The phase transition from nuclear matter to quark matter during proto‐neutron star evolution
The phase transition from nuclear matter to quark matter during proto‐neutron star evolution
复制标题
原中子星演化过程中从核物质到夸克物质的相变
DOI：
10.1046/j.1365-8711.1999.02458.x
复制
发表时间：
1999
影响因子：
4.8
通讯作者：
G. Lugones
中科院分区：
文献类型：
--
作者：
O. Benvenuto;G. Lugones
我们探讨了原中子星中从核物质到夸克物质的相变的发生。为此，我们采用最近的结果，在电子-中微子-简并气体的存在下，这样的相变的基础上，平均场模型核状态方程连同夸克物质状态方程所描述的麻省理工学院的“袋模型”。这些结果表明，这种中微子气体不利于跃迁。通过与Keil & Janka的原中子星星演化计算的比较，我们发现，当袋常数B的值B ≤ 126 MeV fm-3时，确实发生了退禁闭跃迁。我们还发现，当B ≥ 100 MeV fm-3时，中微子的存在将使相变延迟几秒，从而为神冈台组在SN 1987 A中探测到的中微子发射的第二个峰值提供了一个自然的解释。向夸克物质的转变及其随后的衰变应该会以一种非平凡的方式影响原中子星星的演化和超新星爆炸。
We explore the occurrence of a phase transition from nuclear matter to quark matter in proto-neutron stars. To this end, we employ recent results on such a phase transition in the presence of an electron--neutrino--degenerate gas, based on a mean field model nuclear equation of state together with a quark matter equation of state as described by the MIT `bag model'. Those results show that this neutrino gas does not favour the transition. By comparison with the proto-neutron star evolutionary calculations of Keil & Janka, we find that, if the bag constant B has a value B ≤ 126 MeV fm-3, the deconfinement transition indeed occurs. We also find that, if B ≥ 100 MeV fm-3, the phase transition is delayed by the presence of neutrinos by a few seconds after core bounce, thus providing a natural explanation for the second peak of neutrino emission detected in SN 1987A by the Kamiokande Group. The transition to quark matter and its subsequent decay should affect proto-neutron star evolution and supernova explosions in a non-trivial way.
影响因子：
8.6
作者：
HIRATA, K;KAJITA, T;CORTEZ, BG
通讯作者：
CORTEZ, BG