亚临界流体中酶催化制备富含多不饱和脂肪酸甘油酯

研究亚临界流体中酶催化制备富含多不饱和脂肪酸甘油酯.采用亚临界R134a作为固定化脂肪酶Nonozym435催化富含n-3多不饱和脂肪酸甘油酯合成的反应介质,并利用响应面法对影响甘油酯合成的工艺条件进行了优化.结果表明,反应时间、酶用量、底物摩尔比、初始水分是影响酯化率的显著因素.通过对转化率的拟合模型响应面分析,得到了优化工艺条件:在亚临界R134a体系中,体系压力4 MPa,温度40 ℃,反应时间3.59 h,酶量:底物量的3.44%,底物摩尔比质量分数为4.55∶1(甘油/游离脂肪酸),初始水分含量0.81%;在此优化工艺条件下,酯化率的预测值为78.89%,试验值为84.06%.试验值与预测值的相符性很好,RSM模型的有效性得到验证.     

Determination of rate constants for reactions of some hydrohaloalkanes with OH radicals and their atmospheric lifetimes

Rate constants have been measured for the gas-phase reactions of hydroxyl radical with partly halogenated alkanes using the discharge-flow-EPR technique over the temperature range 298–460 K. The following Arrhenius expressions have been derived (units 10^–13 cm³ molecule^–1 s^–1): (8.1 _–1.2 ^+1.5 ) exp{–(1516±53)/T} for CHF₂Cl (HCFC-22); (10.3 _–1.5 ^+1.8 ) exp{–(1588±52)/T} for CH₂FCF₃ (HFC-134a); (11.3 _–1.6 ^+2.1 ) exp{–(918±52)/T} for CHCl₂CF₂Cl (HCFC-122); (9.2 _–2.0 ^+2.5 ) exp{–(1281±85)/T} for CHFClCF₂Cl (HCFC-123a).The atmospheric lifetimes for the substances have been estimated to be 12.6, 12.9, 1.05, and 4.8 years, respectively, and the accuracy of the estimates is discussed.     

A study of the Galactic plane towards l= 305°

We present optical  ( UBVI _C )  observations of a rich and complex field in the Galactic plane towards   l ∼ 305°  and   b ∼ 0°  . Our analysis reveals a significantly high interstellar absorption  ( A _V ∼ 10)  and an abnormal extinction law in this line of sight. Availing a considerable number of colour combinations, the photometric diagrams allow us to derive new estimates of the fundamental parameters of the two open clusters Danks 1 and Danks 2. Due to the derived abnormal reddening law in this line of sight, both clusters appear much closer (to the Sun) than previously thought. Additionally, we present the optical colours and magnitudes of the WR 48a star, and its main parameters were estimated. The properties of the two embedded clusters, DBS2003 130 and 131, are also addressed. We identify a number of young stellar objects which are probable members of these clusters. This new material is then used to revisit the spiral structure in this sector of the Galaxy showing evidence of populations associated with the inner Galaxy Scutum-Crux arm.     

Using caesium‐134 and cobalt‐60 as tracers to assess the remobilization of recently‐deposited overbank‐derived sediment on river floodplains during subsequent inundation events

River floodplains act as sinks for fine‐sediment and sediment‐associated contaminants. Increasing recognition of their environmental importance has necessitated a need for an improved understanding of the fate and residence times of overbank sediment deposits over a broad range of timescales. Most existing investigations have focused on medium‐term accretion rates, which represents net deposition from multiple flood events over several decades. In contrast, the fate of recently‐deposited sediment during subsequent overbank events has received only limited attention. This paper presents a novel tracing‐technique for documenting the remobilization of recent overbank sediment on river floodplains during subsequent inundation events, using the artificial radionuclides, caesium‐134 (¹³⁴Cs) and cobalt‐60 (⁶⁰Co). The investigation was conducted within floodplains of the Rivers Taw and Culm in Devon, UK. Small quantities of fine‐sediment (< 63 µm dia.), pre‐labelled with known activities of either ¹³⁴Cs or ⁶⁰Co, were deposited at 15 locations across each floodplain. Surface inventories, measured before and after three consecutive flood events, were used to estimate sediment loss (in g m^–2). Significant reductions provided evidence of the remobilization of the labelled sediment by inundating floodwaters. Spatial variations in remobilization were related to localized topography. Sediment remobilized during the first two events for the River Taw floodplain were equivalent to 63 · 8% and 11 · 9%, respectively, of the original mass. Equivalent values for the River Culm floodplain were 49 · 6% and 12 · 5%, respectively, of the original mass. Sediment loss during the third event proved too small to be attributed to remobilization by overbank floodwaters. After the third event, a mean of 22 · 5% and 35 · 2% of the original mass remained on the Taw and Culm floodplains, respectively. These results provide evidence of the storage of the remaining sediment. The findings highlight the importance of remobilization of recently‐deposited sediment on river floodplains during subsequent overbank events and demonstrate the potential of the tracing‐technique. Copyright © 2013 John Wiley & Sons, Ltd.     

A dissipative model of interacting winds for WR 140: A comparison with observations

A comparison between the stellar-wind interaction model with electron heat conduction and the ASCA X-ray observations of the (WR+O) binary system WR 140 has been made for the first time. This comparison shows that good agreement with observations can be achieved by varying the physical stellar-wind parameters within the ranges allowed by the accuracy of their determination. The self-consistent two-temperature model with heat conduction is an outgrowth of the model of interacting winds in such systems, which is required to properly interpret future detailed X-ray observations on the Chandra and Newton-XMM satellites.     

The massive Wolf–Rayet binary SMC WR7

We present a study of optical spectra of the Wolf–Rayet star AzV 336a (=SMC WR7) in the Small Magellanic Cloud. Our study is based on data obtained at several Observatories between 1988 and 2001. We find SMC WR7 to be a double-lined WN+O6 spectroscopic binary with an orbital period of 19.56 d. The radial velocities of the He absorption lines of the O6 component and the strong He  ii emission at λ 4686 Å of the WN component describe anti-phased orbital motions. However, they show a small phase shift of ∼1 d. We discuss possible explanations for this phase shift. The amplitude of the radial velocity variations of He  ii emission is twice that of the absorption lines. The binary components have fairly high minimum masses, ∼18 and 34 M_⊙ for the WN and O6 components, respectively.     

Analysis of optical and IR light curves of the WR binary V444 Cygni: are clumps still present?

The results of analysis of new broad band U, J, K, photometric observations of WN5+O6 binary V444 Cyg are presented. Comparison to the old optical data of Cherepashchuk et al. (1984) and IR data of Hartmann (1978) shows that the optical light curve is stable over more than 10 years, while the new infrared light curves are significantly different from the Hartmann's ones. The difference between old and new infrared light curves poses a problem for clumpy structure of WR wind proposed by Cherepashchuk et al. as well as for standard smooth flow wind theory.