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accretion
相关语句
  吸积
    A CALCULATION OF SOFT PHOTON FLUX IN THE TWO-TEMPERATURE ACCRETION DISK MODEL
    在双温度吸积盘模型中软光子能流的计算
短句来源
    THE VARIATION OF PULSE PERIOD OF A X-RAY PULSAR AND K-H INSTABILITY AT THE BOUNDARY OF THE ACCRETION DISK
    X射线脉冲星周期的变化与吸积盘边界的K-H不稳定性
短句来源
    The Thick Accretion Disk Model and Self-gravitating Accretion Disk Model of QSOs
    类星体的厚吸积盘与自引力吸积盘模型
短句来源
    Temperature Distribution of the Accretion Disc Around a Black Hole
    黑洞吸积盘的温度分布
短句来源
    The Accretion Torque Theory of X~Ray Pulsars
    X射线脉冲双星的吸积矩理论
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  “accretion”译为未确定词的双语例句
    Different Types of Accretion Flows Around Massive Black Holes in BL Lac Objects
    BL Lac天体中不同类型的黑洞吸流(英文)
短句来源
    (2) a II * ≈0.940 corresponds to the minimum of the inner marginal radius r ms of black hole accretion disk;
    (2)aII≈0.940对应于黑洞薄盘内边缘半径rms演化的极小值;
短句来源
    We have shown that,compared with the magnetar model,the accretion model for the anomalous X-ray pulsars is unable to account for the distributions of the spin periods observed.
    研究表明 ,与磁星模型相比较 ,反常X射线脉冲星的加速模型不能说明所观测到的自转周期的分布。
短句来源
    A Model of Accretion Disks with Plasma Wave-Turbulence Stress Viscosity
    考虑等离子体波湍动压粘滞的吸和盘模型(英文)
短句来源
    The Effect of Radial Viscous Force on the Stability of a Thin Accretion Disk
    径向粘滞力对薄盘稳定性的影响
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  accretion
Finally I point out the similarities and common physics in Galactic black hole X-ray binaries and active galactic nuclei, and demonstrate that the black hole mass estimation is very much helpful to understand the accretion physics around black holes.
      
Upper Miocene to Holocene sediments from the Cascadia accretionary prism and its oceanic surroundings drilled during ODP Leg 146 are studied in order to reveal their alteration during the accretion.
      
It was found that daily accretion of the Laminaria thallus can remain constant for a long time.
      
In the spawning season, resorption was specified by accretion of the follicular epithelium and release of the homogenized yolk from the oocytes to the follicular wall.
      
The accretion of donor fragments and new branches averaged from 40 to 160 mm per year, depending on the coral species, colony size, and season of transplantation.
      
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The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either...

The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either the power-law or the thermal bremsstrahlung form. 3.The temperature of the thermal bremsstrahlung spectrum is the order of 10~8K. 4.The form of the energy spectrum does not change appreciably when the luminosity fluctuates.

本文研究了密近双星中的 X 射线源的发射机制.本文提出:在致密星(中子星或黑洞)的吸积所形成的 X 射线发射区中,电子对的产生起着重要的作用.这种模型可以定性地说明 X射线双星所具有的几个一般的观测特征,即:1.它们的 X 射线光度都在10~(36)—10~(38)尔格/秒范围中.2.X 射线能谱为幂形式,或热韧致形式.3.热韧致谱的温度数量级为10~K.4.当光度涨落时,能谱形式无明显变化.

From a systematic analysis of the whole history of the protoplanetary cloud and the observational facts of the Earth's atmosphere, we propose a new theory on the Origin of the atmospheres of the Earth and the planets. For the Earth-like planets, there were profound primordial atmospheres originated from the protoplanetary cloud by the accretion of the embryoes of planets. These primordial atmospheres has existed in a time scale of 10~8—10~7 years and were composite from chemically reducing gases. The presence...

