidimensional distribution of the magnitude and orientation of the hyperfine field. Finally, the temperature variations of the respective centre shifts and quadrupole splittings could be explained on the basis of existing theoretical models.  相似文献   

Extragalactic source counts and contributions to the anisotropies of the cosmic microwave background: predictions for the Planck Surveyor mission     

Toffolatti  Argüeso Gómez  De Zotti  Mazzei  Franceschini  Danese  & Burigana 《Monthly notices of the Royal Astronomical Society》1998,297(1):117-127

We present predictions for the counts of extragalactic sources, the contributions to fluctuations and their angular power spectrum in each channel foreseen for the Planck Surveyor (formerly COBRAS/SAMBA ) mission. The contribution to fluctuations owing to clustering of both radio and far-IR sources is found to be generally small in comparison with the Poisson term; however the relative importance of the clustering contribution increases and may eventually become dominant if sources are identified and subtracted down to faint flux limits. The central Planck frequency bands are expected to be 'clean': at high galactic latitude (| b | > 20°), where the reduced galactic noise does not prevent the detection of the extragalactic signal, only a tiny fraction of pixels is found to be contaminated by discrete extragalactic sources. Moreover, the 'flat' angular power spectrum of fluctuations resulting from extragalactic sources substantially differs from that of primordial fluctuations; therefore, the removal of contaminating signals is eased even at frequencies where point sources give a sizeable contribution to the foreground noise.  相似文献   

Contribution of galaxies to the background hydrogen-ionizing flux     

Julien E. G. Devriendt  Shiv K. Sethi  Bruno Guiderdoni  & Biman B. Nath 《Monthly notices of the Royal Astronomical Society》1998,298(3):708-718

We estimate the evolution of the contribution of galaxies to the cosmic background flux at 912 Å by means of a semi-analytic model of galaxy formation and evolution. Such modelling has been quite successful in reproducing the optical properties of galaxies. We assume that high-redshift damped Lyman α systems are the progenitors of present-day galaxies, and we design a series of models that are consistent with the evolution of cosmic comoving emissivities in the available near-infrared, optical, ultraviolet and far-infrared bands along with the evolution of the neutral hydrogen content and average metallicity of damped Lyman α systems. We use these models to compute the galactic contribution to the Lyman-limit emissivity and background flux for 0 ≃  z  ≤ 4. We take into account the absorption of Lyman-limit photons by H  I and dust in the interstellar medium of the galaxies. We find that the background Lyman-limit flux due to galaxies might dominate (or be comparable to) the contribution from quasars at almost all redshifts if the absorption by H  I in the interstellar medium is neglected. Such H  I absorption would result in a severe diminishing of this flux — by almost three orders of magnitude at high redshifts and by one to two orders at z  ≃ 0. Though the resulting galaxy flux is completely negligible at high redshifts, it is comparable to the quasar flux at z  ≃ 0.  相似文献   

Quantitative classification of WC and WO stars     

Crowther  Orsola De Marco  & Barlow 《Monthly notices of the Royal Astronomical Society》1998,296(2):367-378

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Effect of Spectral Resolution on the Mg II Index as a Measure of Solar Variability     

Oran R. White  Giuliana De Toma  Gary J. Rottman  Thomas N. Woods  Barry G. Knapp 《Solar physics》1998,177(1-2):89-103

The solar Mgii core-to-wing ratio is a useful index of UV variability throughout the solar cycle because it has been measured since 1978 in a series of successive satellite missions: Nimbus 7, Solar Mesosphere Explorer (SME), the NOAA 9–14 series, Upper Atmosphere Research Satellite (UARS), and ERS-2. Eventual construction of a single time series from 1978 to the present by combining these measurements will give a long record of almost daily UV variability to serve as a surrogate for estimating both UV and EUV solar radiation. Here we address the effect of spectral resolution on determination of both long-term and short-term solar variability from this index. We use UARS/SOLSTICE measurements of the Mgii line from October 1991 to December 1996 to study the effect of two spectral resolution regimes characteristic of existing measurements, 0.20 to 0.25 nm and 1.10 to 1.15 nm, on determination of the amplitude of 27-day rotational modulation and the more gradual change in chromospheric radiation in the declining phase of solar cycle 22. The two Mgii indices give solar variations that differ by a scaling factor of 2× for both the solar cycle change from 1992 to 1997 and the amplitude of 27-day modulation over the same period. Both types of measurements appear to yield solar signal equally well except at solar minimum when the solar changes become quite small.  相似文献   

CDM models with a BSI step-like primordial spectrum and a cosmological constant     

Julien Lesgourgues  D. Polarski  & A. A. Starobinsky 《Monthly notices of the Royal Astronomical Society》1998,297(3):769-776

A class of spatially flat models with cold dark matter (CDM), a cosmological constant and a broken-scale-invariant (BSI) step-like primordial (initial) spectrum of adiabatic perturbations, generated in an exactly solvable inflationary model where the inflaton potential has a rapid change of its first derivative at some point, is confronted with existing observational data on angular fluctuations of the CMB temperature, galaxy clustering and peculiar velocities of galaxies. If we locate the step in the initial spectrum at k  ≃ 0.05  h Mpc⁻¹, where a feature in the spectrum of Abell clusters of galaxies was found that could reflect a property of the initial spectrum, and if the large-scale flat plateau of the spectrum is normalized according to the COBE data, the only remaining parameter of the spectrum is p — the ratio of amplitudes of the metric perturbations between the small-scale and large-scale flat plateaux. Allowed regions in the plane of parameters (Ω = 1 − Ω_Λ,  H ₀) satisfying all data have been found for p lying in the region (0.8–1.7). Especially good agreement of the form of the present power spectrum in this model with the form of the cluster power spectrum is obtained for the inverted step ( p  < 1,  p  = 0.7–0.8), when the initial spectrum has slightly more power on small scales.  相似文献