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造父变星

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Cepheid variable stars – a class of stars named in honor of Delta Cephei – serve as cosmic yardsticks, enabling astronomers to measure the distances to faraway galaxies.

造父变星——以Delta Cephei的名义命名的一类星——充当宇宙的标尺,使得天文学家可以测量与更为遥远的星系之间的距离。

The SHOES team used Hubble's Near Infrared Camera and Multi-Object Spectrometer and the Advanced Camera for Surveys to observe 240 Cepheid variable stars across seven galaxies.

SHOES团队使用哈勃望远镜的近红外相机和多目标光谱仪、高级巡天相机观测了综括7个星系的240颗造父变星

Cepheids are reliable cosmic distance mileposts. The interval it takes for the Cepheid to complete one pulsation is a direct indication of the stars';s intrinsic brightness.

造父变星是可靠的宇宙距离里程碑,其完整的一个光变周期直接反映了星体的本质光亮度。

The new technique reduced the distance ladder to three "rungs":(1) The distance to galaxy NGC4258 is measured using straightforward geometry and Kepler's laws;(2)Cepheids in six more distant galaxies are used to calibrate the luminosity of Type Ia supernovae;(3) The Hubble constant is measured by observing a brighter milepost marker, Type Ia supernovae, in more distant galaxies hundreds of millions of light-years away, embedded in the expanding universe.

这种新技巧简化了距离跳跃为三个"阶梯":1、星系NGC 4258的距离采用开普勒定律和简单直接的几何方法精确测量;2、在6个更远的星系中的造父变星用来校准Ia超新星的光度;3、深嵌于数亿光年外的膨胀宇宙中的星系中的Ia超新星——一种遥远而明亮的量天尺,被用于精确测定哈勃常数。

At the dimmest part of a Cepheid's cycle, the ionized gas in the outer layers of the star is opaque, and so is heated by the star's radiation, and due to the increased temperature, begins to expand.

造父变星的一个光变周期开始时,恒星最暗,此时其外层电离气体是相对不透明的,因此会吸收恒星的辐射而升温,并开始向外膨胀。

Cepheids dim and brighten regularly, in a pattern that depends on their brightness.

造父变星依据它们的亮度有规律的变明变暗。

Although Cepheids are rare, they provide a very reliable"standard candle" for estimating intergalactic distances.

虽然造父变星数量稀少,它们是估计银河系间距离的一种非常可靠的&标准烛光&。

To reduce the uncertainty in virgo's distance, freedman and her colleagues will search for cepheids in two other galaxies in virgo.

为减少室女星团距离计算上的不确定因素,弗里德曼及其同事准备在室女星团的另两个星系内寻找造父变星

IUsing 146 cepheids selected from the data listed by Kraft and Schmidt,the variation of Δω with R is computed by means of Camm's method.

i利用克拉夫特和施密特列出的造父变星资料中146个星的资料,用加姆方法计算了Δω随 R 的变化。

With Hubble's powerful capabilities, the team was able to side step some of the shakiest rungs along the previous distance ladder involving uncertainties in the behavior of Cepheids.

有了哈勃望远镜的强大能力,团队就能直接跨过某些不稳定的台阶:先前对这些造父变星行为的观测不是很准确。

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