黑洞吸积是类星体的能量来源。
The accretion onto the black hole is the source of the quasar's energy.
然后，我们研究无粘滞的绝热吸积流。
Second, we study the stability in the inviscid adiabatic limit.
此能量释放使吸积盘成为巨大能量的来源。
The energy release can make accretion disks formidable power sources.
含有脉冲星和吸积盘的双星系统出现在大约1430的位置。
Binary star systems containing a pulsar and an accretion disk occur beginning at about 14:30.
吸积黑洞双星是认识黑洞物理的最重要目标之一。
Accreting black hole binaries are important objects to learn black hole physics.
吸积盘的旋转动能(通过磁场机制)转移给了喷流。
The rotational energy of the spinning accretion disk adds momentum to the outflowing jet.
研究了环绕致密天体的吸积盘的稳定性质和振动模式。
Stability properties and oscillation modes of accretion disks around compact objects are studied in this paper.
相反，来自双白矮星并合的超新星产生的X射线辐射要比吸积少很多。
A supernova from a merger of two white dwarfs, on the other hand, would create significantly less X-ray emission than the accretion scenario.
在单星系如我们的太阳系中，普遍认定行星是通过吸积的过程逐渐形成的。
In a one-star system like our solar system, the leading theory as to how the planets formed is through a process called accretion.
由物质吸积导致的Ia型超新星会在爆发前产生大量的X射线辐射。
A Type 1a supernova caused by accreting material produces significant X-ray emission prior to the explosion.
碳质球粒陨石星子被吸积于原始地球上地幔表层，形成原始富碳区。
Carbonaceous chondrite planetesimals were adsorbed on the mantle surface of the primitive earth, forming primitive carbon-rich areas.
在中子星或黑洞伴星上发生吸积的模型，仍应看成是一个有价值的假说。
The model comprising accretion onto a neutron star or black hole companion must still be considered a favored hypothesis.
在本文中我们通过agb星研究了此临界吸积率和金属丰度之间的关系。
In this thesis, we study the relation between the critical accretion rate and the metallicity via AGB stars approach.
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。
This formation, called an accretion disk, may be very important in some stellar birth sequences.
为我们相信吸积盘本身是被磁化的，圆盘的旋转可将磁力线扭曲成螺旋线圈状。
Because the accretion disk itself is believed to be magnetized, the rotation of the disk can twist the magnetic field lines into a helix.
我们可以将很多发生在黑洞对合并时的气体环境和吸积盘里的物理过程与引力辐射联系起来。
We'd be able to connect a lot of the physics happening within the gaseous environment and accretion disk to the binary black hole merger to the gravitational radiation.
宇宙中一系列高光度或者高频率辐射的高能现象可以由吸积过程解释其物理机制。
A range of high-energy phenomena about large luminosity or high frequency radiation can be explained by accretion.
这个模型是指气体从大型红巨星伴星流到白矮星的吸积盘上然后被吸进白矮星中。
In this model, gas flows from the large red giant companion star into a disk and then onto the White Dwarf.
对于静态、绝热吸积流，比能量E、比角动量L和质量吸积率M都是空间的常量。
For a stationary, adiabatic flow the specific energy E, specific angular momentum L and mass accretion rate M are constant in space.
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。
The conclusion is: the short term variability behavior provides a strong support to the thick accretion disk model of AGN.
然而，物理上合理的整体解却是唯一的，它总是使两个吸积率值中之较小者得到实现。
However, the physically acceptable global solution is unique: it is always realized for the smaller of the two accretion rates.
我们利用吸积盘中新的反常磁普朗特数来研究耗散过程对开普勒盘磁不稳定性的影响。
Using the new ?anomalous magnetic Prandtl number? in accretion disks, we study the effect of dissipation on magnetic instability of Keplerian disks.
我们利用吸积盘中新的反常磁普朗特数来研究耗散过程对开普勒盘磁不稳定性的影响。
Using the new ?anomalous magnetic Prandtl number? in accretion disks, we study the effect of dissipation on magnetic instability of Keplerian disks.
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