【摘要】：首先，我們闡述了中子星結(jié)構(gòu)和性質(zhì)的研究現(xiàn)狀及意義，以及致密星非徑向振動(dòng)f-mode的研究方法。在后面的兩個(gè)主要部分，計(jì)算并討論了中子星和夸克星的f-mode振動(dòng)頻率和衰減時(shí)間。 詳細(xì)地，我們利用普遍用來(lái)計(jì)算致密星結(jié)構(gòu)的廣義相對(duì)論下球?qū)ΨQ理想流體靜力學(xué)平衡方程(TOV方程)，并且飽和核密度附近給定對(duì)稱能斜率一個(gè)合理的范圍，計(jì)算了中子星的質(zhì)量-半徑關(guān)系，以及中子星非徑向振動(dòng)f-mode的振動(dòng)頻率和衰減時(shí)間，同時(shí)獲得了頻率和衰減時(shí)間的約束范圍。結(jié)果表明：較大的對(duì)稱能斜率對(duì)應(yīng)著較小的振動(dòng)頻率和較長(zhǎng)的衰減時(shí)間；與牛頓理論做對(duì)比，廣義相對(duì)論下計(jì)算出的f-mode振動(dòng)頻率跟平均密度的平方根存在類似的比例關(guān)系；并且以致密度(M R)作為自變量，以含有衰減時(shí)間的函數(shù)作為因變量進(jìn)行合理的擬合。 另一方面，非牛頓引力的提出是為了使地面實(shí)驗(yàn)給出的軟物態(tài)可以支持觀測(cè)到的大質(zhì)量脈沖星，它提供一種排斥力，在物理上類似于暗能量的作用。本文在夸克星內(nèi)考慮了非牛頓引力，，夸克星物質(zhì)的狀態(tài)方程用MIT口袋模型來(lái)描述，同樣計(jì)算了夸克星的質(zhì)量-半徑關(guān)系和f-mode的振動(dòng)頻率和衰減時(shí)間。研究發(fā)現(xiàn)：對(duì)較大的口袋參數(shù)B，即B=117MeVfm-3時(shí)，計(jì)算出的夸克星最大質(zhì)量為觀測(cè)到的典型脈沖星的質(zhì)量，非牛頓引力應(yīng)該被考慮。而且我們的計(jì)算結(jié)果顯示，與傳統(tǒng)的中子星相比，星體質(zhì)量相同時(shí)夸克星擁有相對(duì)較高的f-mode振動(dòng)頻率。
[Abstract]:Firstly, we describe the present situation and significance of the study on the structure and properties of neutron stars, as well as the research methods of nonradial vibration f-mode for dense stars. The f-mode vibration frequency and attenuation time of neutron star and quark star are calculated and discussed in the following two main parts. In detail, we use the spherical symmetric ideal hydrostatic equilibrium equation (TOV equation), which is generally used to calculate compact star structures, and give a reasonable range of symmetric energy slope near the density of saturated nuclei. The mass-radius relation of the neutron star, the vibration frequency and attenuation time of the non-radial vibration f-mode of the neutron star are calculated, and the constraint range of the frequency and attenuation time is obtained. The results show that the larger symmetric energy slope corresponds to smaller vibration frequency and longer attenuation time, and compared with Newton's theory, the f-mode vibration frequency calculated under general relativity has a similar proportional relationship with the square root of average density. The density (M R) is regarded as the independent variable and the function with attenuation time as the dependent variable. On the other hand, the non-Newtonian gravity is proposed to support the observed large mass pulsars in the soft state given by the ground experiments, which provides a repulsive force that is physically similar to the action of dark energy. In this paper, non-Newtonian gravity is considered in quark stars. The equation of state of quark stars is described by MIT pocket model. The mass-radius relation of quark stars and the vibration frequency and attenuation time of f-mode are also calculated. It is found that the calculated maximum mass of the quark star is the mass of the observed typical pulsar for the larger pocket parameter B, that is, B=117MeVfm-3, and the non-Newtonian gravity should be taken into account. Furthermore, our results show that quark stars have relatively high f-mode vibration frequency when the mass of the stars is the same as that of the conventional neutron stars.
【學(xué)位授予單位】：華南理工大學(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3條

1 燕晶;文得華;;R-mode Instability of Neutron Star with Non-Newtonian Gravity[J];Communications in Theoretical Physics;2013年01期

2 文德華;周穎;;Effects of the symmetry energy slope on the axial oscillations of neutron stars[J];Chinese Physics B;2013年08期

3 文德華;付宏洋;陳偉;;Impact of neutron star crust on gravitational waves from the axial w-modes[J];Chinese Physics B;2011年06期

本文編號(hào)：2278419