沼泽生红冬孢酵母的固体培养条件

以麸皮、豆粕和红糖为基料,固态培养沼泽生红冬孢酵母(Rhodosporidium paludigenum),研究沼泽生红冬孢酵母的固体培养条件和培养基。结果表明,优化的固体培养基和培养条件为:豆粕、麸皮和红糖的最佳质量比为3∶1∶1;每10 g基料,各组分添加量分别为酵母膏0.2 g,硫酸铵0.2 g,水12 mL,接种1.5 mL菌液;培养基厚度2.35 cm。在此条件下培养60 h,红酵母的细胞产量最高达101.9×108g-1。     

1966年邢台地震静态库仑应力触发分析

通过分析1966年邢台5次地震的静态库仑应力触发情况发现,前2次地震对后面的地震有较好的触发,而MS7.2以后地震的触发不理想。从而认为,随着地震的发生和震源深度的增加,岩浆活动对地壳介质的影响越来越大,地壳介质弹性性能越来越弱,即该区域浅部可以用均匀弹性半空间来近似,而深部在岩浆等因素的影响下,用均匀弹性半空间来近似存在较大的误差,不适合用弹性位错理论计算地震的触发关系。这从侧面反映了该地区岩浆活动的剧烈性和超壳断层存在的客观性。     

The radio and X-ray properties of Abell 2319

New radio and X-ray data are reported for the rich cluster Abell 2319. This object is known from optical data to consist of two separate clusters, which are displaced by about 10′ in the NW direction, and could be in a pre-merger state.

In the radio domain, the cluster is characterized by the presence of a central diffuse halo source, more extended and powerful than the prototype halo in the Coma cluster. The radio halo shows an irregular structure, elongated in the NE-SW direction, and also extended towards the NW. We also report data on the extended radio galaxies located within the halo, or in its proximity.

The cluster X-ray brightness distribution shows an elongated structure towards the NW, in the radial region between 6′–12′, i.e. in the direction of the subcluster. This feature is exactly coincident with the NW extension of the radio halo. In addition, more substructural features are identified which could be due to an ongoing merger of the cluster with yet another mass component.

The radio halo morphology is correlated with the X-ray structure and the existence of merger processes in the cluster. The cluster merger can provide energy to maintain the radio halo, while the origin of the relativistic particles seems more problematic.     

Chandra measurements of the distribution of mass in the luminous lensing cluster Abell 2390

We present spatially resolved X-ray spectroscopy of the luminous lensing cluster Abell 2390, using observations made with the Chandra observatory. The temperature of the X-ray gas rises with increasing radius within the central ∼ 200 kpc of the cluster, and then remains approximately isothermal, with kT =11.5_−1.6^+1.5 keV , out to the limits of the observations at r ∼1.0 Mpc . The total mass profile determined from the Chandra data has a form in good agreement with the predictions from numerical simulations. Using the parametrization of Navarro, Frenk and White, we measure a scale radius r _s∼0.8 Mpc and a concentration parameter c ∼3 . The best-fitting X-ray mass model is in good agreement with independent gravitational lensing results and optical measurements of the galaxy velocity dispersion in the cluster. The X-ray gas to total mass ratio rises with increasing radius with f _gas∼21 per cent at r =0.9 Mpc . The azimuthally averaged 0.3–7.0 keV surface brightness profile exhibits a small core radius and a clear 'break' at r ∼500 kpc , where the slope changes from S _X ∼^∝  r ^−1.5 to S _X ∼^∝  r ^−3.6 . The data for the central region of the cluster indicate the presence of a cooling flow with a mass deposition rate of 200–300 M_⊙ yr⁻¹ and an effective age of 2–3 Gyr .     

Infrared photometry of AGB stars

The goal of this article is to show that, if one avoids star forming regions, mass-losing AGB stars can generally be selected from the data that will be provided by the near-infrared surveys which are presently considered. Also, if IRAS data are available, the separation between carbon-rich and oxygen-rich stars can be operated by their positions in infrared colour diagrams. In extragalactic systems, red supergiants can be discriminated from AGB stars by their luminosities.based on observations obtained with the ESO 1-m telescope