祁连山夏季地形云综合探测试验   总被引：1，自引：0，他引：1  

郑国光  陈跃  陈添宇  陈乾  朱君鉴  李照荣 《地球科学进展》2011,26(10):1057-1070

2006年和2007年夏季在祁连山冷龙岭西段开展了地形云云量、云状、大气水汽、风场、雨滴谱和雨强等的综合探测试验,以分析祁连山地形云的特征。结果表明：①祁连山区夏季云量丰富,平均云量在6成以上。西南气流天气背景下总云量多达8成;②祁连山夏季无降水日大气水汽非常少,700 hPa以上层大气相对湿度大多在20%以下;③西南气流背景下祁连山南北侧山谷风的共同作用,气流昼间向山顶辐合,夜间向山谷辐散,当水汽条件充足时,极易抬升形成可以产生降水的地形云;④祁连山降水主要由小于1 mm的雨滴组成。  相似文献   

Twenty-five years of spectral UV-B measurements over Canada,Europe and Japan: Trends and effects from changes in ozone,aerosols, clouds,and surface reflectivity     

《Comptes Rendus Geoscience》2018,350(7):393-402

Spectral UV records of solar irradiance at stations over Europe, Canada, and Japan were used to study long-term trends at 307.5 nm for a 25-year period, from 1992 to 2016. Ground-based measurements of total ozone, as well as satellite measurements of the Aerosol Index, the Total Cloud Cover and the surface reflectivity were also used in order to attribute the estimated changes of the UV to the corresponding changes of these factors. The present study shows that over the Northern Hemisphere, the long-term changes in UV-B radiation reaching the Earth's surface vary significantly over different locations, and that the main drivers of these variations are changes in aerosols and total ozone. At high latitudes, part of the observed changes may also be attributed to changes in the surface reflectivity. Over Japan, the UV-B irradiance at 307.5 nm has increased significantly by ∼3%/decade during the past 25 years, possibly due to the corresponding significant decrease of its absorption by aerosols. It was found that the greatest part of this increase took place before the mid-2000s. The only European station, over which UV radiation increases significantly, is that of Thessaloniki, Greece. Analysis of the clear-sky irradiance for the particular station shows increasing irradiance at 307.5 nm by ∼3.5%/decade during the entire period of study, with an increasing rate of change during the last decade, possibly again due to the decreasing absorption by aerosols.  相似文献   

The Magellanic Clouds: their evolution,structure and composition     

B. E. Westerlund 《Astronomy and Astrophysics Review》1990,2(1):29-78

Summary The Magellanic Clouds play a fundamental role in a number of fields of astronomical research. Their distances are most relevant to the extragalactic distance scale. Their relative proximity offers exceptional opportunities for detailed studies of their stellar and interstellar content. They serve therefore as testing grounds for modern astrophysical theories, in particular concerning the chemical evolution of stars and galaxies.In this review we will discuss recent attempts to determine accurate distances to the Magellanic Clouds. We will consider their stellar generations as the results of interactions between the Large and the Small Magellanic Cloud as well as between the Clouds and the Galaxy. Recent determinations of the chemical abundances of the various age groups will be presented. The fact that the evolution of the Clouds has been slower than that of our Galaxy gives us the opportunity to study the conditions in slightly metalpoor galaxies. Recent progress in observing techniques has added much to our knowledge about the interstellar medium of the Clouds.The Magellanic System, which comprises the Magellanic Clouds, the Inter-Cloud Region and the Magellanic Stream, will be described. We will in particular consider the complex structure of the Large and the Small Cloud and the kinematics of their populations.  相似文献   

SPB stars in the open SMC cluster NGC 371     

C. Karoff  T. Arentoft  L. Glowienka  C. Coutures  T. B. Nielsen  G. Dogan  F. Grundahl  H. Kjeldsen 《Monthly notices of the Royal Astronomical Society》2008,386(2):1085-1091

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Optical follow-up of new Small Magellanic Cloud wing Be/X-ray binaries     

M. P. E. Schurch  M. J. Coe  K. E. McGowan  V. A. McBride  D. A. H. Buckley  J. L. Galache  R. H. D. Corbet  M. Still  P. Vaisanen  A. Kniazev  K. Nordsieck 《Monthly notices of the Royal Astronomical Society》2007,381(4):1561-1568

We investigate the optical counterparts of recently discovered Be/X-ray binaries in the Small Magellanic Cloud (SMC). In total four sources, SXP101, SXP700, SXP348 and SXP65.8 were detected during the Chandra survey of the wing of the SMC. SXP700 and SXP65.8 were previously unknown. Many optical ground-based telescopes have been utilized in the optical follow-up, providing coverage in both the red and blue bands. This has led to the classification of all of the counterparts as Be stars and confirms that three lie within the Galactic spectral distribution of known Be/X-ray binaries. SXP101 lies outside this distribution and is the latest spectral type known. Monitoring of the Hα emission line suggests that all the sources barring SXP700 have highly variable circumstellar discs, possibly a result of their comparatively short orbital periods. Phase-resolved X-ray spectroscopy has also been performed on SXP65.8, revealing that the emission is indeed harder during the passage of the X-ray beam through the line of sight.  相似文献   

