ANALYSIS OF LOCATION CONDITIONS OF FINANCIAL CENTRES IN CHINA

First of all, the necessity of establishing financial centres is expounded. The establishment of financial centres has a lot of benefits to the world economic development, China's economy and the occupied cities. The location conditions of financial centres may be summarized as follows: the location of trade centre, the factors of geographical position, the circumstances of finance, etc.. We consider that the first batch of financial centres in China should be established in the eastern cities of China. So 9 eastern cities in China are chosen as the spare financial centres. According to the location conditions of financial centres, 12 indices are chosen and the method of synthetic weighted average is used to find the best locations of financial centres. The conclusions are that the grade A financial centres should be in Shanghai and the grade B should be in Tianjin and Guangzhou.     

The destructive effects of binary encounters on red giants in the Galactic Centre

We consider the destructive effects of encounters between binaries and red giant stars in the Galactic Centre. Such encounters may explain the observed depletion of luminous red giants within the central 0.2 pc of the galaxy. We consider encounters involving 2- and 8-M⊙ red giants, and thus span the range of stellar masses contributing to the most luminous red giants observed in the Galactic Centre. To explore the phase space of encounters thoroughly, we simulate 18 × 10³ encounters using a modified four-body code in which the red giant core and components of the binary are treated as point masses, and where the envelope configuration is assumed to remain static throughout the encounter. We then rerun a small number of encounters with a smoothed particle hydrodynamics (SPH) code to confirm the reliability of conclusions drawn from the four-body runs. We see two possible pathways to red giant destruction. A large fraction of encounters lead to the formation of common-envelope systems, where two compact objects (drawn from the red giant core and the components of the original binary) form a binary within a common gaseous envelope, whilst the third body is ejected. The destruction of the red giant will then follow when the envelope is ejected as the binary hardens. In a smaller number of encounters, the intruding binary passes through the star and ejects the red giant core from the envelope. The red giant envelope will then disperse on short time-scales. We compute the time-scales for both of these processes to occur in the Galactic Centre for a variety of binary populations.     

The impact of the parking situation in shopping centres on store choice behaviour

The article discusses the effects of changing the parking situation in the surrounding of shopping centres on consumers store choice behaviour. To get insight into these effects a hierarchical logit model of parking lot and store choice behaviour is estimated and validated. The research is based on before-and-after data of supermarket visitors collected in a major regional shopping centre in a suburban area in The Netherlands. The model is estimated using the before data. At the level of the supermarkets the estimated hierarchical logit model performs very well. The model is less accurate at the level of parking lots but still performs satisfactory. Significant attributes are a constant representing the characteristics of the supermarket, the distance between supermarket and parking lot, the number of parking spaces per parking lot, the location of the parking lot vis-à-vis the origin of the consumer, and the availability of supermarket trolley facilities at the parking lot. Validating the model by reproducing the after data yields less satisfactory results. Especially the model does not perform very well on predicting parking lot choice. This revised version was published online in July 2006 with corrections to the Cover Date.     

Methodological aspects of surveying the volume, structure, activities and perceptions of city centre visitors

Counting pedestrians on a street and visitors entering a store is a method used to measure the attractiveness of these places. Their volumes are governed by daily, weekly, monthly and yearly cycles and are subject to random influences. This must be taken into account especially where comparison counts reveal changes. When single streets or stores are counted, it must be ascertained whether this figure is representative of the whole city centre and its retailing. Pedestrian volumes can be used for adjusting interview samples to the distribution in time and space of the city centre visitors. Counts of the qualitative characteristics of the pedestrian with respect to composition of groups reveal that surveys among pedestrians are biased in relation to the size of the group. Special attention in surveys should be given to the linking of activities. Whereas much emphasis is given to the accessibility of the city centre from outside, the ‘inner accessibility’ of the city centre is just as important. Long distances are often walked and many destinations visited. This is best recorded by conducting interviews at public transport stops and car parks. The attractiveness of the city centre depends not only on its physical structures but very much on the subjective perception of them; therefore judgements on accessibility, goods and services offered and the urban ambiance should be recorded. Retailer's attitudes concerning the qualities of the city centre should also be compiled for comparison. This revised version was published online in July 2006 with corrections to the Cover Date.     

