共查询到20条相似文献，搜索用时 23 毫秒
1.
David W. MITTLEFEHLDT David J. LINDSTROM Marilyn M. LINDSTROM Ren R. MARTINEZ 《Meteoritics & planetary science》1999,34(3):357-367
Abstract— Mixing models using major and trace elements show that the bulk composition of lithology A (xenocryst-bearing magnesian basalt) of Elephant Moraine A79001 (EETA79001) can be reasonably approximated as a simple mixture of ～44% EETA79001 lithology B (ferroan basalt) and ～56% of Allan Hills A77005 (ALHA7705) light lithology (incompatible element-poor lherzolite). Micro-instrumental neutron activation analysis (INAA) data on xenocryst-free groundmass samples of lithology A show that about 20–25% of the melt phase could be dissolved lherzolite. The bulk and groundmass samples of lithology A have excesses in Au, which indicates either meteoritic contamination or addition by some unknown martian geochemical process. Previous workers have suggested that lithology A was formed by either assimilation of cumulates (like ALHA77005), by a basalt (like lithology B), or by mixing of basaltic and lherzolitic magmas. The former scenario is energetically improbable and unlikely to explain the normal Fe/Mg zonation in lithology A groundmass pyroxenes, whereas the latter scenario is unlikely to satisfy the constraints of the mixing model indicating the ultramafic component is poor in incompatible elements. We suggest rather that EETA79001 lithology A is an impact melt composed dominantly of basalt like lithology B and lherzolitic cumulates like the trace-element-poor fraction of ALHA77005 or Y-793605. This model can satisfy the energetic, petrologic, and geochemical constraints imposed by the samples. If EETA79001 lithology A is an impact melt, this would have considerable consequences for current models of martian petrologic evolution. It would call into question the generally accepted age of magmatism of martian basalts and preclude the use of lithology A groundmass as a primary martian basalt composition in experimental studies. Regardless, the latter is required because lithology A groundmass is a hybrid composition. 相似文献
2.
《天文和天体物理学研究(英文版)》2015,(8)
A sample of 70 E+A galaxies is selected from 37 206 galaxies in the second data release of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope(LAMOST). This sample is selected according to the criteria for E+A galaxies defined by Goto, and each of these objects is further visually identified. In this sample, most objects are low redshift E+A galaxies with z 0.25, and are located in an area of the sky with high Galactic latitude and magnitude from 14 to 18 mag in the g, r and i bands. A stellar population analysis of the whole sample indicates that the E+A galaxies are characterized by both young and old stellar populations(SPs), and the metalrich SPs have relatively higher contributions than the metal-poor ones. Additionally, a morphological classification of these objects is performed based on images taken from the Sloan Digital Sky Survey. 相似文献
3.
本文概述了高质量消色差波片(水晶+MgF_2)的设计原理,晶体材料的光学质量检查,延迟量的误差控制以及波片胶合等方面的问题. 相似文献
4.
A. Pastorello E. Baron D. Branch L. Zampieri M. Turatto M. Ramina S. Benetti E. Cappellaro M. Salvo F. Patat A. Piemonte J. Sollerman B. Leibundgut G. Altavilla 《Monthly notices of the Royal Astronomical Society》2005,360(3):950-962
We present spectroscopic and photometric observations of the peculiar Type II supernova (SN) 1998A. The light curves and spectra closely resemble those of SN 1987A, suggesting that the SN 1998A progenitor exploded when it was a compact blue supergiant. However, the comparison with SN 1987A also highlights some important differences: SN 1998A is more luminous and the spectra show bluer continua and larger expansion velocities at all epochs. These observational properties indicate that the explosion of SN 1998A is more energetic than SN 1987A and more typical of Type II supernovae. Comparing the observational data with simulations, we deduce that the progenitor of SN 1998A was a massive star (∼25 M⊙ ) with a small pre-supernova radius (≲6 × 1012 cm) . The Ba ii lines, unusually strong in SN 1987A and some faint II-P events, are almost normal in the case of SN 1998A, indicating that the temperature plays a key role in determining their strength. 相似文献
5.
Yaser A. Hafez Rod D. Davies Richard J. Davis Clive Dickinson Elia S. Battistelli Francisco Blanco Kieran Cleary Thomas Franzen Ricardo Genova-Santos Keith Grainge Michael P. Hobson Michael E. Jones Katy Lancaster Anthony N. Lasenby Carmen P. Padilla-Torres José Alberto Rubiño-Martin Rafael Rebolo Richard D. E. Saunders Paul F. Scott Angela C. Taylor David Titterington Marco Tucci Robert A. Watson 《Monthly notices of the Royal Astronomical Society》2008,388(4):1775-1786
Accurate calibration of data is essential for the current generation of cosmic microwave background (CMB) experiments. Using data from the Very Small Array (VSA), we describe procedures which will lead to an accuracy of 1 per cent or better for experiments such as the VSA and CBI. Particular attention is paid to the stability of the receiver systems, the quality of the site and frequent observations of reference sources. At 30 GHz the careful correction for atmospheric emission and absorption is shown to be essential for achieving 1 per cent precision.
