And... And right in the middle, there's a variable star that I discovered.

而… … 而在正央有我所发现的变星。

In 1925, when Edwin Hubble looked at the brightness of variable stars in a smudge called Andromeda, they appeared much dimmer than their pulsing rate predicted, and Hubble realized these stars were too far away to be in the MilkyWay.

1925 年当 Edwin Hubble 看着仙女座星体各种变星的亮度，发现它们的亮度比预测的要暗的多，并且 Hubble 也认识到这些星在个很远的地方，不可能是在银河系内。

They observed variable stars in the Andromeda Galaxy that allowed them to get the distance to the galaxy.

他们观测了仙女座星系的变星，这使得他们能够到达星系的距离。

While studying what we now call the Andromeda  galaxy in 1923, Hubble realised that one of the stars he was looking at was a Cepheid variable  star – a type of star that blinks brighter and dimmer over the course of weeks.

1923 年，在研究我们现在所说的仙女座星系时，哈勃意识到他所看到的星是造父变星——种在几周内闪烁得更亮和更暗的星。

'I am preparing a work on variable stars. There is one of these which I have exceptionally observed for several months, and on this my great theory is mainly based.

“我正在准备部关于变星的作品。之是我几个月来特别观察到的，我的伟大理论主要基于此。

Actual variable stars do exist, but Tabby's Star doesn't fit that profile, it's what's known as an F-type main-sequence star, and shouldn't behave anything like this.

实际的变星确实存在， 但 Tabby's Star 不符合这种情况，它是所谓的 F 型主序星， 不应该有这样的行为。

In this way, Cepheid variables act like standard candles, and Edwin Hubble used these variable stars to measure the distance in the first place.

通过这种方式， 造父变星就像标准烛光，埃德温·哈勃最初就是利用这些变星来测量距离的。

The Cepheid variable stars that Leavitt studied are in the Magellanic clouds, known today to be galaxies outside the Milky Way.

勒维特研究的造父变星位于麦哲伦云，如今已知这些云是银河系外的星系。

Leavitt discovered more than 2,400 variable stars and four novae.

莱维特发现了超过2400变星和四新星。

It was the review of a pamphlet by an American astronomer, in which the author announced a conclusive discovery with regard to variable stars.

那是位美国天文学家对本小册子的评论，作者在书宣布了关于变星的个结论性发现。

Like all other variable stars, Cepheids progress through a complete cycle from maximum brightness to a minimum and then back to maximum again.

像所有他变星样，造父变星会从最大亮度变化到最小亮度，然后再回到最大亮度，完成个完整周期。

Compared with comets, variable stars, which he had hitherto made his study, were, from their remoteness, uninteresting. They were to the former as the celebrities of Ujiji or Unyamwesi to the celebrities of his own country.

与彗星相比，他迄今直在研究的变星由于距离遥远而显得乏味。他们之于前者就像乌吉吉的名人或乌尼亚姆维西之于他自己国家的名人。

Cepheid variables are reasonably easy to recognize because they are among the brightest variable stars, and they have a characteristic light curve, showing fairly rapid increases in brightness followed by a slower tailing off.

造父变星相当容易识别， 因为它们是亮度最高的变星之，并且具有典型的光变曲线，显示出亮度相当迅速的增加， 随后是较为缓慢的减弱过程。

One of the most striking accomplishments of Miss Leavitt was the discovery of 1777 variable stars in the Magellanic clouds.

莱维特小姐最引人注目的成就之，是在麦哲伦云发现了1777变星。

Much of her research focused on variable stars and novae, exploding white dwarfs.

她的研究有很大部分集在变星和新星，即正在爆炸的白矮星上。

His strategy was to search for Cepheid variable stars, stars whose luminosity changes predictably, within nebulae, and to measure their distances from Earth.

他的策略是在星云内部寻找造父变星，这种星星的亮度变化可预测，并测量它们与地球的距离。

Many were out by a factor of 7 due to his method of taking the brightest star in any galaxy, or even the luminosity of the galaxy itself, and assuming it to be a Cepheid variable star.

许多测量结果因7倍之差而偏离， 这是由于他采用的方法：选取任意星系最亮的星，甚至星系本身的亮度，并假设为造父变星。

This mainly involved measuring the brightness of stars, but a specific aspect of Leavitt's work was to identify stars that fluctuate in brightness, known as variable stars.

这主要涉及测量星的亮度，但莱维特工作的个特定方面是识别亮度波动的星，即所谓的变星。

After 1912 Henrietta Swan Leavitt discovers a link between the period of a type of variable star and its brightness, allowing these stars to be used as standard candles for working out distances.

1912年后， 亨丽爱塔·斯万·莱维特发现了某种变星的周期与亮度之间的关联，这使得这类星星能被用作测量距离的标准烛光。

In this way, it should also be possible to determine the distance to any object that contained one or more Cepheid variable star.

这样来，确定包含个或多个造父变星的任何天体的距离也应成为可能。