超致密暗物質(zhì)暈的相關(guān)研究
發(fā)布時間：2018-11-28 14:48
【摘要】：直到上個世紀Einstein創(chuàng)造廣義相對論,我們才第一次真正有了可以用來描述宇宙演化的理論。為了研究的方便Einstein提出了宇宙學(xué)原理：物質(zhì)的分布在足夠大的尺度上是均勻各向同性的。同時為得到一個靜止的宇宙解,Einstein引進宇宙學(xué)常數(shù),然而這樣的靜態(tài)宇宙仍然是不穩(wěn)定的。隨后Hubble觀測到鄰近24個星系的整體紅移,而且紅移和距離成正比,這既是宇宙膨脹的直接證據(jù),也暗示了宇宙的均勻各向同性。20年后伽莫夫提出宇宙起源于大爆炸,還計算了遺留的光子背景溫度；接著貝爾實驗室的工程師彭齊亞斯和威爾斯發(fā)現(xiàn)了理論學(xué)家正在尋找的宇宙微波背景輻射,從而證實了伽莫夫的預(yù)言。另外大爆炸宇宙學(xué)還很好的解釋了宇宙中輕元素的豐度。20世紀70年代,星系旋轉(zhuǎn)曲線、星系速度彌散和引力透鏡等大量觀測表明絕大部分物質(zhì)是暗物質(zhì),沒有顯著的電磁相互作用。1998年Ia超新星的觀測數(shù)據(jù)表明宇宙正在加速膨脹,如果廣義相對論在宇宙尺度上是正確的,那么就有一種負壓強的暗能量存在。由現(xiàn)代宇宙學(xué)的各種觀測己經(jīng)很精確的知道,通常的可見物質(zhì)(主要是重子)只占據(jù)宇宙的4.9%,暗物質(zhì)占據(jù)26.8%,剩下的68.3%是暗能量。本文主要研究一種最近新發(fā)現(xiàn)的暗物質(zhì)結(jié)構(gòu)：超致密暗物質(zhì)暈(UCMHs)o第一章概述了宇宙學(xué)的知識。我們首先簡要回顧了宇宙學(xué)的發(fā)展史,然后介紹了廣義相對論的重要概念,最后得到宇宙學(xué)的演化方程。對于輻射,物質(zhì)和暗能量,我們得到能量密度ρ和宇宙尺度因子a的關(guān)系,以及宇宙尺度因子隨時間演化的方程。第二章系統(tǒng)地描述了暗物質(zhì)的觀測證據(jù),對暗物質(zhì)候選者進行分類并討論了探測暗物質(zhì)的方法。大質(zhì)量弱相互作用粒子(WIMPs)是理想的冷暗物質(zhì)的候選者,而研究最多的WIMPs是最輕的超對稱粒子。我們給出它們在宇宙中的比例Ωx和參數(shù)的關(guān)系式,由現(xiàn)代觀測我們得到暗物質(zhì)參數(shù)如質(zhì)量和截面的限制。熱暗物質(zhì)典型的例子是三代中微子,我們對中微子的質(zhì)量進行了限制。另外我們也討論了暗物質(zhì)的非熱產(chǎn)生機制,同時給出Ωx依賴于參數(shù)的表達式。特別地,我們討論了最簡單的非熱產(chǎn)生例子-大質(zhì)量弱相互作用標量場的凝聚。軸子最初是粒子物理為解決強CP問題而提出的,它是非熱產(chǎn)生的一個好的候選者。探測暗物質(zhì)的方法有測量原子核的核反沖的直接探測,也有測量暗物質(zhì)粒子湮滅或衰變產(chǎn)生的標準模型粒子的間接探測,當(dāng)然大型對撞機也試圖尋找暗物質(zhì)存在的跡象。第三章探討了一種新的暗物質(zhì)結(jié)構(gòu)-超致密暗物質(zhì)暈(UCMHs),它是Ricotti Gould在2009年提出的。當(dāng)存在原初密度擾動δρ0.3的區(qū)域時,就有可能形成原初黑洞。但是當(dāng)密度擾動小于這一臨界值但大于10-3時,雖無法形成原初黑洞,卻會演化成為超緊致暗物質(zhì)暈。和一般的暗物質(zhì)暈相比,UCMHs的密度更大,形成的時間更早。如果暗物質(zhì)是由WIMP粒子構(gòu)成的,那么UCMH通過WIMP湮滅或者衰變產(chǎn)生的粒子如γ射線有可能被Fermi衛(wèi)星或者大氣切連科夫探測器(ACTs)觀測到,產(chǎn)生的中微子信號被IceCube/DeepCore或其它中微子探測器觀測到。對于給定的模型我們計算了來自UCMH的WIMP湮滅產(chǎn)生的γ射線的通量,同時我們也給出了能被探測到的UCMH豐度的下限,以及沒有被探測到的UCMH豐度的上限,并把UCMH豐度的限制轉(zhuǎn)化為小尺度上原初曲率擾動的限制。如果暗物質(zhì)粒子不湮滅的話,衰變將變得很重要。于是我們同時也計算了UCMH中WIMP衰變產(chǎn)生的γ射線信號,得出了相應(yīng)的UCMH豐度和原初曲率擾動的限制。除了γ射線信號,我們也研究了來自UCMH的中微子信號。雖然沒有探測到中微子,我們給出UCMH豐度的限制,并轉(zhuǎn)化為對小尺度上原初曲率擾動的限制。第四章我們總結(jié)了本文的工作,并展望了未來的研究。
[Abstract]:Until the last century, Einstein created the general theory of relativity, the first time we really had a theory that could be used to describe the evolution of the universe. For the sake of the study, Einstein proposed the principle of cosmology: the distribution of matter is homogeneous and isotropic on a sufficiently large scale. At the same time, Einstein introduced the cosmological constant to get a static universe solution, but such a static universe is still unstable. The whole red shift of the adjacent 24 galaxies is then observed by Hubble, and the red shift is proportional to the distance, which is not only the direct evidence of the expansion of the universe, but also the uniform isotropy of the universe. Then the engineers of the Bell Labs, Penzias and Wells, have discovered the cosmic microwave background radiation that the theory scientists are looking for, confirming the predictions of the Galov. In addition, big bang cosmology has well explained the abundance of light elements in the universe. A large number of observations such as the galaxy rotation curve, the galaxy velocity dispersion, and the gravitational lens in the 1970s indicate that the vast majority of the materials are dark matter, There is no significant electromagnetic interaction. The observation data of the Ia supernova in 1998 indicate that the universe is accelerating the expansion, and if the general relativity is correct in the cosmic scale, there is a dark energy of negative pressure. The various observations of modern cosmology have been well known, and usually the visible substance (mainly the weight) occupies only 40.9% of the universe, the dark matter occupies 26. 