density region 3.1x10 11 to 2x10 15 g/cm 3/ A2165 Nuclear matter A9760J Neutron starsThe equation of state and the structure and composition of neutron star matter are investigated in the density region 3.1 × 10 112 × 10 15g/cm 3. Below the density 3.1 × 10 11 g/cm 3 the ...
arXiv:1301.5189v1 [astro-ph.CO] 22 Jan 2013General Relativity and Gravitation manuscript No.(will be inserted by the editor)Structure of neutron stars in R-squared gravityMariana Orellana1,2,∗· Federico Garc´ıa1,2,∗∗· Florencia A. TeppaPannia2,∗∗· Gustavo E. Romero1,...
One of the most intriguing consequence of the extreme conditions inside neutron stars is the possibility of the natural existence of a deconfined strange quark matter phase in the high density interior of the star. The equation of state (EOS) of strange quark matter (SQM) was recently improved...
We compare their respective predictions regarding the structure of neutron stars, in particular the mass-radius relation.关键词: Nuclear matter Nuclear matter aspects of neutron stars Many-body theory Neutron stars DOI: 10.1103/PhysRevC.69.018801 被引量: 320 ...
Structure of neutron stars..ppt上传人:夏风如歌 2016/6/1 文件大小:0 KB 下载得到文件列表 Structure of neutron stars..ppt 文档介绍相关标签 检视剖析 信条剖析 成长剖析 廉政剖析 英语自学剖析 自我检视剖析 护士不足剖析 夜宴剧情剖析 禁酒自查剖析 教师不足剖析 ...
Neutron stars play a unique role in physics and astrophysics. On the one hand, they contain matter under extreme physical conditions, and their theories are based on risky and far extrapolations of what we consider reliable physical theories of the structure of matter tested in laboratory. On th...
We study relationships between the neutron-rich skin of a heavy nucleus and the properties of neutron-star crusts. Relativistic effective field theories with a thicker neutron skin in $^{208}$Pb have a larger electron fraction and a lower liquid-to-solid
Structure of Rotating Neutron Stars in Uniform Strong Magnetic Field,Structure of Rotating Neutron Stars in Uniform Strong Magnetic Field,of,in,In,St..
Influence of a scalar-isovector δ-meson field on the quark phase structure in neutron stars The deconfinement phase transition from hadronic matter to quark matter in the interior of compact stars is investigated. The hadronic phase is described i... GB Alaverdyan - 《天文和天体物理学研究》 ...
We will discuss the properties of equilibrium models of magnetized neutron stars, and we will show how internal and external currents can be related. These magnetic field configurations will be discussed considering also their stability, relevant for their origin and possibly connected to events like ...