Title: ??????: SU(3) C
1 ??????? ??????
??? 2006.6.5
2?????? (????)
- ???????
- ?????? SU(3) CSU(2)LU(1)Y
- Higgs ??????
???????????
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4WMAP The Biggest
Surprise Nothing Particular
Surprising ?Inflation ? ?
?
Important ???????
5- ??
- ???????
- ????????????
- ?????????
6?????
- ??????????,???????????????
- ?????????????,???????-????????
- ??????????????????,???,??????
- Inflation???inflaton?
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8- ???????
-
- ?????????
- II. ??????????
9Application showcase neutrino mass
neutrino mass and abundance
O. Elgaroy et al (2dFGRS) PRL 89, 061301 (2002)
hot dark matter suppress power at small scale
current cosmological bound (95 CL) m?lt1.7/3
eV (weak prior) m? lt0.6/3 eV (strong prior)
vs.
tritium decay m?e lt 2.2 eV
10hep-ph/0503257
11Weighing neutrinos in the presence of a running
primordial spectral indexastro-ph/0605742
- Bo Feng, Jun-Qing Xia, Jun'ichi Yokoyama, Xinmin
Zhang, Gong-Bo ZhaoThe three-year WMAP(WMAP3),
combined with other cosmological observations
from galaxy clustering and Type Ia Supernova
(SNIa), prefers a non-vanishing running of the
primordial spectral index independent of the low
CMB multipoles. Motivated by this feature we
study cosmological constraint on the neutrino
mass, which severely depends on what prior we
adopt for the spectral shape of primordial
fluctuations, taking possible running into
account. As a result we find a more stringent
constraint on the sum of the three neutrino
masses, m_\nu lt 0.76 eV (2 \sigma), compared with
the case where power-law prior is adopted to the
primordial spectral shape.
12?????????? ??(Axion)
?????(Neutralino)
??,???????? Interacting Dark
Matter Non-thermal produced
Neutralino Steril Neutrino
Gravitino Quintessino
13- ??(Axion)
- ????CP??????? (Peccei Quinn)
-
-
- ?? ????
-
- ??
-
- ?????
-
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16Cosmic rays from the halo of the MWsome weak
hints on DM
Baltz et al. 2002
- Some astrophysics observations can not be
explained by the canonical physics. They may
indicate the signal of DM, however, no conclusion
can be drawn now. - One of such experiments is the HEAT. (The HEAT
signal may indicate the non-thermal production or
the subhalo nearby)
17ASg and ARGO (High Duty cycle,Large F.O.V)
TeV
100GeV
???? ARGO ??RPC??
???? AS ? ???????????
Here comes the two experiments hosted by YBJ
observatory. One is call ASg, a sampling detector
covering 1 of the area and have been operated
for 15 years. The other full coverage one is
called ARGO, still under installation. ASg use
scintillation counter and ARGO use RPC to
detector the arrival time and the number of
secondary particles, with which the original
direction and energy of CR particle can be
restored. ASg has a threshold energy at a few TeV
while ARGO down to about 100GeV. Both experiment
have the advantages in high duty cycle and large
field of view. Because for both of the
experiments there is only one layer of detector,
it is very difficult to separate the g ray shower
from CR nuclei showers. Working in the similar
energy range on mountain Jemez near Los Alamos,
by using water cherenkov technique, MILAGRO has
two layer of PMT, which enable it a rather good
capability to separate g ray from background.
Though it locates in a low altitude, has a
smaller effective area, it has similar
sensitivity to ASg experiment. To combine this
technique with high altitude would greatly
improve the sensitivity of our current EAS
experiments.
ARGO hall, floored by RPC. Half installed.
18???
???? ????
?
???? w1/3, ?? w0
19??????? 1,???(?????) ??
???????! ???w-1?
???
Fine Tuning
202,????(Quintessence)
?
??
A.
????????
Within 2 s, the cosmological constant fits well
the data
Data mildly favors a running of the W across -1
21Constraints on EOS from SN Ia
- ??????
- I. ???? w
- II. ??????
- a. b.
- ?? SN Ia ?????
Astro-ph/0510447
22 Feng, Wang Zhang Astro-ph/0404224 Huterer
Cooray Astro-ph/0404062
23 Within 2 s, the cosmological constant fits well
the data
Data mildly favors a running of the W across -1
Feng, Wang Zhang Astro-ph/0404224
??1, ??? w-1 2,
Quintessence -1w1 3, Phantom
-1w 4, Quintom w transit
from below 1 to above -1
24astro-ph/0407259, Steen Hannestad, Edvard
Mortsell
Probing Dark Energy with Supernovae a
concordant or a convergent model? Authors J.-M.
