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...
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 ...
In many astrophysical scenarios, such as core-collapse supernovae and neutron star mergers, as in well as heavy-ion collision experiments, transitions between thermally populated nuclear excited states have been shown to play an important role. Because of its simplicity and ability to extrapolate, ...
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 and effective temperature are increased as well as its crystalline lattice is disordered with grinding time increasing. 研究表明 :随着粉磨...
that makes a bright explosion (supernova) at this point, the heavier elements are finally created if the leftover core is very, very dense, it may form a very small neutron star or a black hole with VERY powerful gravity Cosmology How did the cosmos begin, and what will happen to it?
Neutron Stars. I. Properties at Absolute Zero Temperature The properties of a neutron star at absolute zero temperature are discussed. The problem of determining the ground state of a neutron star is formulated in... JN Bahcall,RA Wolf - 《Physical Review》 被引量: 72发表: 1965年 Decoherence...
Which star is at higher temperature? (a) A red star (b) A blue star? Temperature: The presence of the intensity of the heat in any object is termed as the temperature. The help of the thermometer can estimate the temperature of any object. The temperature can give an idea...
The presence of a mixed-phase region softens the EOS and open the possibility of a direct explosion. At larger densities the EOS is stiff enough to support a neutron star compatible with observations.doi:10.1088/0954-3899/25/5/302A. Drago...
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 atfinite 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 atfinite temperature; ...
4) finite-temperature neutron star 有限温度中子星 5) effective quantum field theory 有效量子场论 6) finite temperature 有限温度 1. A two-dimensional dark energy star model atfinite 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 ci...