赤潮异弯藻对中国对虾感染白斑综合症病毒的影响   总被引：2，自引：2，他引：2       下载免费PDF全文

李才文  管越强  于仁诚  张波  俞志明 《海洋学报》2003,25(1):132-137

白斑综合症病毒(white spot syndrome virus,WSSV)是近年来危害我国乃至世界对虾养殖业的主要流行病原[1-4].WSSV病毒暴发流行范围广、致病性强,自出现以来给对虾养殖业造成了巨大的损失.对虾病毒病的发生是对虾自身的健康状况、病原生物,以及环境条件等各种因素综合作用的结果,外界环境因子或者内环境的变化会引起对虾机体抵抗力下降,从而易受病原生物的感染而发病;同时病原生物的侵入又使机体免疫能力下降而更易受环境因子的胁迫导致疾病突发,因此研究环境因子对病原生物以及对虾抗病力的影响是确保养殖业健康发展的重要环节.  相似文献   

平稳过滤白噪声激励下海洋桩基平台响应分析   总被引：1，自引：0，他引：1  

吴智平  罗传信 《海洋工程》1995,(4)

本文研究了平稳过滤白噪声激励下海洋桩基平台响应分析方法，该方法将强地面运动视为三向平稳过滤白噪声随机过程，应用留数定理推导出积分平台响应的表达式。对一水深为１１４．３ｍ的海洋桩基平台进行了平稳过滤白噪声激励下响应的计算，其成果与平稳白噪声激励下的响应和响应谱法计算结果进行了对比，并得出了相应的结论。  相似文献   

The mass and radius of the M-dwarf in the short-period eclipsing binary RR Caeli     

P. F. L. Maxted  D. O'Donoghue  L. Morales-Rueda  R. Napiwotzki  B. Smalley 《Monthly notices of the Royal Astronomical Society》2007,376(2):919-928

  相似文献   

Post-Common-Envelope Binaries with Distorted Secondaries     

Adela Kawka  Stéphane Vennes 《Astrophysics and Space Science》2005,296(1-4):481-484

We will examine the properties of binary systems which have Roche lobe filling secondaries and white dwarf primaries as well as systems where the secondary is only partially filling its Roche lobe. We will also discuss observational properties such as ellipsoidal variations, light reprocessing and radial velocity measurements of the close binary systems BPM 71214, EC 13471-1258 and GD 245. The properties of BPM 71214 and EC 13471-1258 show that these systems may be pre-cataclysmic variables just prior to the onset of mass transfer or they may be hibernating novae. GD 245 is a pre-cataclysmic variable.  相似文献   

氦白矮星与小质量主序星并合及脉动热亚矮星的形成          下载免费PDF全文

马旭东  张先飞 《天文学报》2020,61(2):19-92

sdBVrs型热亚矮星是一类特殊的热亚矮星,观测显示它们同时具有p模和g模的脉动.目前这一类热亚矮星的演化起源仍然缺乏完备的解释.对氦白矮星与小质量主序星并合模型进行详细计算表明,并合模型的结果符合sdBVrs型热亚矮星的表面有效温度、重力加速度等观测特征,并且能够激发出稳定的p模和g模脉动.因此,氦白矮星与小质量主序星并合是形成sdBVrs型热亚矮星可能的渠道之一.  相似文献   

Continuous measurement of spectrophotometric absorbance in peatland streamwater in northern England: implications for understanding fluvial carbon fluxes     

Richard Grayson  Joseph Holden 《水文研究》2012,26(1):27-39

Bog systems tend to have a flashy hydrological regime with low baseflows and rapid and high storm peaks. Water derived from peatlands often contains significant amounts of organic humic and fulvic materials which form the largest fraction of the dissolved organic carbon component of the fluvial carbon flux. However, most estimates of dissolved organic carbon flux from peatlands are based on sampling that is infrequent and which may miss the periods of high flux during storm events. In order to better characterize the behaviour and fluxes of fluvial carbon it is necessary to operate more frequent sampling. This paper presents data from a continuously operating field‐based spectrophotometer simultaneously measuring absorbance across 200–730 nm at 2·5 nm intervals in runoff from an upland peatland stream. It is shown that absorbance at different wavelengths that have previously been used to characterize dissolved organic carbon varies rapidly during storm events. The probe is shown to even detect changes in absorbance characteristics in response to rainfall events before the stream discharge starts to rise. The high‐resolution behaviour of absorbance characteristics during storm events is different depending on the wavelength studied. Thus, the choice of wavelength used as a proxy for dissolved organic carbon needs careful attention and it may be that automated spectrophotometric methods which provide rich time‐series data from across the spectrum can tell us more about fluxes, processes and sources of aquatic carbon in peatland systems in the future than traditional practices have hitherto allowed. Copyright © 2011 John Wiley & Sons, Ltd.  相似文献   

