·高被引論文摘要·

焦善慶，楊本立，江光佐，等

·高被引論文摘要·

被引頻次：38

多成分宇宙中穩(wěn)定粒子的質(zhì)量和半徑估算

焦善慶，楊本立，江光佐，等

討論了多成分宇宙中穩(wěn)定粒子的基本性質(zhì)，用宇宙演化中的自由流阻尼標(biāo)度理論統(tǒng)一估算了經(jīng)典黑洞、普朗克粒子、核子、電子、暗物質(zhì)粒子、光子的質(zhì)量和半徑，量級(jí)與某些已知數(shù)據(jù)相符。得到宇觀與微觀世界通過(guò)普朗克粒子發(fā)生相互關(guān)聯(lián)，核子則是兩者的明顯分界，不同領(lǐng)域表現(xiàn)出不同的規(guī)律性。

普朗克粒子；黑洞；暗物質(zhì)粒子；核子；光子

來(lái)源出版物：云南大學(xué)學(xué)報(bào)（自然科學(xué)版）, 2001, 23(2): 119-121

被引頻次：26

量子力學(xué)和相對(duì)論的結(jié)合、不相容及發(fā)展

張一方

摘要：基于量子力學(xué)和相對(duì)論的比較，二者既可以結(jié)合又存在不相容。由此討論它們的某些可能的發(fā)展方向。特別探討了3個(gè)方面：測(cè)不準(zhǔn)原理和光速恒定等的矛盾；量子的非局域性顯示出糾纏態(tài)應(yīng)該是一種新的作用距離和強(qiáng)度中等的相互作用；由Dirac負(fù)能態(tài)推導(dǎo)出的負(fù)物質(zhì)可能是一種暗物質(zhì)。

關(guān)鍵詞：量子論；相對(duì)論；測(cè)不準(zhǔn)原理；非局域性；負(fù)物質(zhì)；暗物質(zhì)

來(lái)源出版物：云南大學(xué)學(xué)報(bào)：自然科學(xué)版, 2008, 30(1): 41-46

被引頻次：20

暗物質(zhì)粒子探測(cè)：意義、方法、進(jìn)展及展望

常進(jìn)

摘要：本文回顧了暗物質(zhì)發(fā)現(xiàn)的歷史，介紹了暗物質(zhì)粒子探測(cè)方法和目前國(guó)際最新觀測(cè)結(jié)果，重點(diǎn)討論了空間探測(cè)暗物質(zhì)粒子的技術(shù)方法和可能的突破點(diǎn)，就我國(guó)開(kāi)展暗物質(zhì)粒子空間探測(cè)提出了一些建議。

關(guān)鍵詞：暗物質(zhì)；空間探測(cè)

來(lái)源出版物：工程研究：跨學(xué)科視野中的工程, 2010, 2(2): 95-99

被引頻次：16

光子、暗物質(zhì)粒子、普朗克粒子與狄拉克大數(shù)

焦善慶，楊本立，江光佐，等

摘要：討論了光子、中微子（或暗物質(zhì)粒子）的靜質(zhì)量，從不同的觀點(diǎn)和方法對(duì)黑洞質(zhì)量、核子質(zhì)量、光子質(zhì)量、暗物質(zhì)粒子質(zhì)量和普朗克粒子質(zhì)量作了估算。發(fā)現(xiàn)它們與狄拉克大數(shù)存在某種深層的內(nèi)在關(guān)聯(lián)。

關(guān)鍵詞：光子；暗物質(zhì)粒子；黑洞；普朗克粒子；狄拉克大數(shù)

來(lái)源出版物：云南大學(xué)學(xué)報(bào)（自然科學(xué)版）, 2000, 22(4): 263-265

被引頻次：15

相對(duì)論與量子力學(xué)的關(guān)系及理論的發(fā)展

張一方

摘要：相對(duì)論和量子力學(xué)之間的關(guān)系，既是密切聯(lián)系的，有時(shí)又彼此不相容，特別是測(cè)不準(zhǔn)關(guān)系和光速不變。由此論述了超弦、環(huán)等量子引力理論。最后論證了由Dirac負(fù)能態(tài)推導(dǎo)出的負(fù)物質(zhì)是一種暗物質(zhì)的可能性。

