We start with a brief introduction to the historical background in the early pioneering days when the first neutron star thermal evolution calculations predicted the presence of neutron stars hot enough to be observable. We then report on the first detection of neutron star temperatures by ROSAT X...
Neutron star, any of a class of extremely dense, compact stars thought to be composed primarily of neutrons. Neutron stars are typically about 20 km (12 miles) in diameter. Their masses range between 1.18 and 1.97 times that of the Sun, but most are 1.35
We study the non--linear evolution of magnetic fields in neutron star crusts with special attention to the influence of the Hall drift. Our goal is to unde... JA Pons,U Geppert - 《Astronomy & Astrophysics》 被引量: 38发表: 2015年 Influence of strong magnetic field on β decay in the...
We then consider a model for the spectrum of the X-ray emission from the disk, parameterized by the mass accretion rate, the color temperature and the rotation rate of the neutron star. We derive constraints on these parameters for the X-ray source Cygnus X-2 using the estimates of the ...
1) finite-temperature neutron star 有限温度中子星2) finite temperature 有限温度 1. A two-dimensional dark energy star model at finite temperature; 有限温度下的二维暗能量星模型 2. The energy and thermal effects of mesoscopic capacitance coupling LC circuit at finite temperature; 介观电容耦合LC...
We have computed the field at several temperatures and get a right order of magnitude. We also conclude that a cooler neutron star has a stronger magnetic field. We work in the framework of the nonlin-Wang Qingwu不详Lue XiaofuZuo WeiLi Xiguo中国科学院近代物理研究所和兰州重离子研究装置年报:...
2) finite-temperature neutron star 有限温度中子星 3) effective temperature 有效温度 1. The result shows that its crystallite size is decreased,micro\|strain andeffective temperatureare increased as well as its crystalline lattice is disordered with grinding time increasing. ...
(T=20 MeV).It's found that the different effective interactions give us different descriptions of neutron star.The results of DDME1 and TW99 have little odds,they both give the stronger meson field potential,the smaller hyperon transition density,the harder equation of state and the bigger ...
The surface of a neutron star is around 600,000 degrees C (around 1 million degrees Fahrenheit).What is the Sun? The Sun is the center of the solar system. At the center of the solar system is a star—the Sun. While it shares many characteristics with other stars in the galaxy, it...
and environments with extraordinarily highneutron fluxes. The short-lived high density andtemperature plasmaconditions resemble conditions in the interior of stars. This opens up the opportunity to study these effects for the first time and test the theoretical predictions that affect all reactions associ...