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

Contraction of dark matter galactic halos due to baryonic infall

Blumenthal, GR; Faber, SM; Flores, R; et al.

The formation of dark halos in a universe dominated by cold dark matter

Frenk, CS; White, SDM; Davis, M

Dark matter substructure within galactic halos

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

暗物質(zhì)

·編者按·

暗物質(zhì)（Dark Matter），是指無法通過電磁波的觀測進行研究，也就是不參與電磁相互作用的物質(zhì)。目前只能透過引力產(chǎn)生的效應得知。天文觀測表明：宇宙中可見的重子物質(zhì)僅占宇宙總能量組成的5%左右，看不見的暗物質(zhì)占27%。1933年，瑞士天文學家Zwicky最早提出了暗物質(zhì)的概念。他采用2種方法測量星系團的質(zhì)量，分別是對大量星系的運動速度進行分析，間接估計出星系團的質(zhì)量；以及通過星系團內(nèi)星系的亮度來估計星系團的質(zhì)量。發(fā)現(xiàn)其比太陽的質(zhì)光比要大400倍左右。因此，他推測星系團可能主要由不發(fā)光的物質(zhì)構(gòu)成，暗物質(zhì)的概念由此產(chǎn)生。

目前，人們已經(jīng)普遍認可了暗物質(zhì)的存在，暗物質(zhì)也成為研究宇宙大尺度結(jié)構(gòu)形成過程的必不可少的要素。科學界大致有3種方法探測暗物質(zhì)粒子：第1種方法是用加速器創(chuàng)造暗物質(zhì)粒子，研究其物理特性；第2種方法直接探測暗物質(zhì)粒子和原子核碰撞所產(chǎn)生的信號；第3種辦法是觀測暗物質(zhì)粒子湮滅后產(chǎn)生的穩(wěn)定粒子，如伽馬射線、正電子、反質(zhì)子、中微子等。

有科學家預測，未來暗物質(zhì)研究必將從天文觀測轉(zhuǎn)向?qū)Π滴镔|(zhì)粒子性質(zhì)的實驗探測。未來的10～20年將是暗物質(zhì)研究最重要和關鍵的時期。

本專題得到郭建華研究員（中國科學院紫金山天文臺）、岳騫副教授（清華大學）的大力支持。

·熱點數(shù)據(jù)排行·

截至2016年12月13日，中國知網(wǎng)（CNKI）和Web of Science（WOS）的數(shù)據(jù)報告顯示，以“暗物質(zhì)”為詞條可以檢索到的期刊文獻分別為625、8327條，本專題將相關數(shù)據(jù)按照：研究機構(gòu)發(fā)文數(shù)、作者發(fā)文數(shù)、期刊發(fā)文數(shù)、被引用頻次進行排行，結(jié)果如下。

研究機構(gòu)發(fā)文數(shù)量排名（CNKI）

研究機構(gòu)發(fā)文數(shù)量排名（WOS）

作者發(fā)文數(shù)量排名（CNKI）

作者發(fā)文數(shù)量排名（WOS）

作者發(fā)文數(shù)量排名（CNKI）（續(xù)表）

作者發(fā)文數(shù)量排名（WOS）（續(xù)表）

期刊發(fā)文數(shù)量排名（CNKI）

期刊發(fā)文數(shù)量排名（WOS）

根據(jù)中國知網(wǎng)（CNKI）數(shù)據(jù)報告，以“暗物質(zhì)”等為詞條可以檢索到的高被引論文排行結(jié)果如下。

國內(nèi)數(shù)據(jù)庫高被引論文排行

國內(nèi)數(shù)據(jù)庫高被引論文排行（續(xù)表）

根據(jù)Web of Science統(tǒng)計數(shù)據(jù)，以“暗物質(zhì)”等為詞條可以檢索到的高被引論文排行結(jié)果如下。

國外數(shù)據(jù)庫高被引論文排行

·經(jīng)典文獻推薦·

基于Web of Science檢索結(jié)果，利用Histcite軟件選取LCS（Local Citation Score，本地引用次數(shù)）TOP 50文獻作為節(jié)點進行分析，得到本領域推薦的經(jīng)典文獻如下。

We consider the possibility that the neutralcurrent neutrino detector recently proposed by Drukier and Stodolsky could be used to detect some possible candidates for the dark matter in galactic halos. This may be feasible if the galactic halos are made of particles with coherent weak interactions and masses 1-106GeV; particles with spindependent interactions of typical weak strength and masses 1-102GeV; or strongly interacting particles of masses 1-1013GeV.

來源出版物：Physical Review D, 1985, 31(12): 3059-3063

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.

來源出版物：Astrophysical Journal, 1985, 292: 371-394

Contraction of dark matter galactic halos due to baryonic infall

Blumenthal, GR; Faber, SM; Flores, R; et al.

Abstract:Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.

來源出版物：The Astrophysical Journal, 1986, 301: 27-34

The formation of dark halos in a universe dominated by cold dark matter

Frenk, CS; White, SDM; Davis, M

Abstract:The formation of galactic halos in a flat universe dominated by cold dark matter is investigated. Halos of galactic scale form in abundance only afterzof about 3. Most present-day halos had at least two progenitors of similar size atznot less than 1. The typical rotation speed of halos at the present day is only about 10 percent of their rms velocity dispersion. Dark halos are generically triaxial with, perhaps, a slight preference for near-prolate configurations. It is concluded that, if it is correct, the standard idea that galaxies form by condensation of gas with dark halos may actually require a high-density universe in order to be compatible with observation.

來源出版物：Astrophysical Journal, 1988, 327: 507-525

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.

cosmology : observations; cosmology : theory; dark matter; galaxies : clusters : general; galaxies : formation

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

典

文章題目第一作者來源出版物1 Detectability of certain dark-matter candidates Goodman, MW Physical Review D, 1985, 31(12): 3059-3063 2 The evolution of large-scale structure in a Davis, M Astrophysical Journal, 1985, 292: 371-394 universe dominated by cold dark matter 3 Contraction of dark matter galactic halos due to Blumenthal, GR The Astrophysical Journal, 1986, 301: 27-34 baryonic infall 4 The formation of dark halos in a universe Frenk, CS Astrophysical Journal, 1988, 327: 507-525 dominated by cold dark matter 5 Dark matter substructure within galactic halos Moore, B Astrophysical Journal, 1999, 524(1): L19-L22

Detectability of certain dark-matter candidates

Goodman, MW; Witten, E