關(guān)鍵詞：量子論；相對(duì)論；引力理論；負(fù)物質(zhì)；暗物質(zhì)

來(lái)源出版物：商丘師范學(xué)院學(xué)報(bào), 2008, 24(12): 57-61

被引頻次：12

暗物質(zhì)與暗能量研究新進(jìn)展

蔡榮根，周宇峰

摘要：本文簡(jiǎn)要回顧了暗物質(zhì)和暗能量研究的歷史。重點(diǎn)綜述了暗物質(zhì)實(shí)驗(yàn)探測(cè)的最新進(jìn)展和理論研究動(dòng)態(tài)，對(duì)各種可能的暗能量模型進(jìn)行了比較介紹。最后對(duì)我國(guó)暗物質(zhì)和暗能量方面的研究進(jìn)行了介紹和展望。

關(guān)鍵詞：暗物質(zhì)；暗能量

來(lái)源出版物：中國(guó)基礎(chǔ)科學(xué), 2010, 3: 1-6

被引頻次：8

暗物質(zhì)空間探測(cè)器BGO量能器的讀出設(shè)計(jì)

郭建華，蔡明生，胡一鳴，等

摘要：暗物質(zhì)空間探測(cè)器是中國(guó)科學(xué)院紫金山天文臺(tái)暗物質(zhì)空間天文實(shí)驗(yàn)室提出的，其目的是為了探測(cè)暗物質(zhì)粒子湮滅可能產(chǎn)生的高能電子和伽瑪粒子。整個(gè)探測(cè)器主要由BGO（Bismuth germanate，鍺酸鉍）高能圖像量能器和閃爍體徑跡探測(cè)器構(gòu)成。探測(cè)器的能量探測(cè)范圍將覆蓋10 GeV到10 TeV的高能電子和伽瑪粒子，其中高能粒子的能量主要沉積在BGO量能器中。為了驗(yàn)證探測(cè)器方案，紫金山天文臺(tái)暗物質(zhì)空間天文實(shí)驗(yàn)室設(shè)計(jì)了暗物質(zhì)空間探測(cè)器BGO量能器的讀出系統(tǒng)原型，并對(duì)其進(jìn)行了初步的測(cè)試。

關(guān)鍵詞：儀器；探測(cè)器；暗物質(zhì)；宇宙線

來(lái)源出版物：天文學(xué)報(bào), 2012, 53(1): 72-79

被引頻次：8

中微子的靜止質(zhì)量及其在物理學(xué)和宇宙學(xué)上的意義

周?chē)?guó)榮

摘要：簡(jiǎn)要地介紹了中微子的發(fā)現(xiàn)歷史及其基本特性，著重介紹了Super-Kamiokande中微子天文臺(tái)大氣中微子實(shí)驗(yàn)和太陽(yáng)中微子實(shí)驗(yàn)的基本原理及其最新實(shí)驗(yàn)結(jié)果，對(duì)中微子的靜止質(zhì)量在太陽(yáng)中微子失蹤問(wèn)題、粒子物理學(xué)和宇宙學(xué)上的意義作了討論，指出了與中微子靜止質(zhì)量相關(guān)的3個(gè)有待解決的問(wèn)題。

關(guān)鍵詞：中微子；粒子物理；宇宙學(xué)；暗物質(zhì)

來(lái)源出版物：物理, 1999, 28(5): 290-294

被引頻次： 7

量子史瓦茨黑洞和暗物質(zhì)