The sources for which a 1 per cent relative flux density calibration was achieved included Cas A, Cyg A, Tau A and NGC 7027 and the planets Venus, Jupiter and Saturn. A flux density, or brightness temperature in the case of the planets, was derived at 33 GHz relative to Jupiter which was adopted as the fundamental calibrator. A spectral index at ∼30 GHz is given for each.
Cas A, Tau A, NGC 7027 and Venus were examined for variability. Cas A was found to be decreasing at 0.394 ± 0.019 per cent yr−1 over the period 2001 March to 2004 August. In the same period Tau A was decreasing at 0.22 ± 0.07 per cent yr−1 . A survey of the published data showed that the planetary nebula NGC 7027 decreased at 0.16 ± 0.04 per cent yr−1 over the period 1967–2003. Venus showed an insignificant (1.5 ± 1.3 per cent) variation with Venusian illumination. The integrated polarization of Tau A at 33 GHz was found to be 7.8 ± 0.6 per cent at position angle =148°± 3°. 相似文献
The sources for which a 1 per cent relative flux density calibration was achieved included Cas A, Cyg A, Tau A and NGC 7027 and the planets Venus, Jupiter and Saturn. A flux density, or brightness temperature in the case of the planets, was derived at 33 GHz relative to Jupiter which was adopted as the fundamental calibrator. A spectral index at ∼30 GHz is given for each.
Cas A, Tau A, NGC 7027 and Venus were examined for variability. Cas A was found to be decreasing at 0.394 ± 0.019 per cent yr
6.
Qiu-Sheng Du Hui Li 《中国天文和天体物理学报》2008,8(6)
We study the properties of the He I 10830 (A) line in nine selected solar flares, using spectral data obtained with the Multi-channel Infrared Solar Spectrograph (MISS) at Purple Mountain Observatory (PMO) and photospheric images from the Michelson Doppler Imager (MD1) onboard the Solar and Heliospheric Observatory (SOHO). Our results indicate that, over an area of 3"- 8", the He I 10830 (A) line shows emission exceeding the continuum in nearby quiet region when the Geostationary Operations Environmental Satellite (GOES) X-ray class of the flare reaches a threshold value (C4.5). The He I 10830A line emission is detected only in the kernels of the Hα brightenings, but is not associated with the size of the flare. It is found that, whenever the He I 10830(A) line shows excess emission over the nearby continuum both the Hα and the Ca II 8542 (A) lines display enhanced intensities exceeding their preflare intensities. The He I 10830(A) line emission can occasionally extend into the umbra of the involved sunspot, which is inconsistent with previous studies. The weak com-ponent of He I 10830(A) line changes from emission to absorption earlier than does the main component. Our results favor the photoionization-reconnection mechanism for the excitation of the He I 10830(A) line. 相似文献
7.
The three-dimensional inverse problem is investigated. A quasi-linear system of partial differential equations is derived for the determination of the potential. The solution of this system is studied by a method of differential geometry. A necessary condition for the solution is derived and the determination of the potential is reduced to algebraic equations written in vectorial form. A few examples are also given. 相似文献
8.
The hierarchical substructure of the core of the Perseus cluster of galaxies (A426, A262, A347, N507, and N383) is investigated
using the method of S-tree diagrams. In the main system M (100 galaxies), two substructures AM (35 galaxies) and BM (13 galaxies)
are determined. The group AM can be identified with the cluster A262 and the group N507; BM can be identified with the group
N383; A426 and A347 are in the main system. The axis of symmetry of the system M passes through the Seyfert galaxy N1275 and
is parallel to the axis of symmetry of the group AM, which is the core of increased density of the cluster of galaxies. Radial
segregation of galaxies by morphological types is observed in the systems M and AM. The distribution of galaxies by position
angles is uniform.
Translated from Astrofizika, Vol. 41, No. 1, pp. 65–72, January-March, 1998. 相似文献
9.
E. H. Nikogossian 《Astrophysics》2000,43(1):32-39
The hierarchical structure of the clusters of galaxies A 999, A 1016, and A 1142, which are part of one supercluster, is investigated.
The HTree method is used to determine that A 999 and A 1016 are a single, dynamically bound system consisting of two “cores”
and a common field of galaxies. The composition of the “cores” includes almost all the E and S0 galaxies, the luminosity function
of which is very nearly Gaussian. It is also established that the cluster A 1142 has a nonuniform structure, both in density
distribution and in radial velocity distribution. The location of the maxima in density and in the radial velocity distribution
correlates with the galaxies that are sources of radio and x-ray emission.
