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   

Dynamical behaviour of the primitive asteroid belt     

Adrián Brunini 《Monthly notices of the Royal Astronomical Society》1998,293(4):405-410

In this paper we consider the dynamical evolution and orbital stability of objects in the asteroid belt. A simple physical model, including full gravitational perturbations from both giant planets, is used to compute the dynamical evolution of 1000 test particles simulating the primitive asteroids. The criterion of planet crossing (or close approach in the case of resonant objects) is used to reject particles from the simulation. 44 per cent of the particles survived for the whole time-span covered by the numerical integration (∼10⁹ yr).
The 4:1, 3:1 and to a lesser extent the 2:1 Kirkwood gaps are formed in ∼10⁷ yr of evolution, representing direct numerical evidence about their gravitational origin.
We found that the rms eccentricity and inclination of the sample experience a fast increase during the first 10⁶ yr. The final rms eccentricity is 0.11, ∼60 per cent smaller than the present rms eccentricity (0.17). Nevertheless, the gravitational action of the giant planets suffices to prevent the formation of large objects, allowing catastrophic collisions and the subsequent depletion of material from this zone of the Solar system. The excited eccentricity by Jupiter and Saturn may favour mutual encounters and the further increase of the relative velocities up to their present values.  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   

Heavy-element abundances in seven SC stars and several related stars     

Abia  & Wallerstein 《Monthly notices of the Royal Astronomical Society》1998,293(1):89-106

We employ spectra of resolution 20–35000 of seven SC stars, four S stars, two Ba stars and two K–M stars to derive abundances of a variety of elements from Sr to Eu relative to iron. Special attention is paid to Rb and Tc, and to the ratio of the heavy s-process species to the light s-process elements. Abundances are derived in LTE, both by using model atmospheres in which the carbon and oxygen abundances are nearly equal and by using curves of growth. Spectrum synthesis is used for critical lines such as the 5924-Å line of Tc and the 7800-Å line of Rb. For most of the heavy-element stars the enhancement of the s-process elements is about a factor of 10. The ratio of the heavy to light s-process species is not far from solar, except for RR Her for which the same ratio is +0.45 dex. For Tc the blending by other lines is severe. While we have probably detected the 5924-Å line, we can only present abundances in the less-than-or-equal-to category. For Rb, whose abundance is sensitive to the ⁸⁵Rb/⁸⁷Rb ratio and hence to the neutron density during s-process production, we find a considerable range of abundances, indicating a neutron density from 10⁶ to ≳10⁸ cm⁻³ for the SC stars. For the four S stars the range is from 10⁷ to ≳10⁸ cm⁻³. Recent calculations by Gallino et al. show that neutron densities near 10⁷ cm⁻³ favour the ¹³C source for neutrons, while densities greater than 10⁸ cm⁻³ may be associated with neutrons from the ²²Ne source.  相似文献   

现代侵蚀作用核素示踪研究新进展   总被引：11，自引：1，他引：10  

白占国  万国江 《地球科学进展》1998,13(3):232-237

利用放射性核素示踪环境地球化学过程是国际地球科学的前缘课题。介绍了利用宇宙线成因的短寿命散落核素⁷Be示踪土壤季节性侵蚀及其与湖泊沉积耦合关系的最新研究进展;证实了利用核爆炸散落核素¹³⁷Cs示踪累计性土壤侵蚀和沉积计年的可靠性;阐述了²²⁶Ra和²²⁸Ra在土壤中比活度的形态变化分异具有很好的侵蚀－堆积示踪价值;揭示了在不同生物化学条件下,²¹⁰Pb的行为特征和影响因素,并将²¹⁰Pb_ex示踪碳酸盐岩区域土壤侵蚀速率结果与湖泊沉积速率相耦合,证明了利用²¹⁰Pb示踪土壤侵蚀的可行性。  相似文献   

滨海城市环境工程地质问题的成因系统分析   总被引：3，自引：1，他引：2  

李相然 《工程地质学报》1998,6(3):193-198

滨海城市是我国经济最发达的地区,近年来经济与城市建设均得到迅速发展,城市土地开发力度加大,由此引起的环境工程地质问题也日趋严重。本文分析了我国滨海城市环境工程地质问题的主要类型,对环境工程地质问题的成因系统进行了研究。  相似文献   

Observations of the SW Sextantis star UU Aquarii     

Hoard  Still  Paula Szkody  Robert Connon Smith  & Buckley 《Monthly notices of the Royal Astronomical Society》1998,294(4):689-704

We present 14 nights of medium resolution (1–2 Å) spectroscopy of the eclipsing cataclysmic variable UU Aquarii obtained during a high accretion state in 1995 August–October. UU Aqr appears to be an SW Sextantis (SW Sex) star, as noted by Baptista, Steiner & Horne, and we discuss its spectroscopic behaviour in the context of the SW Sex phenomenon. Emission-line equivalent width curves, Doppler tomography, and line profile simulation provide evidence for the presence of a bright spot at the impact site of the accretion stream with the edge of the disc, and a non-axisymmetric, vertically and azimuthally extended absorbing structure in the disc. The absorption has maximum depth in the emission lines around orbital phase 0.8, but is present from φ≈0.4 to φ≈0.95. An origin is explored for this absorbing structure (as well as for the other spectroscopic behaviour of UU Aqr) in terms of the explosive impact of the accretion stream with the disc.  相似文献   

Simulations of spheroidal systems with substructure: trees in fields   总被引：1，自引：0，他引：1  

S.Vine  S.Sigurdsson 《Monthly notices of the Royal Astronomical Society》1998,295(2):475-487

We present a hybrid technique of N -body simulation to deal with collisionless stellar systems having an inhomogeneous global structure. We combine a treecode and a self-consistent field code such that each of the codes models a different component of the system being investigated. The treecode is suited to treatment of dynamically cold or clumpy components, which may undergo significant evolution within a dynamically hot system. The hot system is appropriately evolved by the self-consistent field code. This combined code is particularly suited to a number of problems in galactic dynamics. Applications of the code to these problems are briefly discussed.  相似文献   

Red quasars not so dusty     

C. R.Benn  M.Vigotti  R.Carballo  J. I.Gonzalez-Serrano  S. F.SÃ&#;¡nchez 《Monthly notices of the Royal Astronomical Society》1998,295(2):451-456

Webster et al. claimed that up to 80 per cent of QSOs may be obscured by dust. They inferred the presence of this dust from the remarkably broad range of B − K optical–infrared colours of a sample of flat-spectrum PKS radio QSOs. If such dust is typical of QSOs, it will have rendered invisible most of those which would otherwise have been detected by optical surveys. We used the William Herschel Telescope on La Palma to obtain K infrared images of 54 B3 radio QSOs selected at low frequency (mainly steep-spectrum), and we find that although several have very red optical–infrared colours, most of these can be attributed to an excess of light in K rather than a dust-induced deficit in B. We present evidence that some of the infrared excess comes from the light of stars in the host galaxy (some, as previously suggested, comes from synchrotron radiation associated with flat-spectrum radio sources). The B − K colours of the B3 QSOs provide no evidence for a large reddened population. Either the Webster et al. QSOs are atypical in having such large extinctions, or their reddening is not due to dust; either way, the broad range of their B − K colours does not provide evidence that a large fraction of QSOs has been missed from optical surveys.  相似文献