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381.
We present relative carbon and oxygen abundances derived via an optically thin recombination line analysis for five WO stars, and compare the derived abundances to recent evolutionary models. New recombination coefficients for O4+, O5+ and O6+ ions have allowed total oxygen abundances to be derived. The final C/He values range between 0.4 and 0.8 by number, consistent with C/He ratios previously derived for WC stars. O/He values range between 0.1–0.4, with C/O ratios between 2.1–4.8.A comparison of the derived abundances with the evolutionary models of Maeder (1990) and Schaller et al. (1992) shows promising agreement. We find reasonably tight agreement between the abundances derived for the WO stars. The degree of enhancement for the oxygen abundances in regions of low metallicity predicted by Maeder (1990) is not corroborated by our results.Additionally we present a revised, quantified classification scheme for WO subtypes. We extend the class to lower excitation, WO5, and place MS 4 (=WR 30a) in this class. Equivalent widths of the strongest lines of MS 4 are also presented. Finally, we present new observations of DR 1, a WO3 star located in the dwarf irregular galaxy IC 1613. 相似文献
382.
河北预算定额软件的开发应用 总被引:1,自引:0,他引:1
本文介绍了采用计算机对施工图预算进行电算化的软件系统。本文从该系统的特点、主要组成和设计思想等方面进行了论述,作为适用的商业应用软件,为社会和教学提供了有力的服务手段。 相似文献
383.
基于神经网络的仿真输出数据的分布识别 总被引:1,自引:0,他引:1
分布识别在仿真输出数据的分析中有着重要的理论和实际价值,但长期以来一直没有很好解决,在研究和改进神经网络的基础上,提出用多层感知机BP网格进行分布识别,给出了基于NN的分布识别模型,并进行了实验检验,实验结果表明本方法识别效率高,并具有很高的可靠性,可以辅助分析者作出准确的判断。 相似文献
384.
A. Herrero 《Space Science Reviews》1993,66(1-4):137-145
We present the results of our observations of stars of type O5 and earlier and show that inclusion of the line blocking between 228 and 912 A solves the problem found by Herrero et al. (1992) in the determination of their stellar parameters. We study the influence of the line blocking and other effects on the mass and helium discrepancies and show that the first one is reduced by the use of spherical, non hydrostatic model atmospheres and that the second one is probably due to exposure of CNO material.The INT is operated on the island of La Palma by the RGO in the Spanish Observatorio de El Roque de los Muchachos of the Instituto de Astrofsica de Canarias 相似文献
385.
文全兴 《华北航天工业学院学报》2001,(1)
本文介绍了液压缸在塑料模抽芯机构中的应用,论述了液压缸的选用、与型芯的连接形式。固定、及如何对液压缸提供液压油等液压缸使用的方法及应该注意的问题。 相似文献
386.
V.A. Kotov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2019,63(10):3385-3389
Time variations of the magnetic field of the Sun, seen as a star (the data 1968–2018, with more than 27 thousand daily measurements of the solar mean magnetic field), allowed to specify the rotation period of the gravitating solar mass: 27.027(6)?days, synodic. This indicates a presumably unknown physical connection between motions of the Sun and the Earth: in the course of a year our star accomplishes nearly 27 half-revolutions, while the planet itself performs an identical number of its spinnings during one complete axial revolution of the Sun. True origin of this strange Sun–Earth resonance is unknown, but it is supposed the phenomenon might be caused by slight coherent perturbations of gravity within the solar system. 相似文献
387.
Floris van der Tak 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
This paper contains a summary of the results from the first years of observations with the HIFI instrument onboard ESA’s Herschel space observatory. The paper starts by outlining the goals and possibilities of far-infrared and submillimeter astronomy, the limitations of the Earth’s atmosphere, and the scientific scope of the Herschel-HIFI mission. The presentation of science results from the mission follows the life cycle of gas in galaxies as grouped into five themes: Structure of the interstellar medium, First steps in interstellar chemistry, Formation of stars and planets, Solar system results and Evolved stellar envelopes. The HIFI observations paint a picture where the interstellar medium in galaxies has a mixed, rather than a layered structure; the same conclusion may hold for protoplanetary disks. In addition, the HIFI data show that exchange of matter between comets and asteroids with planets and moons plays a large role. The paper concludes with an outlook to future instrumentation in the far-infrared and submillimeter wavelength ranges. 相似文献
388.
389.
Francisco C.R. Fernandes José Augusto S.S. Dutra Rafael D. Cunha da Silva Hanumant S. Sawant 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
This work presents the analysis of five fine structures in the solar radio emission, observed between June 2000 and October 2001 by the Brazilian Solar Spectroscope (BSS), in the decimeter frequency band of 950–2500 MHz. Based on their morphological characteristics identified in the dynamic spectra, the fine structures had been classified as type U-like or type J-like bursts. Such emissions are variants of the type III bursts. They support the hypothesis of generation by plasma emission mechanism, from interaction of electron beams accelerated during solar flares, propagating along closed magnetic structures, within the trapped plasma of the solar corona. The spectral and temporal characteristics of the five fine structures had been obtained from the dynamic spectra and the parameters of the agent and the emitting source have been determined, assuming both fundamental and harmonic emissions. The analysis revealed the flux density of the structures is less than 20–80 s.f.u. For assumption of harmonic emission, the interval of values for the source parameters estimated are: the loop size is (0.3–5.1) × 1010 cm; the electron beam velocity is in the range of 0.16–0.53 c; the temperature of coronal loop top is of the order of (0.25–1.55) × 107 K; and the low limit for the magnetic field is of 7–26 G. These results are in agreement with previous determinations reported in the literature. 相似文献
390.
G.S. Suryanarayana K.M. Balakrishna 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(9):2482-2489
It is often noticed that the occurrence rate of Coronal Mass Ejections (CMEs) increases with increase in flare duration where peak flux too increase. However, there is no complete association between the duration and peak flux. Distinct characteristics have been reported for active regions (ARs) where flares and CMEs occur in contrast to ARs where flares alone occur. It is observed that peak flux of flares is higher when associated with CMEs compared to peak flux of flares with which CMEs are not associated. In other words, it is likely that flare duration and peak flux are independently affected by distinct active region dynamics. Hence, we examine the relative ability of flare duration and peak flux in enhancing the CME productivity. We report that CME productivity is distinctly higher in association with the enhancement of flare peak flux in comparison to corresponding enhancement of flare duration. 相似文献