本文選題：中子星 + 質(zhì)量半徑關(guān)系　； 參考：《華中師范大學(xué)》2013年碩士論文

【摘要】：極值條件下的核物質(zhì)理論是在高能核物理的重要課題之一。它在了解重離子碰撞以及致密星的演化起著至關(guān)重要的作用。 結(jié)合致密星內(nèi)部物質(zhì)的狀態(tài)方程(EOS)和流體靜力平衡條件下的TOV方程,就可以得到致密星的質(zhì)量半徑關(guān)系。中子星有非常豐富的結(jié)構(gòu)。中子星的內(nèi)部物質(zhì)可能是高密度的核物質(zhì)、夸克物質(zhì)、奇異夸克物質(zhì)、混合的核夸克物質(zhì),甚至還有可能是色超導(dǎo)。因?yàn)橹凶有鞘怯钪嬷袃H次于黑洞的致密物體,在足夠高的密度下,夸克可以從強(qiáng)子物質(zhì)中解禁閉出來。因?yàn)閹觳环�(wěn)定性,在高密度下夸克甚至可以像電子一樣形成配對(duì),由于兩個(gè)夸克之間的吸引而形成色超導(dǎo)。 不同組成和結(jié)構(gòu)的中子星其EOS都不同。在不同模型和不同EOS的前提下,我們討論了中子星的質(zhì)量半徑關(guān)系,同時(shí)也考慮了旋轉(zhuǎn)。本文首先討論了裸夸克星,并求解了單味色超導(dǎo)狀態(tài)方程(CSL、polar、planar和A),同時(shí)也使用了CFL和2SC的狀態(tài)方程。首先我們固定能隙△,得到不同色超導(dǎo)相下星體旋轉(zhuǎn)頻率對(duì)質(zhì)量半徑關(guān)系的影響。其次,考慮能隙△對(duì)化學(xué)勢的依賴,對(duì)質(zhì)量半徑關(guān)系重新做了對(duì)比。我們發(fā)現(xiàn)狀態(tài)方程對(duì)質(zhì)量半徑關(guān)系有一定影響,同時(shí)隨著旋轉(zhuǎn)頻率增大,星體的質(zhì)量也會(huì)變大。 論文的第二個(gè)工作就是考慮混合星的質(zhì)量半徑關(guān)系。首先采用了BPAL模型來描述強(qiáng)子物質(zhì),并求解強(qiáng)子物質(zhì)的狀態(tài)方程。同時(shí)我們假定強(qiáng)子-夸克相變?yōu)橐粋�(gè)等壓相變過程。因此,可以通過強(qiáng)子-夸克物質(zhì)的化學(xué)勢-壓強(qiáng)圖(U-P圖)來尋找相變點(diǎn)。當(dāng)強(qiáng)子物質(zhì)與三種不同色超導(dǎo)的相變點(diǎn)確定后,再依據(jù)TOV方程和TOV方程旋轉(zhuǎn)微擾修正,我們就可以得到混合星的質(zhì)量半徑關(guān)系圖。 論文最后對(duì)全文所做的研究工作進(jìn)行了一個(gè)小結(jié),同時(shí)也對(duì)以后的工作方向做了大致的描述。
[Abstract]:Nuclear matter theory under extreme condition is one of the important subjects in high energy nuclear physics.It plays a vital role in understanding heavy ion collisions and the evolution of dense stars.The relation of mass radius of dense star can be obtained by combining the equation of state of matter in dense star and the TOV equation under hydrostatic equilibrium condition.Neutron stars have very rich structures.The inner matter of the neutron star may be high density nuclear matter, quark matter, strange quark matter, mixed nuclear quark matter, or even color superconducting.Because neutron stars are the only dense objects in the universe after black holes, quarks can be released from Hadron matter at a sufficiently high density.Because of the Cooper instability, quarks can even be paired like electrons at high density, and color superconductors are formed by the attraction between two quarks.The EOS of neutron stars with different composition and structure is different.On the premise of different models and different EOS, we discuss the relation of mass radius of neutron star and the rotation.In this paper, we first discuss the bare quark stars, and solve the equations of state of the single color superconducting superconducting, CFL and 2SC.First, we fixed the energy gap and obtained the influence of star rotation frequency on the mass radius under different color superconducting phases.Secondly, considering the dependence of energy gap on chemical potential, the relation of mass radius is recompared.It is found that the equation of state has a certain influence on the relation of mass radius, and the mass of stars increases with the increase of rotation frequency.The second work of this paper is to consider the mass radius relation of mixed stars.First, the BPAL model is used to describe the Hadron matter, and the equation of state of the Hadron matter is solved.We also assume that the Hadron-quark phase transition is an isobaric phase transition process.Therefore, the phase transition point can be found by the chemical potential-pressure diagram of Hadron quark matter (U-P diagram).When the phase transition points of Hadron matter and three different color superconductors are determined, and then the perturbation correction is made according to the TOV equation and TOV equation, the mass radius relation diagram of the mixed star can be obtained.At the end of the paper, a summary of the research work is given, and the future work direction is described.
【學(xué)位授予單位】：華中師范大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2013
【分類號(hào)】：P145.6

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 吳雪君，，須重明;慢旋轉(zhuǎn)星體結(jié)構(gòu)的微擾方法[J];天文學(xué)報(bào);1996年03期

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