恒星

The region is in the Large Magellanic Cloud, a satellite of our Milky Way galaxy. It is a fascinating laboratory for observing star-formation regions and their evolution.

这个区域位于我们银河系的伴星系——大麦哲伦云，这个是观察恒星诞生、演化的迷人实验室。

In order to find out the origin of this secondary feature, the astronomers monitored 58 stars in our galactic neighbour, the Large Magellanic Cloud, over two and a half years.

为了找出这种次要周期的起源，天文学家在我们的邻居——大麦哲伦星系中连续监测了58个恒星，时间超过两年半。

Dwarf galaxies such as the Small Magellanic Cloud, with significantly fewer stars compared to our own galaxy, are considered to be the primitive building blocks of larger galaxies.

如小麦哲伦云这样的矮星系——与我们的银河系相比恒星数少得多——被认为是巨星系的形成基础。

Yet, the modern reader would not rate this accomplishment among Galileo's noblest achievements, nor do we refer to Io, Europa, Callisto, and Ganymede as the Medicean stars, planets, or moons, or indeed, as the Medicean anything.

然而，现代读者仍未视此为伽利略最高尚的成就，我们也不指称Io、Europa、Callisto、及Ganymede为麦第奇恒星、行星或卫星，或者把它们当成实际上归属於麦第奇家族的任何事物。

Our observations do not suggest that Li is unaffected by metallicity and/or age.

但是我们的观测不能锂一点也不受恒星金属性或年龄的的影响。

It is known that solar-type stars with high metallicity have a high probability of hosting planets.

因此，高金属性的类太阳恒星很有可能被行星绕转。

This metallicity excess is also present in the solar analogue planet-bearing stars see Fig.

这些恒星的高金属性也可能加剧锂的衰减吗？

The increasing trend at lower metallicity can not be confirmed because of the measurement accuracy.

3晕族恒星中都表现出超丰0.4 dex，但有一定的弥散，在更低金属丰度时超丰是否增加因为观测精度的限制还不能确定。

2C. Can high metallicity be responsible for enhanced Li depletion in these stars?

在类太阳恒星中金属不透明度的增加也可能致使辐射层及对流层之间能量的交换。

Comparison with field stars then leads to the conclusion that neither age nor metallicity is responsible for the excess Li depletion.

通过以上分析，我们可以说锂的过度消耗无论和恒星年龄还是其金属丰度都没有相关性。

The split between the two groups can hardly be papered over.

这两个团体间的分歧难以掩饰。

This approach not only encourages a greater number of responses, but minimizes the likelihood of stale groupthink.

这种做法不仅鼓励了更多的反应，而且减少跟风的可能性。