WR 7a: a V Sagittae or a qWR star?

The star WR 7a, also known as SPH 2, has a spectrum that resembles that of V Sagittae stars although no O  vi emission has been reported. The Temporal Variance Spectrum – TVS – analysis of our data shows weak but strongly variable emission of O  vi lines which is below the noise level in the intensity spectrum.
Contrary to what is seen in V Sagittae stars, optical photometric monitoring shows very little, if any, flickering. We found evidence of periodic variability. The most likely photometric period is   P _phot= 0.227(±14) d  , while radial velocities suggest a period of   P _spec= 0.204(±13) d  . One-day aliases of these periods can not be ruled out. We call attention to similarities with HD 45166 and DI Cru (= WR 46), where multiple periods are present. They may be associated to the binary motion or to non-radial oscillations.
In contrast to a previous conclusion by Pereira et al., we show that WR 7a contains hydrogen. The spectrum of the primary star seems to be detectable as the N  v 4604 Å  absorption line is visible. If so, it means that the wind is optically thin in the continuum and that it is likely to be a helium main sequence star.
Given the similarity to HD 45166, we suggests that WR 7a may be a qWR – quasi Wolf–Rayet – star. Its classification is WN4h/CE in the Smith, Shara & Moffat three-dimensional classification system.     

Quantitative assessment of dissolved radiotracers in the English Channel: Sources, average impact of la Hague reprocessing plant and conservative behaviour (1983, 1986, 1988, 1994)

Knowledge of long-term movements of water-masses in the English Channel has been substantially improved using hydrodynamic modelling coupled with radio-tracers studies; nevertheless, the precision of results so obtained is still largely dependent on measurement precision. New tools are now available to make more accurate determinations of radio-tracer distribution: (1) Repositioning of station locations at the same tide reference-time, giving a homogeneous spatial data set, coupled with the possibility of interpolating and quantifying the amounts of dissolved radioactivity flowing through the English Channel; (2) the first measurements of tritium (³H) in seawater on a large scale in the English Channel demonstrate that this fully conservative radionuclide is a clearly identifiable marker of industrial releases; (3) recent campaigns carried out during the FLUXMANCHE II CCE (1994) programme show the general distribution of dissolved radionuclides ¹³⁷Cs, ¹³⁴Cs, ⁶⁰Co, ¹²⁵Sb, ¹⁰⁶Ru and ³H in the English Channel and the Irish Sea; and (4) the re-utilisation of data from previous campaigns (1983, 1986, 1988) provides indications, at any given location in the English Channel, about the average dilution and distribution of releases derived from the La Hague reprocessing plant. Excesses and losses of radionuclides are now quantified with respect to known source terms; estimates of losses are provided for non-conservative radionuclides, while an excess of ¹³⁷Cs was observed in the English Channel during the period 1983–1994. This excess, which has the same order of magnitude as the quantities released from La Hague plant in the English Channel, could be explained by about 1% of the Sellafield reprocessing plant releases entering the Channel. These results confirm and give a more detailed picture of the previously known distribution of water masses in the English Channel. They lead to clear information about transit times and dilution at this scale, and provide directly comparable data for the validation of hydrodynamic models.     

Dust structure around the Wolf–Rayet star WR104 from lunar occultation observations at 2.2 μm

A rare opportunity of observing a lunar occultation of a Wolf–Rayet star (WR104) in the near-infrared K band (2.2 μm) was utilized to probe the thick dust envelope surrounding the star at a high one-dimensional angular resolution (∼2 mas). Analysis of the occultation light curve shows a dust structure departing significantly from the uniform disc profile. Our results are in good agreement with recent aperture-masking interferometry carried out at the Keck I telescope, which shows a pinwheel structure around WR104. We report additional fine structures in the dust envelope.     

Spectropolarimetric observations of WR 137

We present high signal-to-noise spectropolarimetry of the WC7+OB star WR 137 (HD 192641) covering the spectral range from 3600Å to 1.1µm. The polarization spectrum shows unambiguous evidence for an intrinsic polarization vector.     

中国汽车空调行业HFC-134a需求和排放预测

 近年来HFC-134a作为中国汽车空调行业CFC-12制冷剂最主要的替代品,其消费量增长迅速,是中国消费量最大的HFCs（氢氟烃类物质）。以2005年为基线,通过制冷剂替代、技术进步、熟练操作和政策控制等情景假设,预测了中国汽车空调行业HFC-134a的需求量及排放量。结果表明：到2010和2015年,汽车空调HFC-134a的消费量将分别接近2.0万和3.5万t,排放量将分别接近1.6万和3.0万t,约折合排放21.0 和39.0 Mt CO₂当量。上述排放相对基线情景（即维持当前政策措施和不开展回收活动）,2010年和2015年减排温室气体分别为6.7 和13.0 Mt CO₂当量。     

Structure and kinematics of the interstellar medium around WR 134 and WR 135

Based on our H _α interferometry and 21-cm and CO observations, we analyze the structure and kinematics of the interstellar medium around the stars WR 134 and WR 135. We conclude that the HI bubble found here previously is associated with WR 135, not with WR 134. High-velocity motions of ionized gas that can be interpreted as expansion of the gas swept up by the stellar wind with a velocity up to 50–80 km s^?1 are observed around both stars. The line-of-sight velocity field of the ionized hydrogen in the Cygnus arm is shown to agree with the large-scale line-of-sight velocity distribution of the CO emission.