Translated from Astrofizika, Vol. 43, No. 1, pp. 45-54, January–March, 2000. 相似文献
10.
T. Venturi S. Bardelli G. Zambelli R. Morganti R.W. Hunstead 《Monthly notices of the Royal Astronomical Society》2001,324(4):1131-1146
We report and discuss the results of a 22-cm radio survey carried out with the Australia Telescope Compact Array (ATCA) covering the A3528 complex, a chain formed by the merging ACO clusters A3528–A3530–A3532 , located in the central region of the Shapley Concentration. Simultaneous 13-cm observations are also presented. Our final catalogue includes a total of 106 radio sources above the flux density limit of 0.8 mJy. By cross-correlation with optical and spectroscopic catalogues we found 32 optical counterparts, nine of them belonging to the A3528 complex.
We explored the effects of cluster mergers on the radio emission properties of radio galaxies by means of the radio luminosity function (RLF) and radio source counts. We found that the radio source counts are consistent with the background counts, as already found for the A3558 complex. The RLF for this complex is consistent, in both shape and normalization, with the general cluster luminosity function for early-type galaxies derived by Ledlow & Owen. This result is different from the one we obtained for the A3558 merging complex, the RLF of which is significantly lower than that derived by Ledlow & Owen.
We propose that the different stage of the merger is responsible for the different RLFs in the two cluster complexes in the core of the Shapley Concentration. The early stage of merger for the A3528 complex, proposed by many authors, may not yet have affected the radio properties of cluster galaxies, while in the more much advanced merger in the A3558 region we actually see the effects of this process on the radio emission. 相似文献
We explored the effects of cluster mergers on the radio emission properties of radio galaxies by means of the radio luminosity function (RLF) and radio source counts. We found that the radio source counts are consistent with the background counts, as already found for the A3558 complex. The RLF for this complex is consistent, in both shape and normalization, with the general cluster luminosity function for early-type galaxies derived by Ledlow & Owen. This result is different from the one we obtained for the A3558 merging complex, the RLF of which is significantly lower than that derived by Ledlow & Owen.
We propose that the different stage of the merger is responsible for the different RLFs in the two cluster complexes in the core of the Shapley Concentration. The early stage of merger for the A3528 complex, proposed by many authors, may not yet have affected the radio properties of cluster galaxies, while in the more much advanced merger in the A3558 region we actually see the effects of this process on the radio emission. 相似文献
11.
用云南天文台一米望远镜卡焦摄谱仪(f=175mm相机),在哈雷彗星的日心距分别为1.11AU和0.83AU时,作了两次彗发光谱观测,得到了典型的彗发光谱。本文绘出了各带系清晰的分子发射光谱图及认证结果。此外,本文还给出了彗发CN的(0—1)带(λ4216)和C_3的蓝紫发射(λ4052)及C_2的(2—0)带(λ4365)的强度比CN/C_3和CN/C_2,其值分别为CN/C_3=1.03,CN/C_2=1.00。最后,我们还将结果与其他作者在这次回归中所得到的结果进行了比较。 相似文献
12.
A. Ku
inskas 《Astronomische Nachrichten》1990,311(1):69-73
A review on linear light polarization studies of novae is presented. It is shown that light scattering on dust grains (predominantly graphite) in nova environments is playing a principal role in generation of linear light polarization. A qualitative model responsible for this phenomena is discussed. 相似文献
13.
A photoelectric observation in the near infrared of the 10 February 1977 lunar occultation of Uranus is described and analyzed in terms of planetary radius, limb darkening, and polar brightening. Contact timings, corrected for lunar limb effects, indicate an equatorial radius of 25,700 ± 500km for the visible disk. A modified Minnaert function is used to model limb darkening and polar brightening. Least-squares fits to the observed light curve indicate that Uranus is slightly limb darkened in the passband of the observation (450 ÅA FWHM centered near 6900 ÅA) and that polar brightening is present. 相似文献
14.
徐文莉 《中国天文和天体物理学报》1997,(1)
LAMOST的光学系统由反射施密特改正板MA 和球面主镜MB 组成 ,MA 和MB 均为对角径 1 .1m的六角形子镜的拼镜面 .本文计算了星在子午圈上时望远镜观测不同的天区零视场和有视场时的光学系统衍射能量分布 ,还计算了MA 不变MB 改为整块的 6m镜以及MA 和MB 均为对角径 1 .5m的六角形子镜的拼镜面的衍射能量分布 .对这些计算结果进行分析 ,论证了六角形子镜尺寸选择的合理性 相似文献
15.
The radio source Sgr A and neighbouring features have been mapped at a frequency of 843 MHz with a beamwidth of 43 × 87 arcsec.
