当一颗白矮星以这种方式增长到足够的质量时，它将达到钱德拉·塞卡极限。
When a White Dwarf takes on enough mass in this manner, it reaches a level called the chandrasekhar limit.
目前白矮星的理论模型不能模拟这种行为。
Our current theoretical models of white dwarfs don't predict this sort of behavior.
有一类白矮星的大气层几乎完全由纯氦气构成。
One class of white dwarfs has almost pure helium atmospheres.
这部小说像一个白矮星，通篇篇幅大却又缜密。
讨论过白矮星，一个白矮星半径约为。
相对的，它们最终只是会变冷成为白矮星和黑矮星。
Instead, they should eventually just cool to become white dwarfs and then black dwarves.
白矮星的质量只有以前的一半，体积很小，因此非常致密。
A White Dwarf retains about half of its mass but becomes incredibly dense because of its small size.
不过并不是所有的白矮星都有耐性等上无数个千年。
But not all white dwarfs will spend many millennia cooling their heels.
GD 362是颗白矮星，距离地球150光年，也在银河系。
The star was a White Dwarf called GD 362, and it's 150 light years from Earth, still within our galaxy.
而白矮星则是将其曾用作核燃料的所有氢原子都燃烧殆尽的恒星。
White dwarfs are stars that have burned up all of the hydrogen they once used as nuclear fuel.
估算白矮星冷却的时间长度有助于天文学家深入研究宇宙的年龄。
Estimating how long white dwarfs have been cooling can help astronomers learn much about the age of the universe.
这类白矮星中有着重元素痕迹者，大多也会有氢的痕迹。
Among this group, most of those with traces of heavy elements also have traces of hydrogen.
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.
太阳在50亿年后也将变成白矮星，届时将摧毁水星、金星甚至地球。
Our sun should become a White Dwarf in about five billion years. The process will destroy Mercury, Venus and possibly Earth.
第一颗目标恒星是武仙星群中一颗称为GD358的白矮星。
The primary target is a White Dwarf star known as GD358 in the constellation Hercules.
恒星的中心变成了白矮星，曾经非常热(10万k)非常小。
The center of that star then transformed into a White Dwarf, at once very hot (more than 100, 000 Kelvin) and very small.
白矮星是恒星的残余，已经开始降温了，我们的太阳就是如此。
White dwarves are the remnants of stars like our sun that start to cool.
这颗和我们太阳类似的恒星，已经安然逝去并演变成了一颗密实的白矮星。
The star, which was similar to our sun, had died peacefully and turned into a dense White Dwarf.
炽热的恒星内核会在几十亿年里逐渐冷却，内核在这段时间里叫做白矮星。
The hot, remnant stellar core of NGC 2818 will eventually cool off for billions of years as a White Dwarf.
因为，当一颗靠近白矮星的行星路过它的时候，会使它发出的光线变的模糊不清。
Because a planet that close to its star would dim the dwarf's light as it passes.
某天，几百万年后，LSIV - 14 116将会冷却形成真正的白矮星。
Some day, millions of years from now, LS IV-14 116 will cool off to the point where it becomes a bona fide White Dwarf.
那些双星系统中的白矮星可能有足够强大的引力，能从伴星上吸聚物质。
Those in a binary star system may have a strong enough gravitational pull to gather in material from a neighboring star.
Provencal表示，白矮星是一颗“死”恒星，不像太阳那样自己生成能量。
A White Dwarf is a "dead" star that doesn't generate its own energy like the sun does, Provencal says.
在几百亿年甚至几千亿年之后，白矮星最终冷却形成黑矮星，后者不再散发任何能量。
Eventually—over tens or even hundreds of billions of years—a white dwarf cools until it becomes a black dwarf, which emits no energy.
由于白矮星的质量处在有个亿范围之内，两个星体的并合会导致亮度有些许变化的爆发。
Because white dwarfs can come in a range of masses, the merger of two could result in explosions that vary somewhat in brightness.
这导致研究人员怀疑一个迷途的白矮星离某个中等质量黑洞太接近了，并受其潮汐引力的撕扯。
This leads the researchers to suspect that a whitedwarf star strayed too close to the intermediate-mass black hole andwas ripped apart by tidal forces.
这导致研究人员怀疑一个迷途的白矮星离某个中等质量黑洞太接近了，并受其潮汐引力的撕扯。
This leads the researchers to suspect that a white dwarf star strayed too close to the intermediate-mass black hole and was ripped apart by tidal forces.
因此我们自己这颗含水行星的最终命运可能便是短暂地污染已经变成白矮星的太阳的大气层。
So the ultimate fate of our own watery planet may be to briefly stain the atmosphere of the white-dwarf sun.
因此我们自己这颗含水行星的最终命运可能便是短暂地污染已经变成白矮星的太阳的大气层。
So the ultimate fate of our own watery planet may be to briefly stain the atmosphere of the white-dwarf sun.
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