CUTLASS Finland radar observations of the ionospheric signatures of flux transfer events and the resulting plasma flows   总被引：1，自引：0，他引：1  

G. Provan  T. K. Yeoman  S. E. Milan 《Annales Geophysicae》1998,16(11):1411-1422

The CUTLASS Finland radar has been run in a two-beam special scan mode, which offered excellent temporal and spatial information on the flows in the high-latitude ionosphere. A detailed study of one day of this data revealed a convection reversal boundary (CRB) in the CUTLASS field of view (f.o.v) on the dayside, the direction of plasma flow either side of the boundary being typical of a dawn-cell convection pattern. Poleward of the CRB a number of pulsed transients are observed, seemingly moving away from the radar. These transients are identified here as the ionospheric signature of flux transfer events (FTEs). Equatorward of the CRB continuous backscatter was observed, believed to be due to the return flow on closed field lines. The two-beam scan offered a new and innovative opportunity to determine the size and velocity of the ionospheric signatures associated with flux transfer events and the related plasma flow pattern. The transient signature was found to have an azimuthal extent of 1900 ± 900 km and an poleward extent of 250 km. The motion of the transient features was in a predominantly westward azimuthal direction, at a velocity of 7.5 ± 3 km.  相似文献   

新型耗能(阻尼)减震器的开发与研究   总被引：18，自引：7，他引：11  

周云  刘季 《地震工程与工程振动》1998,18(1):71-79

本文阐述了耗能减震的概念和原理,提出了耗能减震器设计的新思想,研制开发了多种新型实用耗能（阻尼）减震器,并对其中的圆环耗能器、双环耗能器、架颈圆环耗能器、弹塑性－摩擦复合耗能器等进行了循环荷载试验,考察了耗能器代作性能和耗能性能,对已装与未装耗能减震器的钢筋混凝土框架模型进行了伪动力对比实验,进一步考察了耗能减震器的减震效果。在试验研究的基础上,地耗能（阻尼）减震结构体系的分析方法进行了研究,并编  相似文献   

机器基础动力相互作用的研究     

姜忻良  李燕飞  郑刚 《地震工程与工程振动》1998,18(1):95-102

本文分别对单台、双台、联合基础与地基土相互作用体系在扰力作用下的振动特性进行了研究。在计算中考虑了外围土体的影响。通过算例,得到了单台、双台、联合基础的一些振动规律。  相似文献   

地震波测试技术在十三陵蓄能电站工程验收中的应用     

文学宽  许延春 《城市地质》1998,10(1):25-29

介绍了地震波测试技术在钻孔中测试地层动弹模的原理、方法及效果,并计算出静弹模,为工程的质量评价和验收提供了依据。  相似文献   

宝石颜色的命名与判定方法评述     

张庆麟 《上海国土资源》1998,(3):24-29

较系统评述了现有的各种命名与判定宝石颜色的方法,如命名法中的二名法、类似法、色度法和三要素法;判定法中的目测法、仪器测量法和对比法。指出它们均存在有不同程度的缺点,但相对比较起来,用色谱图系的对比法是目前较好的方法。  相似文献   

A new population of brown dwarfs     

M. R. S. Hawkins  C. Ducourant  H. R. A. Jones  & M. Rapaport 《Monthly notices of the Royal Astronomical Society》1998,294(3):505-512

In this paper we report the first results from a survey for low-mass stars and brown dwarfs, based on a photographic stack of around 100 Schmidt plates. This survey extends photographic searches by about 2 mag, and covers an area of 25 deg². Some 30 faint objects with large R − I colours were selected for further study, and were found to have very strong molecular absorption in their spectra, but only moderately red infrared colours. Five of these stars were selected for a parallax programme; three of these were found to be at a distance of around 45 pc, implying a very low luminosity. On the basis of their luminosity alone it is clear that these stars are field brown dwarfs, and we discuss their likely evolutionary status in the context of current models of low-mass stellar evolution.  相似文献   

The light curves of soft X-ray transients     

King  & Ritter 《Monthly notices of the Royal Astronomical Society》1998,293(1):L42-L48