Comparisons have been made with published maps of comparable resolution at different frequencies in order to differentiate
thermal and nonthermal regions. The arc feature to the north of Sgr A appears to consist of low-temperature ionized hydrogen
and to extend partly over Sgr A itself causing patchy absorption at low frequencies; there is some evidence that the hydrogen
in the arc has been expelled from the galactic nucleus. Previous suggestions that Sgr A East is a supernova remnant have been
examined and the interpretation is found to be quite likely, but not compelling. The diffuse component of Sgr A West appears
to be due entirely to ionized hydrogen surrounding the nucleus. 相似文献
16.
17.
用GPS秒信号锁定高频振荡器的方法研究 总被引：1，自引：0，他引：1
对用远距离传输的GPS秒信号锁定本地高频晶体振荡器的方法进行了探讨。介绍了高精度的时间数字转换器TDC(Time to Digital Converter)和对滤波的方法进行了探讨。为了降低成本又能够满足设计要求的精度，还考虑了双D／A转换的方法。有关的硬件系统已经通过了调试和一系列的测试和实验，在测量和控制精度方面，能达到设计的要求。此外，提出了这个系统有待解决的问题，如双D／A转换的非线性问题，Kalman滤波抗野值及继续提高精度的问题。 相似文献
18.
Roger H. Hewins 《Meteoritics & planetary science》1988,23(2):123-129
Abstract— The Allan Hills mesosiderites A77219, A81059 and A81098 are classified as subgroup 1B (Hewins, 1984), on the basis of very fine-grained silicate matrix, low plagioclase content and absence of highly ferroan pyroxenes. Since they are so similar petrologically, it is reasonable to pair them. ALHA 81208, a highly weathered orthopyroxenite, is probably a clast from one of the Allan Hills mesosiderites. Reckling Peak A80258, is a Floran 2B or Hewins 4B mesosiderite. It contains reversely zoned orthopyroxene clasts in a sparse matrix with interstitial/poikilitic plagioclase and highly magnesian (chadacryst) orthopyroxene (close to En80). All pyroxene is much lower in FeO/MnO than Allan Hills mesosiderite pyroxene of similar FeO content. The other Reckling Peak mesosiderites A79015, A80229, A80246 and A80263 contain orthopyroxene and recrystallized orthopyroxenite clasts in a metal-troilite matrix. Orthopyroxenite clasts in ALH A81059 are very similar texturally and modally to RKPA 79015 orthopyroxenite, but differ in pyroxene composition. Orthopyroxene in RKPA 79015 (Prinz et al., 1982) is very similar in Fe/Mg and Fe/Mn to the cores of (reversely zoned) pyroxene clasts in RKPA 80258. On this basis, RKPA 80258 is related to the other Reckling Peak mesosiderites and they could all be paired, assuming that three components (metal, pyroxenite and silicate matrix) were very irregularly mixed in these breccias. Pairing is problematical, in that specimens of a polymict breccia can be so different that they would not be paired if they were not known to have fallen together. The silicate fraction of mesosiderites ranges from diogenitic (RKPA 79015) to analogous to polymict eucrite (Dyarrl Island) although the silicate fractions are not equivalent in detail. The mesosiderite subdivision scheme is amended recognizing this, permitting the classification of the formerly “anomalous” RKPA 79015. 相似文献
19.
20.
S. Bardelli A. Pisani M. Ramella E. Zucca & G. Zamorani 《Monthly notices of the Royal Astronomical Society》1998,300(2):589-598
The 'algorithm driven by the density estimate for the identification of clusters' ( DEDICA ) is applied to the A3558 cluster complex in order to find substructures. This complex, located at the centre of the Shapley Concentration supercluster, is a chain formed by the ACO clusters A3556, A3558 and A3562 and the two poor clusters SC 1327-312 and SC 1329-313. We find a large number of clumps, indicating that strong dynamical processes are active. In particular, it is necessary to use a fully three-dimensional sample (i.e. using the galaxy velocity as third coordinate) in order also to recover the clumps superimposed along the line of sight. Even though a large number of detected substructures was already found in a previous analysis, this method is more efficient and faster when compared with a wide battery of tests, and permits the direct estimate of the detection significance. Almost all subclusters previously detected by the wavelet analyses found in the literature are recognized by DEDICA . On the basis of the substructure analysis, we also briefly discuss the origin of the A3558 complex by comparing two hypotheses: (i) the structure is a cluster–cluster collision seen just after the first core–core encounter; or (ii) this complex is the result of a series of incoherent group–group and cluster–group mergings, focused in that region by the presence of the surrounding supercluster. We studied the fraction of blue galaxies in the detected substructures and found that the bluest groups reside between A3562 and A3558, i.e. in the expected position for the scenario of cluster–cluster collision. 相似文献