8%, and the remaining 68.3% is dark energy. This paper mainly studies a newly discovered dark matter structure: the first chapter of the ultra-dense dark matter halo (UCMHs) o provides an overview of the knowledge of cosmology. We first briefly review the history of cosmology, then introduce the important concept of general relativity, and finally get the evolution equation of cosmology. For radiation, matter and dark energy, we get the relationship between the energy density factor and the cosmic scale factor a, and the equation of the time evolution of the cosmic scale factor. The second chapter systematically describes the observational evidence of dark matter, classifies the dark matter candidates and discusses the method of detecting dark matter. The large mass of weakly interacting particles (WIMPs) is a candidate for the ideal cold dark matter, and the maximum number of WIMPs is the lightest supersymmetric particle. We give the relation of their proportional omega x and the parameters in the universe, and we get dark matter parameters, such as quality and cross-section, from the modern observation. The typical example of a hot dark matter is the third generation of neutrinos, and we have limited the mass of the neutrino. In addition, we also discuss the non-heat generation mechanism of dark matter, and give the expression of 惟 x depending on the parameter. In particular, we have discussed the simplest non-heat generation examples-the coacervation of a large-mass, weak-interaction scalar field. The axis is originally proposed by the particle physics to solve the problem of strong CP, and it is a good candidate for non-heat generation. The method for detecting dark matter has the direct detection of the nuclear recoil of the nuclei, and the indirect detection of the standard model particles produced by the annihilation or decay of the dark matter particles, of course the large collider also tries to find the evidence of the presence of the dark matter. The third chapter discusses a new dark matter structure, ultra-dense dark matter halo (UCMHs), which is proposed by Ricotti Gould in 2009. It is possible to form the original black hole when the initial density disturbance is in the region of 0.3. However, when the density disturbance is less than this critical value but greater than 10-3, the original black hole can not be formed, but it will evolve into a supertight dark matter halo. Compared with the general dark matter halo, the density of the UCMHs is larger and the formed time is earlier. If the dark matter is composed of WIMP particles, the UCMH can be observed by the Fermi satellite or the atmospheric Cerenkov detector (ACTs) by the particles such as X-rays generated by the annihilation or decay of the WIMP, and the generated neutrino signal is observed by the IceCube/ DeepCore or other neutrino detector. for a given model we calculate the flux of the x-rays generated by the wIMP annihilation from the UCMH, while we also give the lower limit of the UCMH abundance that can be detected, and the upper limit of the UCMH abundance that has not been detected, and the limitation of the UCMH abundance is converted into the limit of the initial curvature disturbance on the small scale. Decay will become important if the dark matter particles are not annihilated. So we also calculated the X-ray signal produced by the decay of WIMP in UCMH, and the limitation of UCMH abundance and initial curvature disturbance was obtained. In addition to the X-ray signal, we have also studied the neutrino signal from UCMH. Although the neutrino is not detected, we present the limitation of the UCMH abundance and transform into the limit of the initial curvature disturbance on the small scale. In the fourth chapter, we sum up the work of this paper and look forward to the future research.
