中子星的結(jié)構(gòu)與冷卻
發(fā)布時(shí)間：2018-11-21 11:28
【摘要】：由于核物理理論的不確定性,在中子星的能標(biāo)下可以出現(xiàn)各種可能的自由度。對(duì)于不同的物質(zhì)相或者不同的相互作用模型,將其狀態(tài)方程代入廣義相對(duì)論框架下的恒星結(jié)構(gòu)方程,就能求解出不同的質(zhì)量半徑關(guān)系,從而可以利用觀測(cè)對(duì)狀態(tài)方程進(jìn)行限制。另一方面,對(duì)于不同的微觀組成來(lái)說(shuō),其系統(tǒng)內(nèi)部的動(dòng)力學(xué)過(guò)程也不盡相同,這些差異可能會(huì)在宏觀尺度上通過(guò)中子星的熱輻射性質(zhì)體現(xiàn)出來(lái)。因此,我們?nèi)魧⒅凶有抢鋮s理論與熱輻射數(shù)據(jù)進(jìn)行對(duì)比,也可以得知星體內(nèi)部物質(zhì)的信息。 正因?yàn)榇嬖谀挲g老但溫度高的脈沖星,在研究晚期的中子星冷卻時(shí),我們不能不考慮加熱機(jī)制的影響�；瘜W(xué)加熱就是其中一種對(duì)晚期中子星熱演化有較大貢獻(xiàn)的機(jī)制,它起源于星體因?yàn)檗D(zhuǎn)動(dòng)壓縮而導(dǎo)致的系統(tǒng)化學(xué)平衡的偏離。由于弛豫時(shí)標(biāo)比轉(zhuǎn)動(dòng)壓縮的時(shí)標(biāo)要長(zhǎng),系統(tǒng)偏離之后就再也回不到平衡態(tài),這便有了化學(xué)能的儲(chǔ)存與耗散加熱的競(jìng)爭(zhēng)過(guò)程,最終使得中子星的溫度會(huì)回升到一個(gè)準(zhǔn)平衡態(tài)。 在此基礎(chǔ)上,本文討論了含有強(qiáng)子夸克混合相的中子星在轉(zhuǎn)動(dòng)壓縮時(shí)發(fā)生退禁閉相變的情況。對(duì)于這種情況,內(nèi)部的強(qiáng)子物質(zhì)會(huì)轉(zhuǎn)化成更穩(wěn)定的夸克物質(zhì),并間接導(dǎo)致物質(zhì)組分的變化,同樣的,這也會(huì)引起化學(xué)平衡的偏離與耗散加熱�？紤]了星體內(nèi)部的物質(zhì)分布與轉(zhuǎn)動(dòng)結(jié)構(gòu)之后,我們發(fā)現(xiàn),退禁閉相變的出現(xiàn)使得化學(xué)加熱效率有了明顯的提高,且對(duì)于高磁場(chǎng)的中子星來(lái)說(shuō)也是可以有加熱效果的。 考慮到演化過(guò)程中的化學(xué)能不僅是通過(guò)反應(yīng)被耗散成了可以加熱星體的內(nèi)能,還有一部分會(huì)被非平衡Urca反應(yīng)產(chǎn)生的中微子直接輻射掉,本文也對(duì)化學(xué)能的耗散機(jī)制做了討論。通過(guò)計(jì)算發(fā)現(xiàn),新的耗散機(jī)制對(duì)中子星的冷卻曲線影響不大。
[Abstract]:Due to the uncertainty of nuclear physics theory, various possible degrees of freedom can appear under the energy scale of neutron stars. For different material phases or different interaction models, the equation of state can be substituted into the stellar structure equation under the framework of general relativity, and different mass radii can be solved, thus the state equation can be restricted by observation. On the other hand, for different microscopic compositions, the dynamic processes within the system are different, and these differences may be reflected by the thermal radiation properties of neutron stars on a macro scale. Therefore, if we compare the neutron star cooling theory with the thermal radiation data, we can also know the information of the matter inside the star. Because of the existence of pulsars of high temperature, the influence of heating mechanism should be taken into account in the study of the cooling of neutron stars in the late stage. Chemical heating is one of the major contributions to the thermal evolution of late neutron stars, which originates from the deviation of the chemical equilibrium of the system caused by the rotational compression of stars. Because the relaxation time scale is longer than the time scale of rotational squeezing, the equilibrium state can not be returned to the system after the system deviates, which leads to the competitive process of chemical energy storage and dissipative heating, and finally the temperature of the neutron star will rise to a quasi-equilibrium state. On the basis of this, the deblocking phase transition of neutron stars with Hadron quark mixed phase during rotational compression is discussed. In this case, the internal Hadron matter will be converted into more stable quark matter, and indirectly lead to the change of the composition of the matter. Similarly, this will lead to the deviation of the chemical equilibrium and dissipative heating. Considering the distribution of matter and the rotational structure of the stars, we find that the appearance of the deconfined phase transition can obviously improve the chemical heating efficiency, and it can also be used to heat the neutron stars with high magnetic field. Considering that the chemical energy in the evolution process is not only dissipated to the inner energy of the star by reaction, but also a part of the neutrino radiation produced by the nonequilibrium Urca reaction, the dissipative mechanism of the chemical energy is also discussed in this paper. It is found that the new dissipative mechanism has little effect on the cooling curve of neutron stars.
【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】：2012
【分類(lèi)號(hào)】：P145.6
[Abstract]:Due to the uncertainty of nuclear physics theory, various possible degrees of freedom can appear under the energy scale of neutron stars. For different material phases or different interaction models, the equation of state can be substituted into the stellar structure equation under the framework of general relativity, and different mass radii can be solved, thus the state equation can be restricted by observation. On the other hand, for different microscopic compositions, the dynamic processes within the system are different, and these differences may be reflected by the thermal radiation properties of neutron stars on a macro scale. Therefore, if we compare the neutron star cooling theory with the thermal radiation data, we can also know the information of the matter inside the star. Because of the existence of pulsars of high temperature, the influence of heating mechanism should be taken into account in the study of the cooling of neutron stars in the late stage. Chemical heating is one of the major contributions to the thermal evolution of late neutron stars, which originates from the deviation of the chemical equilibrium of the system caused by the rotational compression of stars. Because the relaxation time scale is longer than the time scale of rotational squeezing, the equilibrium state can not be returned to the system after the system deviates, which leads to the competitive process of chemical energy storage and dissipative heating, and finally the temperature of the neutron star will rise to a quasi-equilibrium state. On the basis of this, the deblocking phase transition of neutron stars with Hadron quark mixed phase during rotational compression is discussed. In this case, the internal Hadron matter will be converted into more stable quark matter, and indirectly lead to the change of the composition of the matter. Similarly, this will lead to the deviation of the chemical equilibrium and dissipative heating. Considering the distribution of matter and the rotational structure of the stars, we find that the appearance of the deconfined phase transition can obviously improve the chemical heating efficiency, and it can also be used to heat the neutron stars with high magnetic field. Considering that the chemical energy in the evolution process is not only dissipated to the inner energy of the star by reaction, but also a part of the neutrino radiation produced by the nonequilibrium Urca reaction, the dissipative mechanism of the chemical energy is also discussed in this paper. It is found that the new dissipative mechanism has little effect on the cooling curve of neutron stars.
【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】：2012
【分類(lèi)號(hào)】：P145.6
【相似文獻(xiàn)】
相關(guān)期刊論文 前10條
1 陸W，
本文編號(hào)：2346830
本文鏈接：http://sikaile.net/kejilunwen/tianwen/2346830.html
最近更新
教材專(zhuān)著
