【摘要】：中子星作為致密物質(zhì)的天然實(shí)驗(yàn)室，一直是很多學(xué)者研究的熱門(mén)課題。本文一方面采用相對(duì)論平均場(chǎng)理論來(lái)研究Δ共振態(tài)在不同中子星物質(zhì)（傳統(tǒng)中子星物質(zhì)、超子物質(zhì)、K介子凝聚等）中的性質(zhì)，研究Δ共振態(tài)對(duì)中子星粒子分布、質(zhì)量-半徑關(guān)系等方面性質(zhì)的影響，進(jìn)而證明Δ共振態(tài)可以存在于中子星的內(nèi)部。另一方面，以弱相互作用理論為基礎(chǔ)，研究Δ共振態(tài)對(duì)核子的直接URCA過(guò)程及中子星冷卻過(guò)程的影響。最后，以脈沖星J1614-2230為例，研究Δ共振態(tài)對(duì)它的影響。結(jié)果表明，脈沖星J1614-2230的內(nèi)核可以由傳統(tǒng)中子星物質(zhì)和Δ共振態(tài)構(gòu)成，并且Δ~（-）和Δ~（0）粒子所占的比例可高達(dá)百分之三十。Δ共振態(tài)對(duì)冷卻的影響較為復(fù)雜，它們能夠降低中微子的發(fā)射率和發(fā)光度，但是在傳統(tǒng)中子星物質(zhì)中，Δ共振態(tài)加速中子星冷卻。 本文的主要內(nèi)容如下： 第一章回顧中子星研究的發(fā)展歷史，介紹中子星的性質(zhì)，以及目前國(guó)內(nèi)外對(duì)中子星的研究現(xiàn)狀，并提出對(duì)未來(lái)的展望。 第二章介紹基本的研究理論，，分析Δ共振態(tài)存在于傳統(tǒng)中子星物質(zhì)及超子物質(zhì)中的可能性，研究在這兩種物質(zhì)中Δ共振態(tài)對(duì)中子星微觀及宏觀性質(zhì)的影響。 第三章給出Δ共振態(tài)可以出現(xiàn)在含反K介子凝聚中子星內(nèi)部的依據(jù)。分析Δ共振態(tài)與反K介子互相影響的性質(zhì)，并研究它們對(duì)中子星的影響。 第四章介紹中子星的冷卻理論，并且討論Δ共振態(tài)對(duì)核子的直接URCA過(guò)程、中微子發(fā)射率、中微子發(fā)光度、冷卻曲線等方面的影響。 第五章研究Δ共振態(tài)存在于具體的中子星內(nèi)部的情況（比如脈沖星J1614-2230），給出他們存在的徑向范圍、粒子數(shù)所占比例、冷卻等性質(zhì)。
[Abstract]:As a natural laboratory of dense matter, neutron star has been a hot topic for many scholars. On the one hand, the relativistic mean field theory is used to study the properties of 螖 resonance state in different neutron star matter (traditional neutron star matter, hyperon matter K meson condensation, etc.) and the distribution of 螖 resonance state to neutron star particle. It is proved that the 螖 resonance state can exist inside the neutron star due to the influence of the mass-radius relation. On the other hand, based on the weak interaction theory, the influence of 螖 resonance state on the direct URCA process of nucleon and the cooling process of neutron star is studied. Finally, the effect of 螖 resonance on the pulsar J1614-2230 is studied. The results show that the core of pulsar J1614-2230 can be composed of conventional neutron star matter and 螖 resonance state, and the proportion of 螖 ~ (-) and 螖 ~ (0) particles can be as high as 30%. The effect of 螖 resonance state on cooling is more complex. They can reduce the emissivity and luminosity of neutrino, but in conventional neutron star matter, 螖 resonance state accelerates the cooling of neutron star. The main contents of this paper are as follows: the first chapter reviews the development history of neutron star research, introduces the nature of neutron star, and the present research status of neutron star at home and abroad, and puts forward the prospect for the future. The second chapter introduces the basic research theory, analyzes the possibility of 螖 resonance state in the traditional neutron star matter and hyperon matter, and studies the influence of 螖 resonance state on the microscopic and macroscopic properties of neutron star in these two kinds of matter. In chapter 3, we give the basis for 螖 resonance state to appear in the neutron star with inverse K meson condensation. The properties of the interaction between 螖 resonance states and inverse K mesons are analyzed and their effects on neutron stars are studied. In chapter 4, the cooling theory of neutron star is introduced, and the effects of 螖 resonance state on the direct URCA process, neutrino emissivity, neutrino luminosity and cooling curve are discussed. In chapter 5, we study the existence of 螖 resonance in the interior of a specific neutron star (for example, pulsar J1614-2230), and give their radial range, the proportion of particles, cooling and so on.
【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】：2012
【分類(lèi)號(hào)】：P145.6

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相關(guān)期刊論文 前2條

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本文編號(hào)：2239040