From a systematic analysis of the whole history of the protoplanetary cloud and the observational facts of the Earth's atmosphere, we propose a new theory on the Origin of the atmospheres of the Earth and the planets. For the Earth-like planets, there were profound primordial atmospheres originated from the protoplanetary cloud by the accretion of the embryoes of planets. These primordial atmospheres has existed in a time scale of 10~8—10~7 years and were composite from chemically reducing gases. The presence of such a reducing atmosphere may be of great significance to the theories of cosmogony and the origin of life. The contents are as follows 1. The escape of the nebulae and the planetary atmosphers. 2. The blowing-off of the atmospheres and the dissipation of gases driven by the solar wind. 3. The accretion of gases by the planetary embryoes. 4. The primordial atmospheres.

在比较系统地分析了原始太阳星云气体演化全过程和地球与行星大气观测事实的基础上,本文讨论了地球与行星大气起源;地球应有一初级原始大气阶段,其主要特征是还原志。文中还求得了初级原始大气的上下限,讨论了这一大气的性质与演化。

In this paper, we used the more rigorous general relativistic viscose hydrodynami-cal equation to discuss and calculate the temperature profile in the accretion disk around a Kerr black hole. We argued that in the accretion disk around a black hole, it is significant in principle for considering the release of the internal energy of the accreting materials. Taking the effect of internal energy of the accreting materials into account and using the classical theory, we have shown that the occurrence...

In this paper, we used the more rigorous general relativistic viscose hydrodynami-cal equation to discuss and calculate the temperature profile in the accretion disk around a Kerr black hole. We argued that in the accretion disk around a black hole, it is significant in principle for considering the release of the internal energy of the accreting materials. Taking the effect of internal energy of the accreting materials into account and using the classical theory, we have shown that the occurrence of solution of the abnormal temperature profile around a Schwarzschild black hole is possible. In this consistent solution, the temperature profile are not always monotonic, i.e. the temperature is not always a monotonic descending function of the raduis r, not as that of the usual case, but there exists probably a temperature profile with maximum at the certian raduis, in consequence it is existed a cooling region.In order to discuss this subject further, it is natural logically development to using the more rigorous relativistic hydrodynamical equation. Therefore, we will follow the general methods by Bardeen, J. M., Press, W. H., Teukolsky, S. A., and Novikov, I. D.. Thome, K. S. et al. to establish a possible model of accretion disk for the Kerr black hole. Our fundamental assumptions are: (1) The central plane of the disk coincides with the equatorial plane of the black hole. The disk is a perfectly aixal-symmtrie and is thin; (2) The orbital motions of the materials in the disk are controled mainly by the gravitational pull of the hole so that the orbits are very nearly geodesic, while the component of the velocity in the radial direction is very small and the motions in the direction normal to the disk may be neglected; (3) The dominate pressure is the gas pressure, but the radiative pressure is negligble; (4) The radial heat transfer is very small in comparison with the energy radiated from the surface of the disk; (5) The internal energy of the accreting materials in the disk must be calculated. Under these assumptions, our main conclusions obtained are: (1) If the radiative mechanism of the materials in the disk is the black-body radiation, the result is coincidence with the classical theory, whatever kind of the viscose law be; (2) For free-free radiation, the temperature profile is in substance just like the classical case. Thus it is further demonstrated theoretically that there exists indeed such a possible accretion disk around the Kerr black hole which has a fast cooling ring region just laid inside the temperature maximum as its main character. In this cooling ring region, there are probably some pecularities which have not existed for the usual temperature profile.

本文采用较严格的广义相对论粘滞流体动力学方程,讨论并计算了在Kerr度规下黑洞吸积盘的温度分布问题.结果表明,对于绕Kerr黑洞的吸积盘,温度确有极大值的分布轮廓.而且,当盘内物质的辐射机制是黑体辐射时,不论粘滞机制属于何种类型,结果都一样;对于自由—自由辐射,采用a粘滞律模型,与我们在文[1]中所得的结果十分类似.这表明文[1]中所取的近似足合适的.计算还表明,在温度极大值所处半径的内面,有一迅速冷却的环状区域存在.在这一环状区域内,有可能具有某些在通常温度分布时所没有的特性.

 
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