【學(xué)位授予單位】：南京大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2014
【分類號】：P145.9
本文編號：2363182
[Abstract]:Until the last century, Einstein created the general theory of relativity, the first time we really had a theory that could be used to describe the evolution of the universe. For the sake of the study, Einstein proposed the principle of cosmology: the distribution of matter is homogeneous and isotropic on a sufficiently large scale. At the same time, Einstein introduced the cosmological constant to get a static universe solution, but such a static universe is still unstable. The whole red shift of the adjacent 24 galaxies is then observed by Hubble, and the red shift is proportional to the distance, which is not only the direct evidence of the expansion of the universe, but also the uniform isotropy of the universe. Then the engineers of the Bell Labs, Penzias and Wells, have discovered the cosmic microwave background radiation that the theory scientists are looking for, confirming the predictions of the Galov. In addition, big bang cosmology has well explained the abundance of light elements in the universe. A large number of observations such as the galaxy rotation curve, the galaxy velocity dispersion, and the gravitational lens in the 1970s indicate that the vast majority of the materials are dark matter, There is no significant electromagnetic interaction. The observation data of the Ia supernova in 1998 indicate that the universe is accelerating the expansion, and if the general relativity is correct in the cosmic scale, there is a dark energy of negative pressure. The various observations of modern cosmology have been well known, and usually the visible substance (mainly the weight) occupies only 40.9% of the universe, the dark matter occupies 26. 8%, and the remaining 68.3% is dark energy. This paper mainly studies a newly discovered dark matter structure: the first chapter of the ultra-dense dark matter halo (UCMHs) o provides an overview of the knowledge of cosmology. We first briefly review the history of cosmology, then introduce the important concept of general relativity, and finally get the evolution equation of cosmology. For radiation, matter and dark energy, we get the relationship between the energy density factor and the cosmic scale factor a, and the equation of the time evolution of the cosmic scale factor. The second chapter systematically describes the observational evidence of dark matter, classifies the dark matter candidates and discusses the method of detecting dark matter. The large mass of weakly interacting particles (WIMPs) is a candidate for the ideal cold dark matter, and the maximum number of WIMPs is the lightest supersymmetric particle. We give the relation of their proportional omega x and the parameters in the universe, and we get dark matter parameters, such as quality and cross-section, from the modern observation. The typical example of a hot dark matter is the third generation of neutrinos, and we have limited the mass of the neutrino. In addition, we also discuss the non-heat generation mechanism of dark matter, and give the expression