密度相关和非线性相对论平均场理论对中子星的描述.ppt

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9/21/2018,2018/9/21,2,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 Summary,2018/9/21,3,. Introduction,1. The discovery o

2、f the two-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.,2018/9/21,4,Based on EOS-independent analytic solutions of Einsteins

3、 equations, 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 ma

4、ss of neutron star 1.97 M can be obtained if the suitable EOS and the coupling constants are chosen,2018/9/21,5,1985, considering the octet, the mass of neutron star calculated by Glendenning is in the range of 1.51.8 M in the framework of relativistic mean field (RMF) theory. But if only nucleons b

5、eing included in the neutron star, the mass of neutron star he obtained would be 2.36 M. It is obvious that considering the hyperons within neutron star would reduce the mass.,2018/9/21,6,Calculations show that the neutron-star mass is very sensitive to the hyperon coupling constants. One of the par

6、ameter selection methods is to choose the coupling constants of meson by the constituent 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 sat

7、uration nucleon density, the prior parameter selection methods to a great extent is extrapolative.,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.,2018/9/21,7,From the resu

8、lts above it can be seen that, considering nucleons within neutron stars, the mass of neutron 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

9、adjusting the hyperon coupling constants.,2018/9/21,8,The Lagrangian density of hadron matter reads as follows,.The RMF theory and the mass of a neutron star,2018/9/21,9,The energy density and pressure of a neutron star are given by,2018/9/21,10,where, m* is the effective mass of baryons,We use the

10、O-V equation to obtain the mass and the radius of neutron stars,2018/9/21,11,. Approximate limitation of the hyperon coupling constants,In this work, we choose the GL97 set listed in Table .,We define the ratios,2018/9/21,12,2018/9/21,13,2018/9/21,14,2018/9/21,15,2018/9/21,16,2018/9/21,17,. Four of the possible models for the neutron star PSR J1614-2230,2018/9/21,18,2018/9/21,19,2018/9/21,20,2018/9/21,21,. Summary,2018/9/21,22,2018/9/21,23,Thank you very much!,