二倍太阳质量中子星的计算研究教学课件.ppt
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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 4/7/2019,2019/4/7,2,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,2019/4/7,3,. Introduction,1. The discovery of
2、 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.,2019/4/7,4,Based on EOS-independent analytic solutions of Einsteins e
3、quations, 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
4、 of neutron star 1.97 M can be obtained if the suitable EOS and the coupling constants are chosen,2019/4/7,5,1985, 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 bein
5、g 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.,2019/4/7,6,Calculations show that the neutron-star mass is very sensitive to the hyperon coupling constants. One of the paramet
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