因为AGB超星风仅仅发生在AGB的最后阶段,所以在超星风发生重要作用之前,中等质量AGB的简并核可以达到钱德拉塞卡极限。
Since AGB superwind only occurs at the final stage of AGB stars, it may allow the degenerate core of intermediate-mass AGB star to reach the Chandresekhar mass before the AGB superwind.
当一颗白矮星以这种方式增长到足够的质量时,它将达到钱德拉·塞卡极限。
When a White Dwarf takes on enough mass in this manner, it reaches a level called the chandrasekhar limit.
当一颗白矮星以这种方式增长到足够的质量时,它将达到一个称为钱德拉·塞卡极限的质量标准。
When a White Dwarf takes on enough mass in this manner it reaches a level called the chandrasekhar limit.
最终中子恒星中暗物质恒星的质量会超过它的“钱德拉·塞卡极限(Chandrashekar limit)——超过了这个极限值,一个恒星就经受不住引力所引起的压力。”
Eventually, the mass of the dark matter star would exceed its "Chandrashekar limit" - beyond which a star cannot withstand gravitational pressure.
最终中子恒星中暗物质恒星的质量会超过它的“钱德拉·塞卡极限(Chandrashekar limit)——超过了这个极限值,一个恒星就经受不住引力所引起的压力。”
Eventually, the mass of the dark matter star would exceed its "Chandrashekar limit" - beyond which a star cannot withstand gravitational pressure.
应用推荐