| 1. | Electron degenerate pressure
电子简并压力 |
| 2. | Neutron degenerate pressure
中子简并压力 |
| 3. | The electron degenerate pressure does not come from the burning of any nuclear fuel and can therefore support the star from further gravitational contraction forever
电子简并压力并非来自任何核反应所以它能永远抵抗恒星的引力。 |
| 4. | Can stop the star from further collapsing . note : again , neutron degenerate pressure does not come from nuclear burning . it can support a neutron star from further gravitational contraction forever
则足以防止恒星进一步收缩同电子简并压力一样中子简并压力并非来自核子反应它可永远?抗恒星的引力收缩。 |
| 5. | Stops it from further contracting . an extremely simplified , but not totally correct , picture is that the electron degenerate pressure develops when the electrons are touching each others
虽然过于简略和不准确，但电子简并压力可勉强看成是来自电子挤至互相触碰时所造成的抵抗力成为了抵抗恒星进一步塌缩的主要力量。 |
| 6. | Nature of the universe - chapter seventeen if the remnant of a supernova explosion is heavier than two or three solar masses , the neutron degenerate pressure is not strong enough to support the star . there does not exist stronger force up to our knowledge and we believe the remnant will collapse to a black hole
在超新星爆发后，如果恒星剩馀质量超过二或三个太阳质量，中子简并压力亦不足以抵抗向内的引力，这时在已知的物理理论里面，再没有更强的力能足以与引力一决雌雄，恒星只可以不断塌缩，成为黑洞。 |
| 7. | If the mass of the core after a supernova explosion is more than 1 . 4 but less than about 3 solar masses , then electron degenerate pressure is not strong enough to support the star . the star will contract to a size even smaller than the white dwarf . the electrons are squeezed into the nuclei and are combined with the protons to form neutrons
假若在超新星爆发后，剩馀核心质量介乎太阳质量的1 . 4至3倍，那么核心中的电子简并压力便再不足以抵抗强大的引力，恒星会进一步收缩，直至电子亦被挤压至原子核内，和质子结合成为中子。 |
