丝绸之路经济带的地理空间认知框架研究

针对现有的丝绸之路经济带研究主要集中在人文角度的描述、统计和分析,缺少形象的空间思维手段和对经济带战略全局的整体把控的现状,该文在分析丝绸之路经济带地理特点的基础上,提出了丝绸之路经济带地理空间认知框架,认为丝绸之路经济带的地理空间认知是从概念空间、数据空间到信息空间、知识空间,最后形成智慧空间的认知深化过程,并重点研究了专家认知和用户认知两个关键环节。在此框架下,该文结合丝绸之路经济带的地理特点和测绘地理信息行业的技术现状从地理概念、地理数据、专家认知和用户认知四个方面分析了丝绸之路经济带的主要认知内容。研究表明,用户地理空间认知的深化程度依赖于前期的专家认知成果,专家在认知过程中必须时刻围绕用户的地理空间认知需求,专家认知和用户认知是地理空间认知有机统一的两个核心环节,不可割裂或偏废;直观的地理概念、准确的地理数据、丰富的专家经验和便捷的分析工具是科学认知丝绸之路经济带的技术保障,可以为区域经济合作战略的实施提供更多的地理智慧。     

地理空间大数据存储管理的地理网络地址研究

针对地理空间数据大数据分布式网络存储管理的地理网络位置搜索问题,从地理网络地址的域名角度,基于2n一维整型数组的全球经纬度剖分格网(GeoSOT)框架提出一种具有地理涵义的空间信息存储网络空间域名地址,即Geonet域名,以统一标识地理空间数据的空间区域位置与计算机存储网络的电子方位,实现用户访问的区域范围、地理空间数据所属地域范围与空间信息存储主机之间的一致性空间关联。     

面向海量用户的气象数据开放平台

气象数据开放平台是类似百度开放平台、淘宝开放平台和腾讯开放平台的气象服务数据开放平台,通过提供基于Http(Hypertext transfer protocol,超文本传输协议)协议的应用程序编程接口,面向社会上的个人和机构提供气象服务数据。平台采用Nginx Web Server提供Web数据接口服务,研发Nginx Module处理用户请求和业务逻辑,利用Nginx模块占用内存少、并发能力强、稳定性高的特点,解决因海量用户访问带来的Web Server高负载问题。平台由3个业务处理子平台组成,包括：API接口平台、用户申请平台、业务管理平台,分别负责接口请求处理、用户申请管理和后台管理。     

The Jeans mass and the origin of the knee in the IMF

We use numerical simulations of the fragmentation of a  1000 M_⊙  molecular cloud and the formation of a stellar cluster to study how the initial conditions for star formation affect the resulting initial mass function (IMF). In particular, we are interested in the relation between the thermal Jeans mass in a cloud and the knee of the IMF, i.e. the mass separating the region with a flat IMF slope from that typified by a steeper, Salpeter-like, slope. In three isothermal simulations with   M _Jeans= 1, 2  and  5 M_⊙  , the number of stars formed, at comparable dynamical times, scales roughly with the number of initial Jeans masses in the cloud. The mean stellar mass also increases (though less than linearly) with the initial Jeans mass in the cloud. It is found that the IMF in each case displays a prominent knee, located roughly at the mass scale of the initial Jeans mass. Thus clouds with higher initial Jeans masses produce IMFs which are shallow to higher masses. This implies that a universal IMF requires a physical mechanism that sets the Jeans mass to be near  1 M_⊙  . Simulations including a barotropic equation of state as suggested by Larson, with cooling at low densities followed by gentle heating at higher densities, are able to produce realistic IMFs with the knee located at  ≈1 M_⊙  , even with an initial   M _Jeans= 5 M_⊙  . We therefore suggest that the observed universality of the IMF in the local Universe does not require any fine tuning of the initial conditions in star forming clouds but is instead imprinted by details of the cooling physics of the collapsing gas.     

Contamination and exclusion in the σ Orionis young group

We present radial velocities for 38 low-mass candidate members of the σ Orionis young group. We have measured their radial velocities by cross-correlation of high-resolution  ( R ≈ 6000) AF2/Wide  Field Fibre Optical Spectrograph (WYFFOS) spectra of the gravity-sensitive Na  i doublet at 8183, 8195 Å. The total sample contained 117 objects, of which 54 have sufficient signal-to-noise ratio to detect Na  i at an equivalent width of 3 Å; however, we only detect Na  i in 38 of these. This implies that very low-mass members of this young group display weaker Na  i absorption than similarly aged objects in the Upper Scorpius OB association. We develop a technique to assess membership using radial velocities with a range of uncertainties that does not bias the selection when large uncertainties are present. The resulting membership probabilities are used to assess the issue of exclusion in photometric selections, and we find that very few members are likely to be excluded by such techniques. We also assess the level of contamination in the expected pre-main-sequence region of colour–magnitude space brighter than   I = 17  . We find that contamination by non-members in the expected pre-main-sequence region of the colour–magnitude diagram is small. We conclude that although radial velocity alone is insufficient to confirm membership, high signal-to-noise ratio observations of the Na  i doublet provide the opportunity to use the strength of Na  i absorption in concert with radial velocities to asses membership down to the lowest masses, where lithium absorption no longer distinguishes youth.     