劉遼，裴壽鏞

摘要：引入Sommerfeld作用量量子化條件來(lái)處理Schwarzschild黑洞的量子化問(wèn)題。發(fā)現(xiàn)此類(lèi)量子化黑洞存在一個(gè)質(zhì)量為的基態(tài)，處于基態(tài)的量子Schwarzschild黑洞不再存在Hawking蒸發(fā)和任何其他輻射，可名之曰暗星。它的存在不僅可以解決信息丟失的疑難，而且極可能是構(gòu)成暗物質(zhì)的主要候選者。

關(guān)鍵詞：量子史瓦茨黑洞；暗物質(zhì)

來(lái)源出版物：物理學(xué)報(bào), 2006, 55(9): 4980-4982

被引頻次：7

暗物質(zhì)、暗能量對(duì)宇宙未來(lái)命運(yùn)的影響

焦善慶，許弟余，龔自正

摘要：據(jù)實(shí)驗(yàn)檢測(cè)和理論計(jì)算，論證了現(xiàn)時(shí)中微子的超對(duì)稱伴子“中性微子”是宇宙暗物質(zhì)的最佳候選粒子。認(rèn)為超新星爆炸釋放的暗能量，迫使宇宙背景光子熱平衡態(tài)的溫度T、壓強(qiáng)p上升。將壓強(qiáng)類(lèi)比為“反引力”，當(dāng)“反引力”（壓強(qiáng)）大于引力，則宇宙將加速膨脹；當(dāng)“反引力”小于引力，則宇宙將收縮。

關(guān)鍵詞：暗物質(zhì)；中性微子；暗能量；光子熱平衡態(tài)；反引力；宇宙命運(yùn)

來(lái)源出版物：云南大學(xué)學(xué)報(bào)：自然科學(xué)版, 2006, 28(4): 316-318

被引頻次：3709

關(guān)鍵詞：cosmology, theory; dark matter; galaxies, halos; methods, numerical

來(lái)源出版物：Astrophysical Journal, 1996, 462(2): 563-575

被引頻次：1911

The evolution of large-scale structure in a universe dominated by cold dark matter

Davis, M; Efstathiou, G; Frenk, CS; et al.

Abstract:The results of numerical simulations of nonlinear gravitational clustering in universes dominated by weakly interacting, 'cold' dark matter are presented. The numerical methods used and the way in which initial conditions were generated are described, and the simulations performed are catalogued. The evolution of the fundamental statistical properties of the models is described and their comparability with observation is discussed. Graphical comparisons of these open models with the observed galaxy distribution in a large redshift survey are made. It is concluded that a model with a cosmological density parameter omega equal to one is quite unacceptable if galaxies trace the mass distribution, and that models with omega of roughly two, while better, still do not provide a fully acceptable match with observation. Finally, a situation in which galaxy formation is suppressed except in sufficiently dense regions is modelled which leads to models which can agree with observation quite well even for omega equal to one.

來(lái)源出版物：Astrophysical Journal, 1985, 292: 371-394

被引頻次：1378

The origin of dwarf galaxies, cold dark matter, and biased galaxy formation

Dekel, A; Silk, J

Abstract:The formation of dwarf, diffuse, metal-poor galaxies as a result of supernova-driven winds is reexamined in view of the accumulating data on the systematic properties of dwarfs in the Local Group and in the Virgo Cluster. The observed luminosity-radiusmetallicity relations are found to be produced naturally inside dominant halos, with a mass-radius relation that resembles the predictions of the “cold” dark matter cosmological scenario. The critical condition for global gas loss as a result of the first burst of star formation is that the virial velocity be below a critical value on the order of 100 km s-1. In any hierarchial scenario for galaxy formation, this condition leads to two distinct classes of galaxies as observed: (1) the diffuse dwarfs which mostly originate from typical density perturbations; and (2) the normal, brighter galaxies which can originate only from the highest density peaks. This provides a statistical biasing mechanism for the preferential formation of bright galaxies in denser regions (clusters and superclusters).

