1·Binary star systems containing a pulsar and an accretion disk occur beginning at about 14:30.
含有脉冲星和吸积盘的双星系统出现在大约1430的位置。
2·The rotational energy of the spinning accretion disk adds momentum to the outflowing jet.
吸积盘的旋转动能(通过磁场机制)转移给了喷流。
3·This formation, called an accretion disk, may be very important in some stellar birth sequences.
这种构成物即所谓吸积盘，它在恒星诞生的某些阶段可能是非常重要的。
4·The single black hole-accretion disk precession model or disk-driven precession model is discussed carefully;
着重论述了单黑洞—吸积盘进动模型或盘致进动模型；
5·That wind flows in from the hot inner regions of the dusty, gaseous accretion disk surrounding the black hole.
风流动的热点区域内的尘埃，气体吸积盘周围的黑洞。
6·Later simulations show that even a companion with an orbit as wide as Neptune's could scoop up an accretion disk.
后来的数值模拟结果显示出，即使伴星的轨道半径大如海王星的轨道，它仍可汲取物质而形成吸积盘。
7·As the accretion disk feeds more mass into itself, the embryo star contracts, growing ever denser and more massive.
随著吸积盘获得越来越多的物质，胚胎恒星就不断收缩，密度和质量都变得越来越大。
8·The conclusion is: the short term variability behavior provides a strong support to the thick accretion disk model of AGN.
这些讨论表明，活动星系核的短时标光变特征对厚吸积盘模型提供了强有力的支持。
9·The structure and radiation of geometrically thick accretion disk of QSOs with magnetic field are discussed in this paper.
本文讨论了具有磁场的几何厚吸积盘结构和辐射。
10·Infalling gas may first collide not only with itself but with an accretion disk of swirling material surrounding the black hole.
正在下落的气体不但会先和自身发生碰撞，还会和黑洞周围盘旋着的物质吸积盘相互碰撞。