Modelling the components of binaries in the Hyades: the dependence of the mixing-length parameter on stellar mass

We present our findings based on a detailed analysis of the binaries of the Hyades, in which the masses of the components are well known. We fit the models of the components of a binary system to observations so as to give the observed total V and B − V of that system and the observed slope of the main sequence in the corresponding parts. According to our findings, there is a very definite relationship between the mixing-length parameter and the stellar mass. The fitting formula for this relationship can be given as  α= 9.19( M /M_⊙− 0.74)^0.053− 6.65  , which is valid for stellar masses greater than  0.77 M_⊙  . While no strict information is gathered for the chemical composition of the cluster, as a result of degeneracy in the colour–magnitude diagram, by adopting   Z = 0.033  and using models for the components of 70 Tau and θ² Tau we find the hydrogen abundance to be   X = 0.676  and the age to be 670 Myr. If we assume that   Z = 0.024  , then   X = 0.718  and the age is 720 Myr. Our findings concerning the mixing-length parameter are valid for both sets of the solution. For both components of the active binary system V818 Tau, the differences between radii of the models with   Z = 0.024  and the observed radii are only about 4 per cent. More generally, the effective temperatures of the models of low-mass stars in the binary systems studied are in good agreement with those determined by spectroscopic methods.     

The interstellar medium in the Upper Cepheus-Cassiopeia region

We have studied the kinematics and spatial distribution of the interstellar gas in the sky region  110°≤ l ≤ 135°, 10°≤ b ≤ 20°  , using the extensive Leiden–Dwingeloo Survey of H  i emission and the Columbia Survey of CO emission. The spectra show two main velocity components, namely feature A that has a mean local standard of rest (LSR) velocity of  ∼0  km s⁻¹  and is due to the Lindblad ring of the Gould belt, and feature C that has a mean LSR velocity of  ∼−11  km s⁻¹  and is associated to the local arm or Orion arm. The H  i and CO distributions of feature A in the region trace a large complex of gas and dust known as the Cepheus Flare, which lies at a distance of 300 pc. The spectral line profiles of feature A, which are rather broad and often double-peaked, reveal that the Cepheus Flare forms part of a big expanding shell of interstellar matter that encloses an old supernova remnant associated with a void inside the Cepheus Flare. On the other hand, by analysing the distribution and velocity structure of feature C, we have detected a second large expanding shell in the region, located at a distance of 800 pc in the local arm. This shell surrounds the stellar association Cepheus OB4 and was probably generated by stellar winds and supernovae of Cepheus OB4. The radii, expansion velocities and H  i masses of the two shells are approximately 50 pc, 4  km s⁻¹ and  1.3 × 10⁴ M_⊙  for the Cepheus Flare shell and 100 pc, 4 km s⁻¹ and  9.9 × 10⁴ M_⊙  for the Cepheus OB4 shell. Both shells have similar ages of the order of a few 10⁶ yr.     

Oriented precipitates of quartz and amphibole in clinopyroxene of metabasites from the Greek Rhodope: a product of open system precipitation during eclogite–granulite–amphibolite transition

In metabasites from the high‐grade metamorphic Kimi Complex of the Greek Rhodope, lamellae of quartz and amphibole were observed together with either rutile or titanite precipitates in the cores of clinopyroxene that underwent a prolonged exhumation history from eclogite via granulite and amphibolite facies conditions. Lamellae are crystallographically oriented along clinopyroxene cleavage planes (010) and interpreted as the result of precipitation during a two‐step intracrystalline compositional adjustment from an omphacite‐ to a Ca‐Tschermak‐rich clinopyroxene and finally to diopside. Even though retrograde diffusion profiles develop in clinopyroxene, the diffusion rates of highly charged ions like Si⁴⁺, Al³⁺and Ti⁴⁺are too slow, so precipitates rich in Si⁴⁺ (quartz), Al³⁺(amphibole) and Ti⁴⁺(rutile or titanite) form as viable kinetic alternatives. These precipitation reactions are not possible isochemically, and additional exchange of ions with the matrix is required for precipitation to occur. This exchange of mainly rapidly diffusing low‐charge ions is postulated to proceed by bulk diffusion (self‐diffusion) and does not require special pathways or fluid, even though these may play an additional role during metamorphism. This hitherto undescribed process of precipitation made possible by diffusional exchange with the matrix through an intact host crystal lattice is termed here as ‘open system precipitation’ (OSP). No prior Ca‐Eskola‐rich (ultrahigh‐pressure, UHP) composition of omphacite is required to explain the observed precipitates. It is proposed that many precipitation phenomena that were hard to explain in a closed‐system scenario can now be explained more readily by OSP. Calculation of an original solid solution composition, as in an UHP phase, from precipitate and host mineral analyses becomes imprecise to the degree that bulk diffusion and hence OSP have been important.