來(lái)源出版物：Astrophysical Journal, 1986, 303: 39-55

被引頻次：1273

The formation and evolution of galaxies within merging dark matter haloes

Kauffmann, G; White, SDM; Guiderdoni, B

Abstract:We construct semi-analytic models for galaxy formation within the framework of a hierarchical clustering scenario for structure formation in the Universe. We use the algorithm of Kauffmann & White to generate ensembles of merging histories for present-day dark matter haloes with a wide range of circular velocities. A galaxy is assumed to form from gas which cools and turns into stars at the centre of a halo until that halo merges with a more massive object. At this time the galaxy loses its source of new gas and becomes a non-dominant object within a larger group or cluster. Our methods thus enable us to ‘look inside’ present dark matter haloes and investigate the formation, evolution and merging of the galaxies that they contain. We begin by investigating the properties of haloes withVc= 220 km s-1, and use the observed properties of our Milky Way system to tune the free parameters that regulate star-formation, hydrodynamic feedback from supernovae and the transformation of discs into spheroids by mergers. We then show that the same parameters lead to good agreement between the properties of galaxies in aVc= 1000 km s-1halo and observational data on the Virgocluster of galaxies. This model correctly reproduces the observed trends in the luminosity, colour, gas content and morphology of galaxies. Turning to an investigation of the properties of the galaxy population as a whole, we highlight a problem that arises when applying this model to a ‘standard’ cold dark matter universe. If the zero-point of the Tully-Fisher relation is set by the properties of our Milky Way system, we find that standard CDM predicts too many haloes and results in a B-band luminosity density of the universe that is a factor of 2 too high. The only apparent solution to this problem is to assume that many haloes remain observationally undetectable. We also compute the gas mass-luminosity relation for galaxies, the variation in galaxy morphology as a function of luminosity, star formation histories according to environment, the field galaxy luminosity function, and predictions for faint galaxy counts in the B and K bands. We conclude that, although it would be premature to attempt a detailed quantitative fit to specific cosmological models, the qualitative agreement between the data and the general picture that we present is already very encouraging.

來(lái)源出版物：Monthly Notices of the Royal Astronomical Society, 1993, 264(1): 201-218

被引頻次：1103

The mass function of dark matter haloes

Jenkins, A; Frenk, CS; White, SDM; et al.

Abstract:We combine data from a number of N-body simulations to predict the abundance of dark haloes in cold dark matter (CDM) universes over more than four orders of magnitude in mass. A comparison of different simulations suggests that the dominant uncertainty in our results is systematic and is smaller than 10-30 per cent at all masses, depending on the halo definition used. In particular, our‘Hubble volume’ simulations of tau CDM and Lambda CDM cosmologies allow the abundance of massive clusters to be predicted with uncertainties well below those expected in all currently planned observational surveys. We show that for a range of CDM cosmologies and for a suitable halo definition, the simulated mass function is almost independent of epoch, of cosmological parameters and of the initial power spectrum when expressed in appropriate variables. This universality is of exactly the kind predicted by the familiar Press-Schechter model, although this model predicts a mass function shape that differs from our numerical results, overestimating the abundance of ‘typical’ haloes and underestimating that of massive systems.

關(guān)鍵詞：gravitation; methods : numerical; cosmology: theory; dark matter

來(lái)源出版物：Bulletin of the American Meteorological Society, 2007, 88: 1383-1394

被引頻次：1103

Dark matter substructure within galactic halos

Moore, B; Ghigna, S; Governato, F; et al.

Abstract:We use numerical simulations to examine the substructure within galactic and cluster mass halos that form within a hierarchical universe. Clusters are easily reproduced with a steep mass spectrum of thousands of substructure clumps that closely matches the observations. However, the survival of dark matter substructure also occurs on galactic scales, leading to the remarkable result that galaxy halos appear as scaled versions of galaxy clusters. The model predicts that the virialized extent of the Milky Way's halo should contain about 500 satellites with circular velocities larger than the Draco and Ursa Minor systems, i.e., bound masses greater than or similar to 108M☉and tidally limited sizes greater than or similar to 1 kpc. The substructure clumps are on orbits that take a large fraction of them through the stellar disk, leading to significant resonant and impulsive heating. Their abundance and singular density profiles have important implications for the existence of old thin disks, cold stellar streams, gravitational lensing, and indirect/direct detection experiments.