of 惟 x depending on the parameter. In particular, we have discussed the simplest non-heat generation examples-the coacervation of a large-mass, weak-interaction scalar field. The axis is originally proposed by the particle physics to solve the problem of strong CP, and it is a good candidate for non-heat generation. The method for detecting dark matter has the direct detection of the nuclear recoil of the nuclei, and the indirect detection of the standard model particles produced by the annihilation or decay of the dark matter particles, of course the large collider also tries to find the evidence of the presence of the dark matter. The third chapter discusses a new dark matter structure, ultra-dense dark matter halo (UCMHs), which is proposed by Ricotti Gould in 2009. It is possible to form the original black hole when the initial density disturbance is in the region of 0.3. However, when the density disturbance is less than this critical value but greater than 10-3, the original black hole can not be formed, but it will evolve into a supertight dark matter halo. Compared with the general dark matter halo, the density of the UCMHs is larger and the formed time is earlier. If the dark matter is composed of WIMP particles, the UCMH can be observed by the Fermi satellite or the atmospheric Cerenkov detector (ACTs) by the particles such as X-rays generated by the annihilation or decay of the WIMP, and the generated neutrino signal is observed by the IceCube/ DeepCore or other neutrino detector. for a given model we calculate the flux of the x-rays generated by the wIMP annihilation from the UCMH, while we also give the lower limit of the UCMH abundance that can be detected, and the upper limit of the UCMH abundance that has not been detected, and the limitation of the UCMH abundance is converted into the limit of the initial curvature disturbance on the small scale. Decay will become important if the dark matter particles are not annihilated. So we also calculated the X-ray signal produced by the decay of WIMP in UCMH, and the limitation of UCMH abundance and initial curvature disturbance was obtained. In addition to the X-ray signal, we have also studied the neutrino signal from UCMH. Although the neutrino is not detected, we present the limitation of the UCMH abundance and transform into the limit of the initial curvature disturbance on the small scale. In the fourth chapter, we sum up the work of this paper and look forward to the future research.
【學(xué)位授予單位】：南京大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2014
【分類號】：P145.9
【共引文獻】
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1 常進;;暗物質(zhì)粒子探測:意義、方法、進展及展望[J];工程研究-跨學(xué)科視野中的工程;2010年02期
2 徐強;陳斌;;A New Exponential Gravity[J];Communications in Theoretical Physics;2014年01期
3 劉文中;歐陽君;楊煥雄;;Quintessence Field as a Perfect Cosmic Fluid of Constant Pressure[J];Communications in Theoretical Physics;2015年03期
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1 封常青;空間暗物質(zhì)探測衛(wèi)星量能器讀出電子學(xué)方法研究[D];中國科學(xué)技術(shù)大學(xué);2011年
2 傅金林;尋找η/η'不可見衰變和電磁轉(zhuǎn)變J/ψ→Pl~+l~-[D];南京大學(xué);2012年
3 陳亞正;暗物質(zhì)直接探測中核效應(yīng)的研究[D];南開大學(xué);2012年
4 李昌鴻;CSTB反彈宇宙（Coupled Scalar Tachyon Bounce Cosmos）模型的構(gòu)造、系統(tǒng)分析以及實驗探測[D];南京大學(xué);2014年
5 陳楠;Z′及CDEX相關(guān)的暗物質(zhì)理論研究[D];清華大學(xué);2014年
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1 衡陽;超級神岡實驗中弱作用重粒子的直接尋找研究[D];清華大學(xué);2010年
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3 李天嬙;DBI暗物質(zhì)暗能量統(tǒng)一模型的理論研究[D];遼寧師范大學(xué);2014年
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