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991.
We present survey data in the narrow-band L filter (nb L ), taken at UKIRT, for a total area of 277 arcmin2 , roughly equally divided between four regions at zero Galactic latitude and longitudes ±4.°3 and ±2.°3. The 80 per cent completeness level for these observations is at roughly magnitude 11.0. This magnitude limit, owing to the low coefficient for interstellar extinction at this wavelength ( A nb L =0.047 AV ), allows us to observe bulge giants. We match the nb L magnitudes with DENIS survey K magnitudes, and find 95 per cent of nb L sources are matched to K sources. Constructing colour–magnitude diagrams, we deredden the magnitudes and find evidence for a longitude-dependent asymmetry in the source counts. We find that there are ∼15 per cent and ∼5 per cent more sources at the negative longitude than at the corresponding positive longitude for the fields at ±4.°3 and ±2.°3, respectively. This is compared with the predictions of some Galactic bar models. We find an asymmetry in the expected sense, which favours gas dynamical models and the recent deconvolution of surface photometry data over earlier treatments of photometric data. 相似文献
992.
Warell Johan LAGERKVIST CLAES-INGVAR Lageros JOHAN S. V. 《Earth, Moon, and Planets》1997,78(1-3):197-203
Dust continuum imaging of comet C/1995 O1 (Hale-Bopp) was carried out with the Swedish Vacuum Solar Telescope (SVST)on La
Palma in April, 1997. Images were reduced according to standard procedure, aligned, averaged, navigated and enhanced with
azimuthal renormalization, rotational derivative, temporal derivative and unsharp masking processing.
The rotational period of the nucleus was determined to 11.5 h and the mean projected dust outflow velocity to 0.41 km s−1. Shell envelopes in the sunward side of the coma were separated by a projected distance of ∼15 000–20 000 km and spiralling
inwards towards smaller radii in the direction of local evening. Small scale inhomogeneities of size 1 000–2 000 km, interpreted
as correlated with variations in dust emission activity, were seen at radii ≤20 000 km. Two overlapping shell systems with
a relative lag angle of ∼55° were evident at the time.
The north pole of the nucleus was directed towards the Earth. The dust emission pattern is very complex and may be due to
several active areas. The shape of the incomplete spiral shell pattern indicates that the angle between the line-of-sight
and the rotational axis of the nucleus was not large.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
993.
P. Jakobsson G. Björnsson J. P. U. Fynbo G. Jóhannesson J. Hjorth B. Thomsen P. Møller D. Watson B. L. Jensen G. Östlin J. Gorosabel E. H. Gudmundsson 《Monthly notices of the Royal Astronomical Society》2005,362(1):245-251
We report the result of a search for Lyα emission from the host galaxies of the gamma-ray bursts (GRBs) 030226 ( z = 1.986), 021004 ( z = 2.335) and 020124 ( z = 3.198) . We find that the host galaxy of GRB 021004 is an extended (around 8 kpc) strong Lyα emitter with a rest-frame equivalent width (EW) of 68+12 −11 Å, and a star formation rate of 10.6 ± 2.0 M⊙ yr−1 . We do not detect the hosts of GRB 030226 and GRB 020124, but the upper limits on their Lyα fluxes do not rule out large rest-frame EWs. In the fields of GRB 021004 and GRB 030226 we find seven and five other galaxies, respectively, with excess emission in the narrow-band filter. These galaxies are candidate Lyα-emitting galaxies in the environment of the host galaxies. We have also compiled a list of all z ≳ 2 GRB hosts, and demonstrate that a scenario where they trace star formation in an unbiased way is compatible with current observational constraints. Fitting the z = 3 luminosity function (LF) under this assumption results in a characteristic luminosity of R *= 24.6 and a faint-end slope of α=−1.55 , consistent with the LF measured for Lyman-break galaxies. 相似文献
994.