關(guān)鍵詞：cosmology : observations; cosmology : theory; dark matter; galaxies : clusters : general; galaxies : formation

來(lái)源出版物：Astrophysical Journal, 1999, 524(1): L19-L22

被引頻次：960

An analytic model for the spatial clustering of dark matter haloes

Mo, HJ; White, SDM

Abstract:We develop a simple analytic model for the gravitational clustering of-dark matter haloes to understandhow their spatial distribution is biased relative to that of the mass. The statistical distribution of dark haloes within the initial density field (assumed Gaussian) is determined by an extension of the Press-Schechter formalism. Modifications of this distribution caused by gravitationally induced motions are treated using a spherical collapse approximation. We test this model against results from a variety ofN-body simulations, and find that it gives an accurate description of a bias function,b (M, R, δ)= δh(M, R, δ)/δ,where δh(M, R, where δ)is the mean overdensity of haloes of mass M within spheres which have radiusRand mass overdensityδ; the results depend only very weakly on how haloes are identified in the simulations. This bias function is sufficient to calculate the cross-correlation between dark haloes and mass, and again we find excellent agreement between simulation results and analytic predictions. Because haloes are spatially exclusive, the variance in the count of objects within spheres of fixed radius and overdensity is significantly smaller than the Poisson value. This seriously complicates any analytic calculation of the autocorrelation function of dark haloes. Our simulation results show, however, that this autocorrelation function is proportional to that of the mass over a wide range inR, even including scales where both functions are significantly greater than unity. Furthermore, the constant of proportionality is very close to that predicted on large scales by the analytic model. Since analytic formulae for the nonlinear autocorrelation function of the mass are already known, this result permits an entirely analytic estimate of the autocorrelation function of dark haloes. We use our model to study how the distribution of galaxies may be biased with respect to that of the mass. In conjunction with other data these techniques should make it possible to measure the amplitude of cosmic mass fluctuations and the density of the Universe.

關(guān)鍵詞：methods, analytical; galaxies, clusters, general; galaxies, formation cosmology, theory; dark matter

來(lái)源出版物：Monthly Notices of the Royal Astronomical Society, 1996, 282(2): 347-361

被引頻次：886

Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes

Sheth, RK; Mo, HJ; Tormen, G; et al.

Abstract:The Press-Schechter, excursion set approach allows one to make predictions about the shape and evolution of the mass function of bound objects. The approach combines the assumption that objects collapse spherically with the assumption that the initial density fluctuations were Gaussian and small. The predicted mass function is reasonably accurate, although it has fewer high-mass and more low-mass objects than are seen in simulations of hierarchical clustering. We show that the discrepancy between theory and simulation can be reduced substantially if bound structures are assumed to form from an ellipsoidal, rather than a spherical, collapse. In the original, standard, spherical model, a region collapses if the initial density within it exceeds a threshold value,δsc. This value is independent of the initial size of the region, and since the mass of the collapsed object is related to its initial size, this means thatδscis independent of final mass. In the ellipsoidal model, the collapse of a region depends on the surrounding shear field, as well as on its initial overdensity. In Gaussian random fields, the distribution of these quantities depends on the size of the region considered. Since the mass of a region is related to its initial size, there is a relation between the density threshold value required for collapse and the mass of the final object. We provide a fitting function to thisδec(m) relation which simplifies the inclusion of ellipsoidal dynamics in the excursion set approach. We discuss the relation between the excursion set predictions and the halo distribution in high-resolution N-body simulations, and use our new formulation of the approach to show that our simple parametrization of the ellipsoidal collapse model represents an improvement on the spherical model on an object-by-object basis. Finally, we show that the associated statistical predictions, the mass function and the large-scale halo-to-mass bias relation, are also more accurate than the standard predictions.

