YS-80-122海洋低温碱性蛋白酶的性质

碱性蛋白酶是一种最重要的工业用酶,广泛应用于洗涤、食品、皮革和丝绸行业.海洋低温碱性蛋白酶是一种应用我国海洋嗜极微生物黄海黄杆菌(YS-80-122)代谢产物并通过现代生物工程手段开发出的一类新型酶.通过6000转/分离心(4℃),收集(30%-65%)硫酸铵沉淀,透析后等电聚焦制备分离(12W),并经凝胶S-200过滤,获得纯品经SDS- PAGE 聚丙烯酰胺凝胶和C8 HPLC 图谱已达到电泳纯.其分子量为49,320Dal,等电点为8.5.建立酶活-温度-pH 方程与模型( r2＞0.9),可求出其最适温度为30℃,最适pH为9.5,低温(T≤30℃)和低 pH(pH≤8)对保持其稳定性有利.经试验该酶与大多数金属离子和增稠剂及表面活性剂适应性良好.Pb2 、 Ag 、Cu2 对其有抑制作用,EDTA对其有强烈抑制作用.该酶性质与以往发现碱性蛋白酶性质不同,属于一种新型海洋酶.     

太湖北岸风浪谱的特征分析

利用１９９２年在太湖北岸马迹山地区测得的浅水风风浪资料，采用ＦＦＴ方法求算风浪频谱，对谱结构特征的分析表明，观测到的风浪谱在平衡范围谱值按－４．０幂指数衰减，风浪谱形状与文圣常给出的理论结果比较接近。另外，分析以风要素为参量得到的无因次化频谱可以看出，观测谱基本满足谱的相似律。     

利用高密度电阻率法进行断层破碎带探查的数值模拟方法

为明确不同条件下断层破碎带的异常特征 ,提高高密度电阻率法 (HDR)的应用效果 ,该文在大量探测实例的基础上提出断层破碎带的地电模型 ;用有限元数值模拟的方式计算出不同地表电性层的情况下 ,高、低阻断层破碎带在不同电测的异常特征并确定最佳采集装置形式 ;并正演模拟倾斜断层的异常分布形态 ,给出为提高视电阻率断面对断层产状反映能力的数据处理方法     

X-ray reflection in accreting stellar-mass black hole systems

The X-ray spectra of accreting stellar-mass black hole systems exhibit spectral features due to reflection, especially broad iron Kα emission lines. We investigate the reflection by the accretion disc that can be expected in the high/soft state of such a system. First, we perform a self-consistent calculation of the reflection that results from illumination of a hot, inner portion of the disc with its atmosphere in hydrostatic equilibrium. Then, we present reflection spectra for a range of illumination strengths and disc temperatures under the assumption of a constant-density atmosphere. Reflection by a hot accretion disc differs in important ways from that of a much cooler disc, such as that expected in an active galactic nucleus.     

Post-Newtonian N-body simulations

We report on the first fully consistent conventional cluster simulation which includes terms up to the third-order post-Newtonian approximation. Numerical problems for treating extremely energetic binaries orbiting a single massive object are circumvented by employing the special 'wheel-spoke' regularization method of Zare which has not been used in large- N simulations before. Idealized models containing   N = 1 × 10⁵  particles of mass  1 M_⊙  with a central black hole (BH) of  300 M_⊙  have been studied on GRAPE-type computers. An initial half-mass radius of   r _h≃ 0.1  pc is sufficiently small to yield examples of relativistic coalescence. This is achieved by significant binary shrinkage within a density cusp environment, followed by the generation of extremely high eccentricities which are induced by Kozai cycles and/or resonant relaxation. More realistic models with white dwarfs and 10 times larger half-mass radii also show evidence of general relativity effects before disruption. An experimentation with the post-Newtonian terms suggests that reducing the time-scales for activating the different orders progressively may be justified for obtaining qualitatively correct solutions without aiming for precise predictions of the final gravitational radiation wave form. The results obtained suggest that the standard loss-cone arguments underestimate the swallowing rate in globular clusters containing a central BH.     

水动力对越南巴达棱湾表层沉积物和岸滩的影响

基于越南巴达棱湾2007年4月采集的42个表层沉积物样品及实测水文资料,分析越南巴达棱湾表层沉积物特征,并结合GSTA模型分析表层沉积物的运移趋势。结果表明:越南巴达棱湾表层沉积物以粗颗粒为主,在潮流和波浪的作用下呈中西部粗、东部细的分布特征;其西侧表层沉积物沿岸线自西南向湾内运移,中西近岸区沉积物垂直于岸线做离岸输移,在湾的东侧存在自东北向西南的运移趋势,并与从湾西运移过来的底沙相遇,形成运移辐聚区,并在余流的作用下,向西运移;"波浪掀沙,潮流输沙"是该地区表层沉积物输运的主要作用机制;在波浪的作用下,研究海域的海岸线处于侵蚀状态,有后退的趋势。     

Black hole spin dependence of general relativistic multi-transonic accretion close to the horizon

We introduce a novel formalism to investigate the role of the spin angular momentum of astrophysical black holes in influencing the behavior of low angular momentum general relativistic accretion. We propose a metric independent analysis of axisymmetric general relativistic flow, and consequently formulate the space and time dependent equations describing the general relativistic hydrodynamic accretion flow in the Kerr metric. The associated stationary critical solutions for such flow equations are provided and the stability of the stationary transonic configuration is examined using an elegant linear perturbation technique. We examine the properties of infalling material for both prograde and retrograde accretion as a function of the Kerr parameter at extremely close proximity to the event horizon. Our formalism can be used to identify a new spectral signature of black hole spin, and has the potential of performing the black hole shadow imaging corresponding to the low angular momentum accretion flow.     

Magnetic field and radius of the innermost stable circular orbit near super‐massive black holes in active galactic nuclei

Magnetic fields in an accretion disk around the central black hole can modify the size of the innermost stable circular orbit (ISCO) and can produce a difference to the classical Novikov‐Thorne radius. We estimated the ISCO magnetic field strength from the polarimetric observations of the accretion‐disk radiation. This estimate is obtained taking into account the effect of the Faraday rotation of the polarization plane at the distance of the mean free path of photons between successive electron scattering events. We present the new method for estimating the ISCO radius in the accretion disk, i.e. in the nearest vicinity of a central black hole. Our estimates confirmed the Frolov, Shoom & Tzounis (2014) and Ranea‐Sandoval & Garcia (2015) conclusion that the magnetic field in the accretion disk decreases the size of the innermost stable circular orbit. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)