Hiroyuki Hirashita Huirong Yan 《Monthly notices of the Royal Astronomical Society》2009,394(2):1061-1074
We investigate shattering and coagulation of dust grains in turbulent interstellar medium (ISM). The typical velocity of dust grain as a function of grain size has been calculated for various ISM phases based on a theory of grain dynamics in compressible magnetohydrodynamic turbulence. In this paper, we develop a scheme of grain shattering and coagulation and apply it to turbulent ISM by using the grain velocities predicted by the above turbulence theory. Since large grains tend to acquire large velocity dispersions as shown by earlier studies, large grains tend to be shattered. Large shattering effects are indeed seen in warm ionized medium within a few Myr for grains with radius a ≳ 10−6 cm. We also show that shattering in warm neutral medium can limit the largest grain size in ISM ( a ∼ 2 × 10−5 cm) . On the other hand, coagulation tends to modify small grains since it only occurs when the grain velocity is small enough. Coagulation significantly modifies the grain size distribution in dense clouds (DC), where a large fraction of the grains with a < 10−6 cm coagulate in 10 Myr. In fact, the correlation among RV , the carbon bump strength and the ultraviolet slope in the observed Milky Way extinction curves can be explained by the coagulation in DC. It is possible that the grain size distribution in the Milky Way is determined by a combination of all the above effects of shattering and coagulation. Considering that shattering and coagulation in turbulence are effective if dust-to-gas ratio is typically more than ∼1/10 of the Galactic value, the regulation mechanism of grain size distribution should be different between metal-poor and metal-rich environments. 相似文献
995.
996.
Yang Liu Darren W. Schnare Benjamin C. Eimer Lawrence A. Taylor 《Planetary and Space Science》2008,56(11):1517-1523
In order to study the toxicity of lunar dust, the respirable size fraction of lunar soil needed to be separated with an apparatus that possesses the following capabilities: no use of liquid; fully recoverable sample; and use of only small sample quantities (<1 gm). We report the design of a simple apparatus that meets these requirements and implements an inertial-impaction mechanism established in aerosol science. Lunar soil was agitated at a frequency of 100 Hz using a vibration table with a containment chamber under a constant air flow. The air flow carried the lofted lunar dust particles past four impactors (four T-junction connectors), upon which a fraction of large particles were captured during the impaction. The fine particles in the air flow were then collected by an end-of-the line membrane filter. Detailed examination of particles on the filter showed that the majority (∼80-90 wt%) are <3 μm (geometric diameter), suggesting a high level of effectiveness for the apparatus. 相似文献
997.
Helen J. Fraser Suzanne E. Bisschop Klaus M. Pontoppidan Alexander G. G. M. Tielens Ewine F. van Dishoeck 《Monthly notices of the Royal Astronomical Society》2005,356(4):1283-1292
A solid-state feature was detected at around 2175 cm−1 towards 30 embedded young stellar objects in spectra obtained using the Infrared Spectrometer and Array Camera at the European Southern Observatory Very Large Telescope. We present results from laboratory studies of CO adsorbed at the surface of zeolite wafers, where absorption bands were detected at 2177 and 2168 cm−1 (corresponding to CO chemisorbed at the zeolite surface) and 2130 cm−1 (corresponding to CO physisorbed at the zeolite surface), providing an excellent match to the observational data. We propose that the main carrier of the 2175-band is CO chemisorbed at bare surfaces of dust grains in the interstellar medium. This result provides the first direct evidence that gas–surface interactions do not have to result in the formation of ice mantles on interstellar dust. The strength of the 2175-band is estimated to be ∼4 × 10−19 cm molecule−1 . The abundance of CO adsorbed at bare grain surfaces ranges from 0.06 to 0.16 relative to H2 O ice, which is, at most, half of the abundance (relative to H2 O ice) of CO residing in H2 O-dominated ice environments. These findings imply that interstellar grains have a large (catalytically active) surface area, providing a refuge for interstellar species. Consequently, the potential exists for heterogeneous chemistry to occur involving CO molecules in unique surface chemistry pathways not currently considered in gas grain models of the interstellar medium. 相似文献
998.
999.
1000.
黄土中石英的含量与结晶度指数的测定 总被引:2,自引:0,他引:2
碎屑石英是风成黄土最主要的组成矿物,其结晶度指数与粉尘源区石英的母岩类型有关,其含量则可用于估算风尘通量变化进而恢复源区的干旱化历史。通过详细的探讨,揭示了测试条件及数据处理方法对石英含量和结晶度指数估算的可能影响。结果表明:(1)测量石英结晶度指数时扫描的步长和速度有别于测量石英含量时的参数设置;(2)数据处理时,先对数据进行人工手动扣除背景,结晶度指数要依据衍射图谱67.74°处和67.85°处的峰谷值进行估算,而石英含量的估算主要依据衍射图谱中20.9°处石英峰与28.4°处硅粉峰;(3)石英结晶度指数需要反复压片测量多次取平均值。 相似文献