本文選題：中子星 + 核物質(zhì)參數(shù)組��； 參考：《渤海大學(xué)》2014年碩士論文

【摘要】：近幾十年來，中子星一直是天體物理、粒子物理，以及核物理領(lǐng)域?qū)W者們研究的熱門課題。目前，觀測到的脈沖星已經(jīng)達(dá)到兩千多顆，這為中子星的理論研究提供了豐富的觀測數(shù)據(jù)。當(dāng)前對中子星的研究工作可分為四個(gè)方面，分別是中子星冷卻性質(zhì)的研究、中子星內(nèi)部結(jié)構(gòu)的研究、中子星磁場方面的研究以及動(dòng)力學(xué)方面的研究。對于中子星的研究，很多物理學(xué)家已經(jīng)做了大量工作，并且也有了很大進(jìn)展。但是，目前對于中子星的物質(zhì)組成、冷卻性質(zhì)等仍無定論，中子星的眾多謎團(tuán)尚未解開。 本文采用的理論是相對論平均場理論和相關(guān)的弱作用理論，通過GM1、GPS250以及NL-SH參數(shù)組來研究中子星的物質(zhì)組成、結(jié)構(gòu)以及中微子發(fā)射率、發(fā)光度等性質(zhì)。本文共分為五個(gè)部分。第一部分介紹中子星的研究歷史，國內(nèi)外目前的研究現(xiàn)狀以及星體的結(jié)構(gòu)性質(zhì)和研究意義。第二部分給出相對論平均場理論以及常用的參數(shù)組。第三部分分別采用GM1、GPS250和NL-SH三組參數(shù)，，計(jì)算中子星物質(zhì)的介子勢、狀態(tài)方程（EOS）以及中子星的質(zhì)量-半徑關(guān)系等。第四部分給出中子星的冷卻理論，在不同的參數(shù)下計(jì)算中微子發(fā)射率、星體發(fā)光度及冷卻曲線等，并且把不同質(zhì)量、不同參數(shù)下算得的中子星的冷卻性質(zhì)進(jìn)行對比研究。第五部分給出結(jié)論�；\統(tǒng)地說，GPS250參數(shù)下算得的中子星冷卻速度較快，并且星體質(zhì)量對冷卻速度的影響相對明顯。
[Abstract]:In recent decades, neutron stars have been a hot topic in astrophysics, particle physics and nuclear physics. At present, more than 2,000 pulsars have been observed, which provides abundant observation data for the theoretical study of neutron stars. The current research work on neutron star can be divided into four aspects, namely, the study of the cooling property of the neutron star, the study of the inner structure of the neutron star, the study of the magnetic field of the neutron star and the study of the dynamics of the neutron star. Many physicists have done a lot of work and made great progress on neutron stars. However, the composition and cooling properties of neutron stars are still unknown, and many mysteries of neutron stars have not been solved. The theory used in this paper is the relativistic mean field theory and the related weak action theory. The composition, structure, neutrino emissivity and luminosity of neutron star are studied by GM1GPS250 and NL-SH parameter set. This paper is divided into five parts. The first part introduces the history of neutron stars, the current research situation at home and abroad, the structure, properties and significance of stars. In the second part, the relativistic mean field theory and the commonly used parameter sets are given. In the third part, the meson potential, the equation of state (EOS) and the mass-radius relation of neutron star are calculated by using GM1GPS250 and NL-SH respectively. In the fourth part, the cooling theory of neutron star is given. The neutrino emissivity, star luminosity and cooling curve are calculated under different parameters, and the cooling properties of neutron star with different mass and different parameters are compared and studied. The fifth part gives the conclusion. In general, the cooling rate of neutron stars calculated under the parameters of GPS250 is relatively fast, and the effect of star mass on cooling rate is relatively obvious.
【學(xué)位授予單位】：渤海大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2014
【分類號(hào)】：P145.6

【參考文獻(xiàn)】

相關(guān)期刊論文 前4條

1 賈煥玉,呂洪鳳,孟杰;_Λ~(208)Pb的超子分布半徑和中子星結(jié)構(gòu)[J];高能物理與核物理;2002年10期

2 包特木爾巴根;唐高娃;;中子星研究歷史回顧、現(xiàn)狀及展望[J];南陽師范學(xué)院學(xué)報(bào);2009年03期

3 丁文波;喻孜;密更;王春艷;;Neutron star cooling in various sets of nucleon coupling constants[J];Chinese Physics C;2013年05期

4 徐峰;岳友嶺;徐仁新;;脈沖星、中子星與夸克星[J];自然雜志;2007年04期

本文編號(hào)：1892105