Final Stages of Stellar Evolution
Final Stages of Stellar Evolution
复制标题
恒星演化的最后阶段
DOI：
10.1007/978-3-642-14734-0_5
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发表时间：
2010
期刊：
影响因子：
--
通讯作者：
G. Bisnovatyi
中科院分区：
文献类型：
--
作者：
G. Bisnovatyi
在演化的最后阶段，核燃料被消耗，恒星由于冷却而发出辐射。它相对较冷，密度很高，而压力主要来自物质简并。1931年，Chandrasekhar[322]获得了一个基本结果，即由于简并电子而产生压力的恒星具有最大质量。在ρ>；1.15×109g cm−3(对于56Fe，对于其他核，参见表10.1)，中子化开始，恒星变得不稳定。稳定(中子星)星仅在ρc≈1.5x1014g cm−3时再现，并存在密度为ρc≈1.15×1015g cm−3时，其不稳定性源于广义相对论(GR)效应。奥本海默和沃尔科夫在1939年确定了中子星质量极限的存在[517]，但对于各种状态方程，它的值已经被重新计算了很多次。在给定的状态方程P(ρ)下求解牛顿理论(9.3.13a)和(10.1.1a)以及GR(11.2.3)和(11.2.4)中的冷星平衡方程，得到了证明存在两个最大质量和一个不稳定区域(下落M(ρc))的曲线M(ρc)。图11表示与处于完全热力学平衡的物质的最小能量相对应的状态方程的曲线M(ρc)。
During the final evolutionary stages the nuclear fuel is consumed, and the star emits radiation owing to cooling. It is relatively cold and has a very high density, while the pressure arises mainly from the matter degeneracy. Chandrasekhar [322] in 1931 obtained the fundamental result that a star where the pressure is due to degenerate electrons has a maximum mass. At ρ > 1.15 × 109 g cm−3 (for 56Fe, for other nuclei see Table 10.1) the neutronization begins, and stars become unstable. Stable (neutron) stars reappear only at ρ c ≈ 1.5 × 1014 g cm−3 and exist to densities ρ c ≈ 1.15 × 1015 g cm−3, where instability arises from general relativity (GR) effects. Oppenheimer and Volkov established in 1939 the existence of a mass limit for neutron stars [517], but its value has been recalculated many times for various equations of state. Solving the equilibrium equations for cold stars in Newtonian theory (9.3.13a) and (10.1.1a) and in GR (11.2.3) and (11.2.4) at a given equation of state P(ρ) has allowed derivation of the curve M(ρ c ) demonstrating the existence of two maximum masses and an instability region (falling M(ρ c )). Figure 11.1 represents the curve M(ρ c ) from [267] for the equation of state corresponding to a minimum energy of matter in full thermodynamic equilibrium.
影响因子：
2.2
作者：
M. Barkov;S. Komissarov
通讯作者：
M. Barkov;S. Komissarov
DOI：
10.1111/j.1365-2966.2009.15792.x
发表时间：
2009-08
影响因子：
4.8
作者：
M. Barkov;S. Komissarov
通讯作者：
M. Barkov;S. Komissarov