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961.
The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements
relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this
mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements,
there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition
resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison
et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar
and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize
and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
962.
Mahaffy P.R. Donahue T.M. Atreya S.K. Owen T.C. Niemann H.B. 《Space Science Reviews》1998,84(1-2):251-263
The Galileo Probe Mass Spectrometer measurements in the atmosphere of Jupiter give D/H = (2.6 ± 0.7) × 10-5 3He/4He = (1.66 ± 0.05) × 10-4These ratios supercede earlier results by Niemann et al. (1996) and are based on a reevaluation of the instrument response at high count rates and a more detailed study of the contributions of different species to the mass peak at 3 amu. The D/H ratio is consistent with Voyager and ground based data and recent spectroscopic and solar wind (SW) values obtained from the Infrared Spectroscopic Observatory (ISO) and Ulysses. The 3He/4He ratio is higher than that found in meteoritic gases (1.5 ± 0.3) × 10-4. The Galileo result for D/H when compared with that for hydrogen in the local interstellar medium (1.6 ± 0.12) × 10-5 implies a small decrease in D/H in this part of the universe during the past 4.55 billion years. Thus, it tends to support small values of primordial D/H - in the range of several times 10-5 rather than several times 10-4. These results are also quite consistent with no change in (D+3He)/H during the past 4.55 billion years in this part of our galaxy. 相似文献
963.
John C. Raymond Raid Suleiman John L. Kohl Giancarlo Noci 《Space Science Reviews》1998,85(1-2):283-289
A great deal of evidence for elemental abundance variations among different structures in the solar corona has accumulated
over the years. Many of the observations show changes in the relative abundances of high- and low-First Ionization Potential
elements, but relatively few show the absolute elemental abundances. Recent observations from the SOHO satellite give absolute
abundances in coronal streamers. Along the streamer edges, and at low heights in the streamer, they show roughly photospheric
abundances for the low-FIP elements, and a factor of 3 depletion of high-FIP elements. In the streamer core at 1.5 R·, both
high- and low-FIP elements are depleted by an additional factor of 3, which appears to result from gravitational settling.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
964.
965.
为了获得某高温升燃烧室副喷嘴性能及其与喷口尺寸的相互关系,通过试验研究了供油压力和离心喷嘴的关键结构参
数对燃油流量、喷雾锥角和雾化性能的影响。研究的关键参数有喷口长度与喷口直径,采用3维相位多普勒粒子分析仪测量了某
一直线上各点的数密度分布,以及R-R(Rosin-Rammler)分布的特征直径D 和均匀度指数N。结果表明:在供油压力为164~3350
kPa的条件下,燃油流量和喷雾锥角随喷口长径比(旋流室与喷口直径比不变)和旋流室与喷口直径比(喷口长径比不变)的增大
而减小,增大喷口长径比和减小旋流室与喷口直径比可改善雾化效果。研究获得的规律为三旋流高温升燃烧室喷嘴优化设计提
供了重要的理论依据。 相似文献
966.
为探究低展弦比压气机转子在风车状态下由压气机模式向涡轮模式转化过程中性能、内部流场结构以及气动损失的演化过程,提出了一种基于叶片和流体间能量传递的简化数值计算方法,以获得某转速下的风车状态临界流量点。在数值模拟的基础上,重点对比了同一转速线上压气机工况点(小流量工况)、风车临界点和涡轮工况点下叶尖泄漏损失的演化机制,同时探究了叶片通道内流动分离的演化过程。 结果显示,随着转速的增加,转子风车状态临界流量呈现近似线性的变化趋势。而同转速下随流量增大,叶尖泄漏流从吸力面流向压力面,并与压力面上的低能量流体进行掺混,造成了流动堵塞。同时,从压气机模式转向涡轮模式的过程中,叶尖区域的流动分离从吸力面分离转变为压力面分离,随后分离强度和尺寸逐渐增大,造成的气动损失显著增加;而在轮毂区域,流动分离始终保持吸力面分离,其分离尺度沿径向有所发展。 相似文献
967.
为了获得三旋流燃烧室喷嘴雾化性能与喷嘴几何尺寸的相互关系,针对供油压力以及旋流槽长宽比和旋流槽角度等关
键结构参数对燃油流量、喷雾锥角和雾化性能的影响进行了试验研究。采用3 维相位多普勒粒子分析仪测量了某一直线上各点的
索太尔平均直径和数密度分布,以及Rosin-Rammler 分布的特征直径和均匀度指数。结果表明:当供油压力提高时,燃油流量和喷
雾锥角增大;旋流槽几何尺寸的变化对燃油流量和喷雾锥角有不同的影响,当旋流槽长宽比和旋流槽角度增大时,燃油流量减小,
喷雾锥角增大。研究所获得的规律为三旋流高温升燃烧室的喷嘴优化设计提供了重要的理论依据。 相似文献
968.
Marchi S. Asphaug E. Bell J. F. Bottke W. F. Jaumann R. Park R. S. Polanskey C. A. Prettyman T. H. Williams D. A. Binzel R. Oran R. Weiss B. Russell C. T. 《Space Science Reviews》2022,218(4):1-28
Space Science Reviews - Analysis of Homestake, Gallex and GNO measurements reveals evidence of variability of presumed solar-neutrino-flux measurements. Analysis of Super-Kamiokande neutrino... 相似文献
969.
A.R. Engel K. Beurle A. Bewick P.K.S. Harper J.J. Quenby N.J.C. Spooner A.G. Fenton K.B. Fenton A.B. Giles J.G. Greenhill D.M. Warren I.M. Martin 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
Hard X-ray balloon altitude measurements with a 1600 cm2 phoswich array are described. Data from observations on Sco X-1, GX1+4, GX5−1, Nova Oph. 1977, SMC X-1, SS433, IC 4329A and MR 2251-178 are presented. The role of Comptonisation in X-ray production for Sco X-1 and GX1+4 is discussed. 相似文献
970.
G. Hasinger W. Pietsch C. Reppin J. Trümper W. Voges E. Kendziorra R. Staubert 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
The Crab was observed in a balloon flight from Palestine/Texas on 9/28/81 at hard X-ray energies (20–200 keV). The light curve is significantly sharper than reported previously for this energy range. The pulse-averaged as well as the interpulse spectra show breaks in our energy-range. The variation of spectral index across the pulse has an amplitude similar to that found at lower energies by OSO-8 and larger than reported by HEAO-1 A4 at hard X-rays. For a sharp emission line at 77 keV a 99% upper limit of 1.0*10−3 photons/ cm2 sec can be placed, a factor of 4 lower than line fluxes reported previously. Pulse-shape fits to the optical, X-ray, hard X-ray and gamma ray light-curves reveal a consistent picture of the origin of the interpulse and off-pulse emission, the breaks in the spectra and the variation of spectral index, providing arguments against a thermal component and also a polar cap emission model for NP0532. 相似文献