關(guān)鍵詞：galaxies : clusters : general; cosmology : theory; dark matter

來(lái)源出版物：Monthly Notices of the Royal Astronomical Society, 2001, 323(1): 1-12

被引頻次：862

First results from the LUX dark matter experiment at the Sanford Underground Research Facility

Akerib, DS; Araujo, HM; Bai, X; et al.

Abstract:The Large Underground Xenon (LUX) experiment is a dual-phase xenon time-projection chamber operating at the Sanford Underground Research Facility (Lead, South Dakota). The LUX cryostat was filled for the first time in the underground laboratory in February 2013. We report results of the first WIMP search data set, taken during the period from April to August 2013, presenting the analysis of 85.3 live days of data with a fiducial volume of 118 kg. A profile-likelihood analysis technique shows our data to be consistent with the background-only hypothesis, allowing 90% confidence limits to be set on spin-independent WIMP-nucleon elastic scattering with a minimum upper limit on the cross section of 7.6×10-46cm2at a WIMP mass of 33 GeV/c2. We find that the LUX data are in disagreement with low-mass WIMP signal interpretations of the results from several recent direct detection experiments.

來(lái)源出版物：Physical Review Letters, 2014, 112(9): 091303

被引頻次：859

Accelerating universes with scaling dark matter

Chevallier, M; Polarski, D

Abstract:Friedmann-Robertson-Walker universes with a presently large fraction of the energy density stored in anX-component withwX＜ -1/3, are considered. We find all the critical points of the system for constant equations of state in that range. We consider further several background quantities that can distinguish the models with differentwXvalues. Using a simple toy model with a varying equation of state, we show that even a large variation ofwXat small redshifts is very difficult to observe withdL(z) measurements up toz＜similar to＞ 1. Therefore, it will require accurate measurements in the range 1 ＜z＜ 2 and independent accurate knowledge of Ωm,0(and/or ΩX,0) in order to resolve a variablewXfrom a constantwX.

來(lái)源出版物：International Journal of Modern Physics D,2001, 10(02): 213-223

The structure of cold dark matter halos

Navarro, JF; Frenk, CS

We use N-body simulations to investigate the structure of dark halos in the standard cold dark matter cosmogony. Halos are excised from simulations of cosmologically representative regions and are resimulated individually at high resolution. We study objects with masses ranging from those of dwarf galaxy halos to those of rich galaxy clusters. The spherically averaged density profiles of all our halos can be fitted over two decades in radius by scaling a simple “universal” profile. The characteristic overdensity of a halo, or equivalently its concentration, correlates strongly with halo mass in a way that reflects the mass dependence of the epoch of halo formation. Halo profiles are approximately isothermal over a large range in radii but are significantly shallower thanr-2near the center and steeper thanr-2near the virial radius. Matching the observed rotation curves of disk galaxies requires disk mass-to-light ratios to increase systematically with luminosity. Further, it suggests that the halos of bright galaxies depend only weakly on galaxy luminosity and have circular velocities significantly lower than the disk rotation speed. This may explain why luminosity and dynamics are uncorrelated in observed samples of binary galaxies and of satellite/spiral systems. For galaxy clusters, our halo models are consistent both with the presence of giant arcs and with the observed structure of the intracluster medium, and they suggest a simple explanation for the disparate estimates of cluster core radii found by previous authors. Our results also highlight two shortcomings of the CDM model. CDM halos are tooconcentrated to be consistent with the halo parameters inferred for dwarf irregulars, and the predicted abundance of galaxy halos is larger than the observed abundance of galaxies. The first problem may imply that the core structure of dwarf galaxies was altered by the galaxy formation process, and the second problem may imply that galaxies failed to form (or remain undetected) in many dark halos.