We have analysed archived Ginga data on the Z source Sco X-2 (GX 349+2). We present the first detailed investigation of its X-ray fast-time variability, as a function of position in the Z track. During the two-day observation over the period 5–7 March 1989, the source was in the so-called flaring branch, and the lower part of the socalled normal branch. We found broad peaked noise with a centro...

A model for irradiated dust disks around Herbig Ae stars is proposed. The model is based on the flaring disk model of Chiang & Goldreich (1997, henceforth CG97), but with the central regions of the disk removed. The inner rim of the disk is puffed up and is much hotter than the rest of the disk, because it is directly exposed to the stellar flux. If located at the dust evaporation radius, its r...

The neutron-star X-ray transient XTE J1701-462 was observed for ∼3 Ms with RXTE during its 2006-2007 outburst. Here we report on the discovery of three type-I X-ray bursts from XTE J1701462. They occurred as the source was in transition from the typical Z-source behavior to the typical atoll-source behavior, at ∼ 10% of the Eddington luminosity. The first burst was detected in the Z-source flar...

Many rural communities in the Nigeria Delta Region have been exposed to the flaring of Associated (AG) gas due to increased extraction of petroleum in the area. The study aimed at assessing the effect of gas flaring on the built environment using buildings as the main observed objects. Two rural communities (Obrikom and Omoku) were used for the case-control study. The study, carried out within ...

The disposal of associated gases through flaring has been a major problem for the Nigerian oil and gas industries and most of theses gases are flared due to the lack of commercial out lets. The resultant effects of gas flaring are the damaging effect of the environment due to acid rain formation, green house effect, global warming and ozone depletion. This writes up is aimed at evaluating groun...

Here we present observational results on the RS CVn star UX Arietis from four very-long-baseline interferometry observations distributed in time to cover the rotational period of 6.44 days. The data are better fit by two Gaussian components than by the usual core-plus-halo model. In the first three days the sizes of the two components did not change much from hour to hour but their relative pos...