Five young star clusters in the outer region of the Small Magellanic Cloud     

Andrés E. Piatti  Ata Sarajedini  Doug Geisler  Carme Gallart  Marina Wischnjewsky† 《Monthly notices of the Royal Astronomical Society》2007,382(3):1203-1212

Colour–magnitude diagrams in the Washington system are presented for the first time for five star clusters projected on to the outer region of the Small Magellanic Cloud (SMC). The clusters are found to have ages in the range 0.1–1.0 Gyr, as derived from the fit of isochrones with   Z = 0.004  . This sample increases substantially the number of young clusters in the outer SMC – particularly in the south-east quadrant – with well-derived parameters. We combine our results with those for other clusters in the literature to derive as large and homogeneous a data base as possible (totalling 49 clusters) in order to study global effects. We find no conclusive evidence for a dispersion in the cluster ages and metallicities as a function of their distance from the galaxy centre, in the SMC outer region. L 114 and 115, although very distant, are very young clusters, lying in the bridge of the SMC and therefore most likely formed during the interaction which formed this feature. We also find very good agreement between the cluster age–metallicity relation (AMR) and the prediction from a bursting model from Pagel & Tautvaišienė with a burst that occurred 3 Gyr ago. Comparing the present cluster AMR with that derived by Harris & Zaritsky for field stars in the main body of the SMC, we find that field stars and clusters underwent similar chemical enrichment histories during approximately the last couple of Gyr, but their chemical evolution was clearly different between 4 and 10 Gyr ago.  相似文献   

Cepheid parallaxes and the Hubble constant   总被引：1，自引：0，他引：1  

Floor van Leeuwen  Michael W. Feast  Patricia A. Whitelock  Clifton D. Laney 《Monthly notices of the Royal Astronomical Society》2007,379(2):723-737

Revised Hipparcos parallaxes for classical Cepheids are analysed together with 10 Hubble Space Telescope ( HST )-based parallaxes. In a reddening-free V , I relation we find that the coefficient of log  P is the same within the uncertainties in our Galaxy as in the Large Magellanic Cloud (LMC), contrary to some previous suggestions. Cepheids in the inner region of NGC 4258 with near solar metallicities confirm this result. We obtain a zero-point for the reddening-free relation and apply it to the Cepheids in galaxies used by Sandage et al. to calibrate the absolute magnitudes of Type Ia supernova (SNIa) and to derive the Hubble constant. We revise their result for H ₀ from 62 to 70 ± 5 km s⁻¹ Mpc⁻¹. The Freedman et al. value is revised from 72 to 76 ± 8 km s⁻¹ Mpc⁻¹. These results are insensitive to Cepheid metallicity corrections. The Cepheids in the inner region of NGC 4258 yield a modulus of 29.22 ± 0.03 (int.) compared with a maser-based modulus of 29.29 ± 0.15. Distance moduli for the LMC, uncorrected for any metallicity effects, are 18.52 ± 0.03 from a reddening-free relation in V , I ; 18.47 ± 0.03 from a period–luminosity relation at K ; 18.45 ± 0.04 from a period–luminosity–colour relation in J , K . Adopting a metallicity correction in V , I from Macri et al. leads to a true LMC modulus of 18.39 ± 0.05.  相似文献   

X-ray bright sources in the Chandra Small Magellanic Cloud Wing Survey – detection of two new pulsars     

K. E. McGowan  M. J. Coe  M. Schurch  V. A. McBride  J. L. Galache  W. R. T. Edge  R. H. D. Corbet  S. Laycock  A. Udalski  D. A. H. Buckley 《Monthly notices of the Royal Astronomical Society》2007,376(2):759-770

We investigate the X-ray and optical properties of a sample of X-ray bright sources from the Small Magellanic Cloud (SMC) Wing Survey. We have detected two new pulsars with pulse periods of 65.8 s (CXOU J010712.6−723533) and 700 s (CXOU J010206.6−714115), and present observations of two previously known pulsars RX J0057.3−7325 (SXP101) and SAX J0103.2−7209 (SXP348). Our analysis has led to three new optical identifications for the detected pulsars. We find long-term optical periods for two of the pulsars, CXOU J010206.6−714115 and SXP101, of 267 and 21.9 d, respectively. Spectral analysis of a subset of the sample shows that the pulsars have harder spectra than the other sources detected. By employing a quantile-based colour–colour analysis we are able to separate the detected pulsars from the rest of the sample. Using archival catalogues we have been able to identify counterparts for the majority of the sources in our sample. Combining this with our results from the temporal analysis of the Chandra data and archival optical data, the X-ray spectral analysis, and by determining the X-ray to optical flux ratios we present preliminary classifications for the sources. In addition to the four detected pulsars, our sample includes two candidate foreground stars, 12 probable active galactic nuclei, and five unclassified sources.  相似文献   

How well do we know the age and mass distributions of the star cluster system in the Large Magellanic Cloud?     

Richard de Grijs  Peter Anders 《Monthly notices of the Royal Astronomical Society》2006,366(1):295-307

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CCD photometry of variable stars in the Magellanic Clouds – VII. The eclipsing binaries MACHO*05:36:48.7−69:17:00 in the LMC, and MOA J005018.4−723855 and J005623.5−722123 in the SMC     

G. P. Bayne  W. Tobin  J. D. Pritchard  K. R. Pollard  M. D. Albrow 《Monthly notices of the Royal Astronomical Society》2004,349(3):833-840

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