Equivalent width, shape and proper motion of the iron fluorescent line emission from molecular clouds as an indicator of the illuminating source X-ray flux history

Observations of the diffuse emission in the 8–22 keV energy range, elongated parallel to the Galactic plane, and detection of the strong 6.4-keV fluorescent line with ∼ 1 keV equivalent width from some giant molecular clouds (e.g. Sgr B2) in the Galactic Centre region suggest that the neutral matter of these clouds is (or was) illuminated by powerful X-ray radiation, which gave rise to the reprocessed radiation. The source of this radiation remains unknown. A transient source close to the Sgr B2 cloud, or a short outburst of the X-ray emission from a supermassive black hole at the Galactic Centre are the two prime candidates under consideration. We argue that a new generation of X-ray telescopes combining very high sensitivity and excellent energy and angular resolutions would be able to discriminate between these two possibilities when studying time-dependent changes of the morphology of the surface brightness distribution, the equivalent width and the shape of the fluorescent line in Sgr B2 and other molecular clouds in the region. We note also that detection of broad and complex structures near the 6.4-keV line in the spectra of distant AGNs, which are X-ray weak now, may prove the presence of violent activity in the central engines of these objects in the past. Accurate measurements of the line shape may provide information on the time elapsed since the outburst. Proper motion (super- or subluminal) of the fluorescent radiation wave front can give additional information on the location of the source. Observations of the described effects can provide unique information on the matter distribution inside Sgr B2 and other giant molecular clouds.     

Variability associated with α accretion disc theory for standard and advection-dominated discs

The α turbulent viscosity formalism for accretion discs must be interpreted as a mean field theory, modelling a steady state only on spatial or time-scales greater than those of the turbulence. The extent of the scale separation determines the relative precision error (RPE) of the predicted luminosity L _ν. Turbulence and the use of α implies that (1) field line stretching gives a magnetic pressure  α²/6 of the total pressure generally, and a one-to-one relation between α and the pressure ratio for thin discs, and (2) large turbulent scales in advection-dominated accretion flows (ADAFs) predict a lower L _ν precision than thin discs for a given observation duration and central mass. The allowed variability (or RPE) at frequency ν increases with the size of the contributing region. For X-ray binary ADAFs, the RPE ∼ 5 per cent at R  ≤ 1000 Schwarzchild radii ( R _s) for averages over  1000 s. However, current data for galaxies like NGC 4258 and M87 give RPEs in L _ν of 50–100 per cent even at R  ≤ 100  R _S. More data are required, but systematic deviations from ADAF predictions are more significant than random deviations, and may constrain properties of the turbulence, the accretion mode, the assumption of a steady state or the accretion rate.     

Contribution to the search for binaries among Am stars – VIII. New spectroscopic orbits of eight systems and statistical study of a sample of 91 Am stars

Red clump giant (RCG) stars can be used as distance indicators to trace the mass distribution of the Galactic bar. We use RCG stars from 44 bulge fields from the OGLE-II microlensing collaboration data base to constrain analytic triaxial models for the Galactic bar. We find the bar major-axis is oriented at an angle of 24°–27° to the Sun–Galactic Centre line-of-sight. The ratio of semimajor and semiminor bar axis scalelengths in the Galactic plane   x ₀, y ₀  , and vertical bar scalelength z ₀, is   x ₀ :  y ₀ :  z ₀= 10 : 3.5 : 2.6  , suggesting a slightly more prolate bar structure than the working model of Gerhard which gives the scalelength ratios as   x ₀ :  y ₀ :  z ₀= 10 : 4 : 3  .