| 1. | Hydrogen to helium conversion provides the prime source of energy for stars on the main sequence .
由氢向氦的转变是主序星能量的主要来源。 |
| 2. | And stars in this region are called main sequence stars
，位于此区域的星则称为主序星。 |
| 3. | It takes about 0 . 1 to 100 million years for the cloud to become a main sequence star
这个收缩过程需要十万至一亿年，才能演化成一颗主序星。 |
| 4. | After it reaches the main sequence , the star will stay there for millions to billions of years
一般恒星会在主序星阶段逗留一百万至一百亿年。 |
| 5. | The corona activity of late - type main sequence stars also depend on the stellar spectral type
晚型主序星的冕球活动也表现出对恒星光谱型的依赖性。 |
| 6. | The corona activity of late - type ms stars exist a inflexion nearby f5 . there have two fold reason
分析结果显示f型主序星的冕球活动在光谱型f5附近存在拐点。 |
| 7. | The corona activity of g , k , m type stars decrease with color index increasing as a whole
但是m型主序星的冕球活动是随色指数的增大而下降，这与m型主序星色球活动的行为相反。 |
| 8. | Main sequence stars have stable luminosities and sizes . to be honest , they are quite boring compare to their deaths
主序星的光度和大小十分稳定，或者你可以说相对于恒星的死亡舞曲，主序阶段相当沈闷。 |
| 9. | When a star is at the main sequence stage , its interior continuously fuses four hydrogen nuclei i . e . protons into one helium nucleus
在主序星阶段，恒星内部不断把四粒氢原子核即质子融合成一颗氦原子核。 |
| 10. | B . the surge of nuclear fusion would expand the gas in the core , cooling the core back down and quickly returning the nuclear fusion rate to normal
太阳会变成一个更大、更热、更明亮的主序星并且会保持这种状态直到核心的氢燃料用尽为止。 |