超大型离心机基础自振特性研究     

王鸿振  张春生  黄维  郭德昌  蒋建群 《岩土力学》2022,43(7):1942-1950

某超大型离心机基础埋置于复杂软土地基中,自振特性研究十分关键。分别建立离心机基础的等效土弹簧模型和实体地基模型,对比分析不同地基模拟方法下的模态分析结果;开展基于白噪声激励的动力时程分析,分析地基参振质量对自振特性的影响。结果表明：超大型离心机基础前两阶模态振型分别为水平横向和纵向的摆动;基于不同的地基模拟方法计算得到的振型结果一致,自振频率相差在10%以内;超大型离心机基础结构的前两阶地基参振质量分别为1.376倍和0.998倍的基础总质量,地基参振质量使得结构的振动响应幅值下降50%左右,频谱峰值频率减小约2 Hz。结论对大型埋置式动力机器基础的自振特性研究具有指导和参考意义。  相似文献   

Observational characteristics and possible asphericity of overluminous Type Ia supernovae     

Keiichi Maeda  Koichi Iwamoto 《Monthly notices of the Royal Astronomical Society》2009,394(1):239-249

A few Type Ia supernovae (SNe Ia) have been suggested to be an explosion of a super-Chandrasekhar-mass white dwarf (WD) in order to account for their large luminosities, requiring a large amount of ⁵⁶Ni. However, the candidate overluminous SNe Ia 2003fg, 2006gz and (moderately overluminous) SN 1991T have very different observational features: the characteristic time-scale and velocity are very different. We examine if and how the diversity can be explained, by one-dimensional spherical radiation transport calculations covering a wide range of model parameters (e.g. WD mass). The observations of SN 2006gz are naturally explained by the super-Chandrasekhar-mass model. SN 1991T represents a marginal case, which may either be a Chandrasekhar or a super-Chandrasekhar-mass WD explosion. In contrast, the low velocity and short time-scale seen in SN 2003fg indicate that the ejecta mass is smaller than the Chandrasekhar mass, which is in apparent contradiction to the large luminosity. We suggest that the problem is solved if the progenitor WD, and thus the SN explosion, is aspherical. This may reflect a rapid rotation of the progenitor star, likely a consequence of the super-Chandrasekhar-mass WD progenitor. The observed differences between SNe 2003fg and 2006gz may be attributed to different viewing orientations.  相似文献   

Magnetized massive stars as magnetar progenitors     

Ren-Yu Hu  Yu-Qing Lou 《Monthly notices of the Royal Astronomical Society》2009,396(2):878-886

  相似文献   

Axisymmetric magnetic fields in stars: relative strengths of poloidal and toroidal components     

Jonathan Braithwaite 《Monthly notices of the Royal Astronomical Society》2009,397(2):763-774

In this third paper in a series on stable magnetic equilibria in stars, I look at the stability of axisymmetric field configurations and, in particular, the relative strengths of the toroidal and poloidal components. Both toroidal and poloidal fields are unstable on their own, and stability is achieved by adding the two together in some ratio. I use Tayler's stability conditions for toroidal fields and other analytic tools to predict the range of stable ratios and then check these predictions by running numerical simulations. If the energy in the poloidal component as a fraction of the total magnetic energy is written as E_p / E , it is found that the stability condition is a ( E / U ) < E_p / E ≲ 0.8 where E /U is the ratio of magnetic to gravitational energy in the star and a is some dimensionless factor whose value is of order 10 in a main-sequence star and of order 10³ in a neutron star. In other words, whilst the poloidal component cannot be significantly stronger than the toroidal, the toroidal field can be very much stronger than the poloidal–given that in realistic stars we expect E / U < 10⁻⁶. The implications of this result are discussed in various contexts such as the emission of gravitational waves by neutron stars, free precession and a 'hidden' energy source for magnetars.  相似文献