安徽大别山腹地中生代火山岩的发现及其地质意义   总被引：10，自引：0，他引：10  

钱存超  贾十军 《安徽地质》1998,(1)

近期作者等在大别山腹地开展１∶５万区调过程时,于中深变质岩中发现一套中生代火山岩系;主要岩石类型为石英安山质晶屑凝灰熔岩、火山角砾岩及凝灰岩。通过详细观察、追索,其中查明火山岩系的空间分布及其与围岩的接触关系。对认识大别山的构造演化及热隆—顶蚀作用、超高压变质带的形成、折返机制等提供新的依据。  相似文献   

四川南部珙县早侏罗世一新蜥脚类恐龙   总被引：3，自引：0，他引：3  

何信禄  王长生  刘尚忠  周凤云  刘图强  蔡开基  代兵 《四川地质学报》1998,(1)

简介在珙县下侏罗统自流井组东岳庙段中,发现的原始蜥脚类恐龙化石的一新属种石碑珙县龙。成年个体长约１４ｍ。化石材料相当丰富,除头骨不完全外,其他部分乃至全部均保存完好。它是早期的原始的蜥脚类,但又和蜥脚类有不少共同点。它对研究蜥脚类的起源和进化,具有重要意义  相似文献   

TFe/TiO_2比值在攀枝花层状辉长岩体钒钛磁铁矿矿床勘探中的应用     

邱仁轩  谢世敏 《四川地质学报》1998,(1)

攀枝花钒钛磁铁矿床是我国特大型晚期岩浆分凝型矿床。本文首次用ＴＦｅ／ＴｉＯ２比值对矿带、矿层、火成堆积旋回进行了详细划分,同时对断层位置、性质及矿床成因进行了判定,并提出在层状辉长岩体中,当ＴＦｅ／ＴｉＯ２比值小于２∶１的部位是寻找独立钛铁矿矿床最佳地段  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   

Sodium beacon tip–tilt determination with Rayleigh-aided auxiliary telescope technique     

S. Esposito  A. Riccardi  & R. Ragazzoni 《Monthly notices of the Royal Astronomical Society》1998,294(3):489-493

The usefulness of tracking the Rayleigh portion of a mesospheric sodium laser guide star as reference for absolute tip–tilt recovery in the frame of the auxiliary telescopes technique is shown. This approach leads to the reduction of the ground occupation needed to attain a given sky coverage by more than one order of magnitude. Speed, tracking precision, and the number of auxiliary telescopes are also reduced, making this new approach a more attractive one. The use of a low-altitude Rayleigh spot reinforces the fundamental limitations affecting this and other techniques, thus degrading significantly the quality of the recovered tip–tilt. However, it is shown that, provided adequate care is taken in the collection and treatment of data, an interesting tilt signal can still be retrieved.  相似文献   

On the global structure of self-gravitating discs for softened gravity     

Jesper Sommer-Larsen  Henrik Vedel  & Uffe Hellsten 《Monthly notices of the Royal Astronomical Society》1998,294(3):485-488

The effects of gravitational softening on the global structure of self-gravitating discs in centrifugal equilibrium are examined in relation to hydrodynamical/gravitational simulations. The one-parameter spline softening proposed by Hernquist & Katz is used.
It is found that if the characteristic size of a disc, r , is comparable to or less than the gravitational softening length, ε, then the cross-section of the simulated disc is significantly larger than that of a no-softening (Newtonian) disc with the same mass and angular momentum.
We demonstrate, furthermore, that if r ≲ε/2 then the scaling relation r ∝ε^3/4 holds for a given mass and specific angular momentum distribution with mass. Finally, we compare some of the theoretical results obtained in this paper and a previous one with the results of numerical Tree-SPH simulations and find qualitative agreement.  相似文献   

Molecular hydrogen line emission from the reflection nebula Parsamyan 18     

Ryder  Allen  Burton  Ashley  & Storey 《Monthly notices of the Royal Astronomical Society》1998,294(2):338-346

The newly commissioned University of New South Wales Infrared Fabry–Perot (UNSWIRF) has been used to image molecular hydrogen emission at 2.12 and 2.25 μm in the reflection nebula Parsamyan 18. P 18 is known to exhibit low values of the (1–0)/(2–1) S(1) ratio, suggestive of UV-pumped fluorescence rather than thermal excitation by shocks. Our line ratio mapping reveals the full extent of this fluorescent emission from extended arc-like features, as well as a more concentrated thermal component in regions closer to the central exciting star. We show that the emission morphology, line fluxes and gas density are consistent with the predictions of photodissociation region (PDR) theory. Those regions with the highest intrinsic 1–0 S(1) intensities also tend to show the highest (1–0)/(2–1) S(1) line ratios. Furthermore, variations in the line ratio can be attributed to intrinsic fluctuations in the incident radiation field and/or the gas density, through the self-shielding action of H₂. An isolated knot of emission discovered just outside P 18, and having both an unusually high (1–0)/(2–1) S(1) ratio and relative velocity, provides additional evidence for an outflow source associated with P 18.  相似文献   

On the nature of the Galactic nebula We 1–12     

Kimeswenger 《Monthly notices of the Royal Astronomical Society》1998,294(2):312-314

In 1977, Weinberger published a list of 12 new extended possible planetary nebulae (PNe). Whereas, because of their characteristic morphology and/or the presence of a blue central star, almost all of them could easily be suspected to be genuine planetary nebulae, one object (No. 12) captivated because of its unusually bright central star. This find prompted Kaler & Feibelman to question the PN nature of this object (We 1–12) on the basis of IUE spectra. A definite conclusion could, however, not be drawn by them; thus, until now, the real nature of We 1–12 remained unsolved. For the first time, a spectral investigation of both the central star and the nebula is presented in this paper. It definitely shows that this intriguing object is an (isolated) H  ii region and its central star, as previously assumed, is an early B star which serves as the ionizing source. We 1–12, a part of which is coincident with a weak IRAS point source, is at a distance of 2–2.6 kpc and is reddened by E ( B − V )=0.6–0.8 mag.  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 UVX quasar optical luminosity function and its evolution     

Pippa Goldschmidt  & Lance Miller 《Monthly notices of the Royal Astronomical Society》1998,293(1):107-112

The recently finished Edinburgh UVX quasar survey at B <18 is used together with other complete samples to estimate the shape and evolution of the optical luminosity function in the redshift range 0.3< z <2.2. There is a significantly higher space density of quasars at high luminosity and low redshift than previously found in the PG sample of Schmidt & Green, with the result that the shape of the luminosity function at low redshifts ( z <1) is seen to be consistent with a single power law. At higher redshifts the slope of the power law at high luminosities appears to steepen significantly. There does not appear to be any consistent break feature which could be used as a tracer of luminosity evolution in the population.  相似文献