1. The CMB shape (Black body spectrum); 2. Detect the temperature fluctuation (~10-5).
Precision Cosmology
SN, Maxima, Boomerang, DASI, WMAP, SDSS, 2dfGRS, “Golden Sample”, SNLS
精灵
暗能量场：宇宙空间中的“以太”
QF F 精细结构常数的改变
Quintom ??
Dark Energy and neutrinos：
Any connection between Dark Energy and neutrinos?
1. ΛCDM: (103ev)4 (m )4
2. QCDM: mQ
Cosmology and Collider Physics
中科院高能所 张新民
2006.10.28
John C. Mather NASA Goddard Space Flight Center, Greenbelt, MD, USA, George F. Smoot University of California, Berkeley, CA, USA
nB
nb nb
gb
2 2
E(E2
m
1/ 2
m2)
dE
[1 1exp[(E
)
/
T
]
] 1
1exp[(E ) /T ]
nB
c
gbQ T 2 6M
宇宙熵密度：
s
2 2
45
gT 3
nB / s
15c
4 2
gbQ gMT
观测值：
nB / s 10 10
模型： V (Q) f (Q)Exp[( / M Planck )Q]
COBE
Inflation + Dark Matter + Dark Energy + Particle Physics
WMAP
Questions:
1. Inflation mechanism ... ? 2. Dark Matter Particle ... ? 3. Properties of Dark Energy ... ? 4. How to generate the matter and anti-matter asymmetry ... ?
Sloan Digital Sky Survey (SDSS) Two degree Field Galaxy Redshift Survey
III. 数据拟和分析：
Monte Carlo Markov Chains 上海超级计算机
创新点：暗能量扰动
Results
No questions about the existence of Dark Matter and Dark Energy
Solar Neutrino oscillation ：
i
d dr
e
1 2E
U
(m10 (M
M 1 (r ))2 3 (r))2
(M 3 (r))2 (m20 M 2 (r))2
U
A(r ) 0
0 0
e
D.B. Kaplan et al., PRL 93,091801 (2003);
V. Barger et al., hep-ph/0502196;
II. One of such experiments is the HEAT. There is an excess above 8 GeV, which can be explained by dark matter annihilation.
III. Sensitivity will be greatly improved at Pamela and AMS02.
两种产生机制： 1. 热产生 （像光子退耦一样） 2. 非热产生
Dark Matter Detection
There are great pct detection. New experiments are going to take data.
The last result is given by CDMS. The null result give stronger constraints on the SUSY parameters. The DAMA region is almost entirely excluded.
Dark Matter Detection
C.S. Li, Z.G. Si, ......
一个统一描述 DE 和 B 的模型
问题的提出： Dirac 理论
反粒子 －－－－Baryogenesis “真空不空” －－－－ Dark Energy
微观
宇观
Any connections?
Lint
c Q M
J
B
重子有效化学势
热平衡
1033 eV
m 2 M pl
If yes, very interesting: 2 of the biggest discoveries in the recent years Predictions : neutrino masses vary and cosmological CPT violation
Solution:
Q 3
4 10(2
4)
g1 / 2T 2
nB
/
s
0.01c
T M
Cosmological CPT Violation
1. 右手中微子的 Majorana 质量项破坏轻子数 2. 右手中微子的 Yukawa 耦合项破坏 C 和 CP 3. 右手中微子脱离热平衡
Sphaleron 过程将部分轻子数转化为重子数
V.A. Kuzmin, V.A. Rubakov and M.E. Shaposhnikov, Phys. Lett. B 155, 36 (1985).
粒子宇宙学研究进展
•暗物质粒子探测
•暗能量模型
•Baryogenesis and Top Quark Physics
需要新物理
暗物质：中微子是暗物质，但不是冷暗物 质；什么是冷暗物质？
暗能量：势能和真空能是暗能量，但理论 预言太大－宇宙学常数问题？
反物质：标准模型可以产生正反物质不对 称，但太小，需要新物理？
Outline of the talk
Current Status on Cosmology; Baryogenesis and collider physics; Cosmological CPT violation and its test with CMB; Summary
宇宙学模型及其检验
Q ll
M
QN
c R
N
R
m
Xinmin Zhang etal. PRD68, 087301 (2003)
Neutrino oscillation probes of Dark Energy
Basic idea：meff ( ) m0 M ( )
given by Veff ()
Veff ( ) V ( ) i ( ) i ,e, p, n
轴子(Axion)
为解决强CP破坏问题而引进 (Peccei & Quinn)
g
2 s
32
a~a G a
( 10 9 ?)
轴子: 标量粒子
ma
~
2QCD f PQ
~ 103 eV
探测:
至今未发现
WIMP(弱作用重粒子)
例如，超对称模型中的中性伴随子(neutralino).
Picture of DM distribution at the galaxy
Sakharov 三条件: A.D. Sakharov, JETP Lett. 5, 24 (1967).
1. 重子数破坏 2. C 和 CP 破坏 3. 脱离热平衡
Leptogenesis
M. Fukugita and T. Yanagida, Phys. Lett. B 174, 45 (1986); P. Langacker, R.D Peccei, and T. Yanagida, Mod. Phys.Lett.A 1,541 (1986); M.A. Luty, Phys. Rev. D 45, 455 (1992); R.N. Mohapatra and X. Zhang, Phys. Rev. D 45, 2688 (1992).
I. 宇宙学参数
暗能量模型：
Primordial power spectrum:
Dark Energy equation of state:
II. 天文观测数据： • 超新星（SN）
High Z Search Team (Riess et al. 2004) Supernova Legacy Survey (SNLS)
Taking the contribution from dark matter annihilation into account the data can be well explained.
Detection of Dark Matter in China
I. Yang BaJing
II. Quintessino Heavy long-lived charged particle
• 微波背景辐射（CMB）
Wilkinson Microwave Anisotropy Probe (WMAP) Observations
Balloon Observations Of Millimetric Extragalactic Radiation And Geophysics