There's a problem with the accelerating rate of the expansion of the Universe.
宇宙膨脹的加速速度存在一個問題。
More specifically, there's a problem with how we measure the accelerating rate of the expansion of the Universe, called the Hubble Constant.
更具體地說，我們如何測量宇宙膨脹的加速速率，稱為哈勃常數，存在一個問題。
We have two major methods for measuring the Hubble Constant, and no matter how many times we apply them, they always return different results.
我們有兩種主要的測量哈勃常數的方法，無論我們使用它們多少次，它們總是返回不同的結果。
This has led some to suggest we need new physics to explain the discrepancy.
這導致一些人建議我們需要新的物理學來解釋這種差異。
But theoretical physicist Lucas Lombriser of the University of Geneva in Switzerland has come up with a different approach.
但是瑞士日內瓦大學的理論物理學家Lucas Lombriser提出了一種不同的方法。
According to Lombriser, if the Milky Way galaxy is floating in a vast low-density cavity in space, that could explain why the measurements don't match up.
根據Lombriser的說法，如果銀河系漂浮在太空中巨大的低密度空腔中，這就可以解釋為什麼測量結果不匹配。
By adjusting our equations to account for that density difference, we could significantly reduce the measurement gap.
通過調整我們的方程來考慮密度差異，我們可以顯著減小測量間隙。
But before we get into that, we need to briefly explain the two measurements of the Hubble Constant.
但在我們開始之前，我們需要簡要解釋哈勃常數的兩個測量值。
The first is based on the cosmic microwave background (CMB), the faint glow of background radiation permeating the Universe, left over from the Big Bang.
第一個是基於宇宙微波背景(CMB)，即宇宙大爆炸遺留下來的背景輻射滲透宇宙的微弱輝光。
The CMB has been pretty comprehensively mapped by a number of surveys, so we know it has hotter and cooler regions that correspond with expansions and contractions of matter in the early Universe.
許多調查已經相當全面地繪製了CMB的地圖，所以我們知道它有更熱和更冷的區域，與早期宇宙中物質的膨脹和收縮相對應。
These can be studied to learn about the expansion history of the Universe.
這些可以被研究來了解宇宙的膨脹歷史。
Based on this information, calculations of the Hubble Constant usually return a result hanging around the vicinity of around 67.4 kilometres per second per megaparsec.
基於這些信息，哈勃常數的計算通常會得到大約67.4千米每秒的結果。
The other method for arriving at the Hubble Constant involves measuring the distances to objects with known brightness, such as extremely bright Type Ia supernovae and Cepheid variable stars, a type of star that has a known relationship between its brightness and its periodic pulsations.
得出哈勃常數的另一種方法涉及測量到已知亮度的物體的距離，例如極明亮的Ia型超新星和造父變星，這是一種已知的恆星，其亮度和週期脈動之間存在已知的關係。
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