We show that the light curves of soft X-ray transients (SXTs) follow naturally from the disc instability picture, adapted to take account of irradiation by the central X-ray source during the outburst. Irradiation prevents the disc from returning to the cool state until central accretion is greatly reduced. This happens only after most of the disc mass has been accreted by the central object, on a viscous time-scale, accounting naturally for the exponential decay of the outburst on a far longer time-scale (τ20–40 d) than seen in dwarf novae, without any need to manipulate the viscosity parameter α. The accretion of most of the disc mass in outburst explains the much longer recurrence time of SXTs compared with dwarf novae. This picture also suggests an explanation of the secondary maximum seen in SXT light curves about 50–75 d after the start of each outburst, since central irradiation triggers the thermal instability of the outer disc, adding to the central accretion rate one viscous time later. The X-ray outburst decay constant τ should on average increase with orbital period, but saturate at a roughly constant value ∼40 d for orbital periods longer than about a day. The bolometric light curve should show a linear rather than an exponential decay at late times (a few times τ). Outbursts of long-period systems should be entirely in the linear decay regime, as is observed in GRO J1744−28. UV and optical light curves should resemble the X-rays but have decay time-scales up to 2–4 times longer.  相似文献   

The dwarf galaxy population of the Coma cluster to M_R=−11: a detailed description     

Neil Trentham 《Monthly notices of the Royal Astronomical Society》1998,293(1):71-88

We present the luminosity function and measurements of the scalelengths, colours and radial distribution of dwarf galaxies in the Coma cluster down to R =24. Our survey area is 674 arcmin²; this is the deepest and most detailed survey covering such a large area.
Our measurements agree with those of most previous authors at bright and intermediate magnitudes. The new results are as follows.
(1) Galaxies in the Coma cluster have a luminosity function φ( L )∝ L ^α that is steep (α∼−1.7) for −15< M_R <−11, and is shallower brighter than this. The curvature in the luminosity function at M_R ∼−15 is statistically significant.
(2) The galaxies that contribute most strongly to the luminosity function at −14< M_R <−12 have colours and scalelengths that are consistent with those of local dwarf spheroidal galaxies placed at the distance of Coma.
(3) These galaxies with −14< M_R <−12 have a colour distribution that is very strongly peaked at B − R =1.3. This is suggestive of a substantial degree of homogeneity in their star formation histories and metallicities.
(4) These galaxies with −14< M_R <−12 also appear to be more confined to the cluster core ( r ∼200 kpc) than the brighter galaxies. Alternatively, this observation may be explained in part or whole by the presence of an anomalously high number of background galaxies behind the cluster core. Velocity measurements of these galaxies would distinguish between these two possibilities.  相似文献   

The galaxy luminosity function in clusters and the field     

Neil Trentham 《Monthly notices of the Royal Astronomical Society》1998,294(2):193-200

We present the results from a CCD survey of the B -band luminosity function of nine clusters of galaxies, and compare them to published photographic luminosity functions of nearby poor clusters like Virgo and Fornax, and also to the field luminosity function. We derive a composite luminosity function by taking the weighted mean of all the individual cluster luminosity functions; this composite luminosity function is steep at bright and faint magnitudes and is shallow in-between.
All clusters have luminosity functions consistent with this single composite function. This is true both for rich clusters like Coma and for poor clusters like Virgo.
This same composite function is also individually consistent with the deep field luminosity functions found by Cowie et al. and Ellis et al., and also with the faint end of the Las Campanas Redshift Survey R -band luminosity function, shifted by 1.5 mag. A comparison with the Loveday et al. field luminosity function, which is well determined at the bright end, shows that the composite function, which fits the field data well fainter than M _B=−19, drops too steeply between M _B=−19 and −22 to fit the field data there.  相似文献   

The biconical kiloparsec structure generated by nuclear starbursts     

Guillermo Tenorio-Tagle  & Casiana Muñoz-Tuñón 《Monthly notices of the Royal Astronomical Society》1998,293(3):299-305

Two-dimensional calculations of the hydrodynamics produced by nuclear starbursts, taking into consideration the accretion or infall of disc matter on to the heart of the starburst, are here shown to lead to stationary solutions that naturally account for the kpc-scale biconical X-ray and optically detected filamentary structure. The calculated flows are critically compared with former models and with observations of nuclear starbursts. For the infall models, we find that the mechanical energy power of the nuclear cluster must exceed a threshold value, imposed by the rate of disc mass accretion, to undergo blowout. This, combined with an initial mass function (IMF), is shown to regulate the minimum amount of mass that a starburst needs to generate kpc-scale outflows.  相似文献