二倍太阳质量中子星的计算研究教学课件

1、二倍太阳质量中子星的计算研究 赵先锋滁州学院机械与电子工程学院9/21/20229/21/20221 Main Content Introduction The RMF theory and the mass of a neutron star Approximate limitation of the hyperon coupling constants Four of the possible models for the neutron star PSR J1614-2230 Summary9/21/20222. Introduction1. The discovery of the t

2、wo-times solar mass neutron star PSR J1614-2230 The neutron star PSR J1614-2230, which mass is 1.97 M and may be the heaviest by now, was observed in 2010. Obviously, it will be meaningful to describe its mass theoretically.9/21/20223 Based on EOS-independent analytic solutions of Einsteins equation

3、s, Demorest et al calculated the mass of the neutron star and found that the calculations, which is in the hadronic level, can not obtain the mass of the neutron star PSR J1614-2230 because of its too smaller mass. But we think that this may be questionable.2. In the hadronic level, the mass of neut

4、ron star 1.97 M can be obtained if the suitable EOS and the coupling constants are chosen9/21/20224 Calculations show that the neutron-star mass is very sensitive to the hyperon coupling constants. One of the parameter selection methods is to choose the coupling constants of meson by the constituent

5、 quark model SU(6) symmetry and to choose the couplings constants of meson by fitting the , and well depth in nuclear matter. Because the energy density of neutron star matter is several times larger than the saturation nucleon density, the prior parameter selection methods to a great extent is extr

6、apolative. In the interior of a neutron star, the hyperons would be produced with the baryon number density increase. So it is reasonable to think that neutron stars containing hyperons.9/21/20226 From the results above it can be seen that, considering nucleons within neutron stars, the mass of neut

7、ron star which is greater than 1.97 M may be obtained if the suitable EOS and the coupling constants are chosen. In this work, we apply the RMF theory to describe the mass of the neutron star PSR J1614-2230 by adjusting the hyperon coupling constants.9/21/20227The energy density and pressure of a ne

8、utron star are given by9/21/20229where, m* is the effective mass of baryonsWe use the O-V equation to obtain the mass and the radius of neutron stars9/21/202210. Approximate limitation of the hyperon coupling constantsIn this work, we choose the GL97 set listed in Table .We define the ratios9/21/2022119/21/2022129/21/2022139/21/2022149/21/202216. Four of the possible models f