A source extent analysis of the Lancang earthquake ( M _s=7.6) of 1988     

Si-Hua Zheng  Jian Yang 《地震学报(英文版)》1998,11(4):393-402

Source extent parameters of the 1988 Lancang earthquake (M _s=7.6) were estimated by computing the second-central moment of displacement pulses of far field long period SH waves. We inverted the source duration T, the fault length L and the directivity parameter D by the least squares, and obtained that T=11.77 s, D=15.05 km·s, and L=70.94 km. We also find that this event is a symmetrically bilateral rupture and fault segments in two opposite rupture directions have the same value of 35 km in length. Combining analysis of aftershock distribution, the results would imply that there is an area in the joint part of the rupture area of two main shocks, which is not broken yet during the main shocks. Due to the dislocation accompanied during the main shocks, the strain would be rearranged. The joint part has enough strength to accumulate enough strain energy to excite a larger aftershock.  相似文献   

大连开发区场地地震设计参数     

钱瑞华  徐峰 《工程地质学报》1998,6(1):72-74

根据工作区潜在震源区划分、潜在震源区地震活动性参数和地震动衰减关系, 进行场地地震危险性分析, 得到不同概率水平下场区相应地震烈度和基岩水平加速度峰值及其反应谱。根据场地工程地震条件划分不同地质单元及相应的场地类别, 进行不同概率水平的地震反应分析计算, 确定地震动设计参数。  相似文献   

White dwarf masses in magnetic cataclysmic variables: multi-temperature fits to Ginga data     

Mark Cropper  Gavin Ramsay  & Kinwah Wu 《Monthly notices of the Royal Astronomical Society》1998,293(3):222-232

One method of obtaining the mass of the white dwarf in magnetic cataclysmic variables (mCVs) is through their hard X-ray spectra. However, previous mass estimates using this method give lower limits because the temperature of the plasma in the post-shock region (where the hard X-rays are emitted) is lower than the temperature of the shock itself. In AM Her systems, the additional cooling of the post-shock plasma by cyclotron emission will further lower the derived mass. Here we present estimates of the masses of the white dwarf in 13 mCVs derived using Ginga data and a model in which X-rays are emitted from a multi-temperature emission region with the appropriate temperature and density profile. We include in the model reflection from the surface of the white dwarf and a partially ionized absorber. We are able to achieve good fits to the data. We compare the derived masses with previous estimates and the masses for larger samples of isolated white dwarfs and those in CVs.  相似文献   

Weighing a galaxy bar in the lens Q2237 +=0305     

RobertSchmidt  Rachel L.Webster  Geraint F.Lewis 《Monthly notices of the Royal Astronomical Society》1998,295(2):488-496

In the gravitational lens system Q2237+0305 the cruciform quasar image geometry is twisted by 10c by the lens effect of a bar in the lensing galaxy. This effect can be used to measure the mass of the bar. We construct a new lensing model for this system with a power-law elliptical bulge and a Ferrers bar. The observed ellipticity of the optical isophotes of the galaxy leads to a nearly isothermal elliptical profile for the bulge, with a total quasar magnification of 16⁺⁵₋₄. We measure a bar mass of (7.5 ∼ 1.5) −10⁸ h ⁻¹₇₅ M⊙ in the region inside the quasar images.  相似文献   

CCD photometry of variable stars in the Magellanic Clouds — V. The eclipsing binaries HV 1620 and HV 2241     

Pritchard  Tobin  Clark  & Guinan 《Monthly notices of the Royal Astronomical Society》1998,297(1):278-290

Using improved techniques, high-quality CCD uvbyVI _C photometry has been obtained for the 14th magnitude eclipsing binaries HV 1620 in the Small Magellanic Cloud (SMC) and HV 2241 in the Large Magellanic Cloud (LMC). IUE ultraviolet spectrophotometry was also obtained. These data have been analysed using the Wilson & Devinney synthetic light-curve code and Kurucz model atmospheres. Both systems are semi-detached and appear to have undergone mass exchange. In HV 1620 the mass ratio and the effective temperatures of the primary and secondary are q  =  M ₂/ M ₁ = 0.68 ± 0.03, T _eff,1 = 33 000 ± 4500 K and T _eff,2 = 24 000 ± 3500 K. The corresponding values for HV 2241 are 0.53 ± 0.01, 27 000 ± 3000 K and 20 200 ± 1500 K. Using the radial-velocity curves obtained by Niemela & Bassino with a 1-m telescope, we find that both systems are massive, as expected. Reddening considerations suggest both systems may lie towards the rear of their respective Clouds.  相似文献   

