remaining hydrogen

简明释义

残留氢

英英释义

例句

1.The technician checked the gauge for remaining hydrogen before starting the experiment.

技术人员在开始实验前检查了剩余氢气的表盘。

2.After the reaction, we measured the amount of remaining hydrogen to ensure it was safe to proceed.

反应后，我们测量了剩余的氢气量，以确保可以安全进行。

3.To calculate the efficiency of the process, we need to know the remaining hydrogen after each cycle.

为了计算过程的效率，我们需要知道每个周期后的剩余氢气。

4.The fuel cell only operates efficiently when there is enough remaining hydrogen in the tank.

燃料电池只有在油箱中有足够的剩余氢气时才能高效运行。

5.Engine performance can be affected by the level of remaining hydrogen in the system.

系统中剩余氢气的水平会影响发动机性能。

作文

In the vast universe, hydrogen is the most abundant element, making up about 74% of the elemental mass of the universe. However, as stars evolve and go through various stages of their life cycles, they consume a significant portion of this hydrogen. The concept of remaining hydrogen (剩余氢) becomes crucial when discussing the life expectancy of stars and the chemical processes that occur within them. Understanding how much remaining hydrogen (剩余氢) exists in a star can help astronomers predict its future and the eventual formation of elements heavier than hydrogen. For instance, our Sun, which is currently in the middle of its life cycle, has a core composed primarily of hydrogen. As it fuses hydrogen into helium through nuclear fusion, the amount of remaining hydrogen (剩余氢) decreases over time. Scientists estimate that the Sun has enough remaining hydrogen (剩余氢) to continue its fusion process for approximately another 5 billion years. After this period, the Sun will exhaust its supply of hydrogen, leading to dramatic changes such as expanding into a red giant and ultimately shedding its outer layers to form a planetary nebula.The study of remaining hydrogen (剩余氢) is not limited to just stars like our Sun; it also plays a vital role in understanding the formation of galaxies and the evolution of the universe itself. In the early universe, vast clouds of hydrogen gas coalesced under gravity to form the first stars. As these stars lived and died, they enriched the surrounding medium with heavier elements while consuming much of the remaining hydrogen (剩余氢). This process is essential for the formation of new stars and planets, as the availability of remaining hydrogen (剩余氢) influences star formation rates.Moreover, the remaining hydrogen (剩余氢) in interstellar space is a critical factor in astrophysics. When scientists observe regions of space where remaining hydrogen (剩余氢) is still plentiful, they often find areas of active star formation. These regions, known as molecular clouds, are dense and cold, providing the perfect conditions for hydrogen atoms to clump together and eventually form new stars. Thus, the presence of remaining hydrogen (剩余氢) is an indicator of potential star birth and the ongoing cycle of matter in the universe.In conclusion, the study of remaining hydrogen (剩余氢) is essential for understanding the lifecycle of stars, the formation of galaxies, and the evolution of the universe. It serves as a key component in the complex web of cosmic events that shape our understanding of the cosmos. By examining the remaining hydrogen (剩余氢) in various celestial bodies, astronomers can gain insights into the past, present, and future of the universe, allowing us to appreciate the intricate dance of creation and destruction that defines the cosmos.