本文選題：混合星 + 物態(tài)方程　； 參考：《華南理工大學(xué)》2012年碩士論文

【摘要】：物態(tài)方程是理論研究中子星結(jié)構(gòu)和性質(zhì)的重要輸入量。將物態(tài)方程輸入TOV方程，就可以得到中子星的內(nèi)部結(jié)構(gòu)如密度、壓強隨半徑的變化，及質(zhì)量和半徑等宏觀特性。不同的物態(tài)方程，會得出迥然不同的中子星宏觀特征。中子星的質(zhì)量和半徑是其重要的外部特性，對于基本物理理論的驗證有著非常關(guān)鍵的作用。對中子星質(zhì)量的觀測將對中子星的物態(tài)方程提供有效的約束，特別是大質(zhì)量中子星的觀測發(fā)現(xiàn)。最近觀測到的PSRJ1614-2230中子星具有較大的星體質(zhì)量，被精確測定為1.97±0.04M⊙(其中M⊙為太陽質(zhì)量：2×10~(30)kg)對中子星物質(zhì)物態(tài)方程提供了較為嚴(yán)格的約束，即在經(jīng)典理論框架下它將排除所有較軟的物態(tài)方程。在各種理論模型中，超子態(tài)、夸克態(tài)等的出現(xiàn)將會使物態(tài)方程軟化。例如，混合星模型的物態(tài)方程就具有較軟的物態(tài)方程。同時，地面重離子碰撞試驗也支持高密度非對稱核物質(zhì)具有較軟物態(tài)方程的結(jié)論。 那么，大質(zhì)量的中子星的發(fā)現(xiàn)，，是否真的可以排除較軟的物態(tài)方程呢？在對引力的認(rèn)識還并不完善的今天，我們對此并不能給出肯定的答案。早就被試驗證實的小尺度下引力將嚴(yán)重偏離牛頓引力的事實提醒我們：在致密天體中這種非牛頓引力可能會具有明顯的物理效應(yīng)。研究表明，非牛頓引力為軟物態(tài)方程支持大質(zhì)量中子星提供了一種有效的物理機制。本論文主要研究了考慮非牛頓引力下的快速轉(zhuǎn)動混合星（hybrid star）的結(jié)構(gòu)和性質(zhì)：包括質(zhì)量——半徑關(guān)系、Kepler轉(zhuǎn)速、轉(zhuǎn)動慣量、引力紅移以及轉(zhuǎn)動動能和引力結(jié)合能之比等。結(jié)果表明，非牛頓引力和快速轉(zhuǎn)動都會有效地增大混合星能支持的最大質(zhì)量；Kepler轉(zhuǎn)速下能支持的最大質(zhì)量比靜態(tài)時增加約20%左右。轉(zhuǎn)動對于考慮非牛頓引力的混合星整體結(jié)構(gòu)性質(zhì)（包括質(zhì)量——半徑關(guān)系、轉(zhuǎn)動慣量、轉(zhuǎn)動動能和引力結(jié)合能之比等）都具有明顯的影響，但對極向引力紅移影響相對較小。
[Abstract]:The equation of state is an important input for the theoretical study of the structure and properties of neutron stars. When the equation of state is input into the TOV equation, the internal structure of the neutron star, such as the variation of the density, the pressure with the radius, the mass and the radius, and so on, can be obtained. Different equations of state will result in very different macro characteristics of neutron stars. The mass and radius of neutron stars are important external properties and play a very important role in the verification of basic physical theory. The observation of neutron star mass will provide an effective constraint on the equation of state of neutron star, especially the observation of large mass neutron star. The recently observed PSRJ1614-2230 neutron star has a large stellar mass, which has been accurately determined to be 1.97 鹵0.04M _ (?) (where M _ (?) is the solar mass of 2 脳 10 ~ (2) 脳 10 ~ (2) ~ (30) kg), which provides a relatively strict constraint on the equation of state of matter of the neutron star. That is, under the framework of classical theory, it will exclude all the softer equations of state. In various theoretical models, the occurrence of hyperon and quark states will soften the equation of state. For example, the equation of state of the mixed star model has a softer equation of state. At the same time, the ground heavy ion collision test also supports the conclusion that high density asymmetric nuclear matter has a soft equation of state. So can the discovery of a massive neutron star really exclude the softer equation of state? In today's imperfect understanding of gravity, we cannot give a definite answer to it. The fact that gravity will deviate seriously from Newton's gravity on a small scale, which has long been proved by experiments, reminds us that this kind of non-Newtonian gravity may have obvious physical effects in dense celestial bodies. It is shown that non-Newtonian gravitation provides an effective physical mechanism for the support of large mass neutron stars by the equations of state of soft matter. In this paper, the structure and properties of hybrid stars with fast rotation considering non-Newtonian gravity are studied, including the mass-radius relation Kepler rotational speed, moment of inertia, gravitational redshift and the ratio of rotational kinetic energy to gravitational binding energy. The results show that both non-Newtonian gravity and rapid rotation can effectively increase the maximum mass supported by the mixed star at Kepler speed by about 20% compared with the static one. Rotation has obvious influence on the global structure properties of mixed stars considering non-Newtonian gravity (including mass-radius relation, moment of inertia, ratio of rotational kinetic energy to gravitational binding energy, etc.), but has relatively little effect on the red shift of polar gravity.
【學(xué)位授予單位】：華南理工大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2012
【分類號】：P145.6

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本文編號：1940245