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

而… … 而在正中央有一颗我所发现变星。

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中变星，这使得他们能够到达星离。

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

她研究有很大一部分集中在变星和新星，即正在爆炸白矮星上。

A celestial body that has a known luminosity, such as a Cepheid variable star.

已知光天体，如造父变星。

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

莱维特发现了超过2400颗变星和四颗新星。

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之一，是在麦哲伦云中发现了1777颗变星。

I observe from seven or eight till about two in the morning, with a view to my great work on variable stars.

我从七八点观察到凌晨两点左右， 以期我在变星方面伟大工作。

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

像所有其他变星一样，造父变星会从最大亮变化到最小亮，然后再回到最大亮，一个整周期。

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

他策略是在星云内部寻找造父变星，这种星星亮变化可预测，并测量它们与地球离。

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， 造父变星像标准烛光，埃德温·哈勃最初是利用这些变星来测量离。

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

这样一来，确定包含一个或多个造父变星任何天体离也应为可能。

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

勒维特研究造父变星位于麦哲伦云中，如今已知这些云是银河外星。

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

那是一位美国天文学家对一本小册子评论，作者在书中宣布了关于变星一个结论性发现。

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.

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

In 1609, Fabricius confirmed that Myra Cetaei was a periodic variable star, showing that, contrary to the prevailing Greek philosophy that the cosmos was unchanging, stars were not constant.

1609年， Fabricius确认Myra Cetaei是一颗周期性变星，表明与当时流行希腊哲学认为宇宙不变观点相反，恒星并不是恒定不变。

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.

这主要涉及测量恒星亮，但莱维特工作一个特定方面是识别亮波动恒星，即所谓变星。

'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.

“我正在准备一部关于变星作品。其中之一是我几个月来特别观察到，我伟大理论主要基于此。

'I have made an amazing discovery in connexion with the variable stars, ' he exclaimed. 'It will excite the whole astronomical world, and the world outside but little less.

“我在变星方面有了惊人发现，”他惊呼道。 “它会激发整个天文界兴奋，而外面世界却不会那么兴奋。”

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周期与其亮之间关联，这使得这类星星能被用作测量离标准烛光。

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， 因为它们是亮最高变星之一，并且具有典型光变曲线，显示出亮相当迅速增加， 随后是较为缓慢减弱过程。