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helium white dwarf 氦白矮星
It will quietly and steadily burn the hydrogen to helium and become a white dwarf. 它会稳定地把氢转化为氦,然后安静的死去,成为白矮星。
It is then referred to as a White Dwarf. 这时，它被称为白矮星。
Each white dwarf is a burned up, dying star like the sun. 每个白矮星都是类似于太阳燃烬后残存的恒星，
A white dwarf is the inert remnant of what used to be a sunlike star. 白矮星是类似太阳的恒星在死亡后所留下恒久不变的残骸。
As the white dwarf spins, the columns of infalling gas rotate with it. 当白矮星自转时，被吸入的气柱也跟著一起转起来。
Since a 7-solar-mass is too large to be a white dwarf or neutron star,it must be a black hole. 因为有着7个太阳质量的星体不可能是白矮星或中于星，所以它一定是黑洞。
The researchers suggest that there are many white dwarf stars throughout this halo. 研究人员猜想，光晕内到处有白矮星。
The nova phenomenon generally occurs in a binary system that has as one member a very hot white dwarf. 新星这种现象一般发生在双星系统中，其中一颗子星是非常热的白矮星。
Recall that Type I supernova is the strong explosion of a nova that even the white dwarf is destroyed. 还记得I型超新星是足以令中心白矮星炸毁的新星爆发吗?
It would take only an hour for the white dwarf to smash through, but the damage would be irreversible. 白矮星只需要一个小时就可以猛穿而过，但其所造成的破坏是无法挽回的。
Since a 7-solar-mass is too large to be a white dwarf or neutron star, it must be a black hole. 因为有着7个太阳质量的星体不可能是白矮星或中于星，所以它一定是黑洞。
Except for an anomalously high surface abundance of nitrogen, the white dwarf should appear unchanged. 除非表面含氮量异常之高，白矮星应该不会显出变化。
The atmospheres of white dwarfs usually consist entirely of hydrogen and helium, but sometimes heavier elements such as calcium or magnesium are detected contaminating the stellar material. 白矮星的大气通常完全是氢和氦,但是有时会在其天体组成中检测到重元素污染,比如钙和镁。
Data from the Chandra observation show that the central ten-million-degree Celsius cloud is the remains of a supernova explosion that destroyed a white dwarf star. 来自钱德拉的观测数据表明，中心温度达上千万摄氏度的云湍团是超新星爆发的残余，爆发摧毁了一颗白矮星。
Novae occur in double star systems comprising a white dwarf - the end product of a solar-like star - and, generally, a low-mass normal star - a red dwarf. 双星系统中包含一个白矮星（类似太阳的恒星的最终演化产品）和一个红矮星（一种低质量的普通星球）。
Every 20 years or so, the red giant star dumps enough hydrogen gas onto its companion white dwarf star to set off a brilliant thermonuclear explosion on the white dwarf's surface. 大约每过20年，红巨星向它的白矮伴星上输出足够的氢气，在白矮星表面产生一次耀眼的热核爆炸。
If the mass of the white dwarf becomes greater than about 1.4 times the mass of the Sun, it becomes unstable and is blown apart in a thermonuclear explosion. 如果白矮星的质量超过了太阳的1.;4倍，它会变得不稳定，并在热核爆炸中碎裂。
The remnant central stellar core, destined to become a white dwarf star, glows in light so energetic it causes the previously expelled gas to fluoresce. 中央残留的恒星核注定会变成一颗白矮星，发出强光，使得先前喷出的气体发出荧光。
Although white dwarf cosmochronology is still in its infancy, it already shows its potential as a powerful tool for estimating the ages of the various objects. 白矮星宇宙纪年学是一个很新的研究领域，但它已经在确定天体年龄方面显示出很大的潜力。