Interacting OB star binaries: LZ Cep, SZ Cam and IU Aur     

T. J.Harries  R. W.Hilditch  G.Hill 《Monthly notices of the Royal Astronomical Society》1998,295(2):386-396

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Contribution of galaxies to the background hydrogen-ionizing flux     

Julien E. G. Devriendt  Shiv K. Sethi  Bruno Guiderdoni  & Biman B. Nath 《Monthly notices of the Royal Astronomical Society》1998,298(3):708-718

We estimate the evolution of the contribution of galaxies to the cosmic background flux at 912 Å by means of a semi-analytic model of galaxy formation and evolution. Such modelling has been quite successful in reproducing the optical properties of galaxies. We assume that high-redshift damped Lyman α systems are the progenitors of present-day galaxies, and we design a series of models that are consistent with the evolution of cosmic comoving emissivities in the available near-infrared, optical, ultraviolet and far-infrared bands along with the evolution of the neutral hydrogen content and average metallicity of damped Lyman α systems. We use these models to compute the galactic contribution to the Lyman-limit emissivity and background flux for 0 ≃  z  ≤ 4. We take into account the absorption of Lyman-limit photons by H  I and dust in the interstellar medium of the galaxies. We find that the background Lyman-limit flux due to galaxies might dominate (or be comparable to) the contribution from quasars at almost all redshifts if the absorption by H  I in the interstellar medium is neglected. Such H  I absorption would result in a severe diminishing of this flux — by almost three orders of magnitude at high redshifts and by one to two orders at z  ≃ 0. Though the resulting galaxy flux is completely negligible at high redshifts, it is comparable to the quasar flux at z  ≃ 0.  相似文献   

The z=2.72 galaxy cB58: a gravitational fold arc lensed by the cluster MS 1512+36     

Stella Seitz  R. P. Saglia  Ralf Bender  Ulrich Hopp  Paola Belloni  & Bodo Ziegler 《Monthly notices of the Royal Astronomical Society》1998,298(4):945-965

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Metallicity and photospheric abundances in field K and M dwarfs     

M. Zboril  & P. B. Byrne 《Monthly notices of the Royal Astronomical Society》1998,299(3):753-758

Elemental abundances in late-type stars are of interest in several ways: they determine the location of the stars in the HR diagram and therefore their ages, as well as the atmospheric structure in their middle and upper photospheres. Especially in the case of chromospherically active late-type stars the question arises to what degree the upper photosphere is influenced by the nearby chromosphere. Analysing S/N ∼ 200 and Δλ/λ ∼ 20 000 data, we found a mean metallicity index [M/H] = −0.2 for programme K and M field stars based on an analysis of spectra in the region 5500–9000 Å. We also found that the Ca  I 6162-Å transition is a potential surface gravity indicator for K-type stars. For the chromospheric activity interval 4.4 < log  F _{Mg II}  < 6.6 we did not find any chromospheric activity impact on photospheric and upper photospheric transitions. With the derived metallicity, we confirmed the Li abundance from our previous paper and thus its dependence on the Mg  II chromospheric activity index. The nature of the spectrum for the active M-type star Gl 896A is explained by pure rotation of 14 km s⁻¹. As far as the lithium–rotation relation is concerned, the spectrum of Gl 517 is rotationally broadened as well, by 12 km s⁻¹, and the Li abundance is the second highest in our sample of stars. However, there is no link between very high Li abundance, 2.2 dex, in the K dwarf star Gl 5 and stellar rotation.  相似文献   

Extended source effects in astrometric gravitational microlensing     

Shude Mao  & Hans J. Witt 《Monthly notices of the Royal Astronomical Society》1998,300(4):1041-1046

Extended source size effects have been detected in photometric monitoring of gravitational microlensing events. We study similar effects in the centroid motion of an extended source lensed by a point mass. We show that the centroid motion of a source with uniform surface brightness can be obtained analytically. For a source with a circularly symmetric limb-darkening profile, the centroid motion can be expressed as a one-dimensional integral, which can be evaluated numerically. We find that when the impact parameter is comparable to the source radius, the centroid motion is significantly modified by the finite source size. In particular, when the impact parameter is smaller than the source radius, the trajectories become clover-leaf like. Such astrometric motions can be detected using space interferometers such as the Space Interferometry Mission . Such measurements offer exciting possibilities for determining stellar parameters, such as stellar radius, to excellent accuracy.  相似文献