Virey, A. Ealet, C. Tao, A. Tilquin, A.
Bonissent, D. Fouchez, P. Taxil,astro-ph/0407452
25 Constraints on dark energy with SN Ia (Riess)
SDSS WMAP-1
????? W0-1.30 W11.25
Observing dark energy dynamics with supernova,
microwave background and galaxy clustering
Jun-Qing Xia, Gong-Bo Zhao, Bo Feng, Hong Li and
Xinmin Zhang Phys.Rev.D73, 063521,
2006
26Global fitting with SN Ia, galaxy clustering and
WMAP3
- Quintom is also mildly favored
- The standard ?CDM model is
- still a good fit to the current data
-
Probing dynamics of DE with supernova, galaxy
clustering and the three-year Wilkinson
Microwave Anisotropy Probe (WMAP) observations
G.-B. Zhao, J.-Q. Xia, B. Feng and X. Zhang,
astro-ph/0603621
27Riess et al, astro-ph/0402512
SNAP Collaboration astro-ph/0405232
28?????????
- ??????????????
- ??????(Quintessence, Phantom, Quintom)?????
- Quintom is mildly favored
?????? ???????????--???????
29Quintessence ? ????????
?????????
30Quintessence ? ????????
????
???,???,???,PRD68, 087301 (2003)
??????????
GRB Delay of flight time? ?????? NEUTRINO
OSCILLATIONS AS A PROBE OF DARK ENERGY D.
Kaplan, A. Nelson, N. Weiner
31Cosmological evolution of Interacting Dark
Energy models with massvarying
neutrinos hep/ph/0412002
-Xiaojun Bi, Bo Feng, Hong Li, Xinmin Zhang
32??????????
????
?? ?????? ??,
???????
- D.B. Kaplan et al., PRL 93,091801 (2003)
- V. Barger et al., PRL 95 (2005) 211802
- M. Cirelli et al., NPB 719 219 (2005).
33??????????
????????????
34?????????
35Oscillating Quintom and the Recurrent Universe
astro-ph/0407432 Bo
Feng, Minzhe Li, Yunsong Piao, Xinmin Zhang
36Astro-ph / 0605366
Parameterization
37?????
??
BBN
CMB
Sakharov????
- ???B???(??)
- C?CP??( C???????, P????? )(CKM??)
- ?????(??????)
?????????????????,??,?????????, ???????
? ???CPT????
Spontaneous baryo(lepto)genesis ??
CPT?? ?????
38?????? Baryogenesis ??????? Leptogenesis
???????? ?? (???) ??????CP??
(?????2100????????????)
39Leptogenesis ??
M. Tegmark et al, Phys.Rev. D 69, 103501 (2004).
???????
Sakharov ??? A.D. Sakharov, JETP Lett. 5,
24 (1967).
1. ????? 2. C ? CP ?? 3. ?????
Leptogenesis M. Fukugita and T.
Yanagida, Phys. Lett. B 174, 45 (1986).
1. ?????? Majorana ???????? 2. ?????? Yukawa
????? C ? CP 3. ??????????
Sphaleron ??????????????
V.A. Kuzmin, V.A. Rubakov and M.E. Shaposhnikov,
Phys. Lett. B 155, 36 (1985).
40Seesaw ??
M. Gell-Mann, P. Ramond and, R. Slansky T.
Yanagida R.N. Mohapatra and G. Senjanovic S.L.
Glashow.
For a review, see S.M. Bilenky, C. Giunti, and
W. Grimus, Prog.Part. Nucl. Phys. 43, 1 (1999).
41Type-I Seesaw ???? Leptogenesis ??
M. Fukugita and T. Yanagida, Phys. Lett. B 174,
45 (1986) M.A. Luty, Phys. Rev. D 45, 455
(1992) R.N. Mohapatra and X. Zhang, Phys. Rev.
D 45, 2688 (1992).
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43????
????
W. Buchmuller, P. Di Bari, and M. Plumacher,
Nucl. Phys. B 665, 445 (2003) Annals. Phys.
315, 305 (2005).
44?????? ? ???
????? Dirac ?? ???
?----?Baryogenesis ???? ?----? Dark
Energy ??
?? Any connections?
45????????
??? ?
?????
???
??
Solution
46????
Bo Feng, Hong Li, Minzhe Li and
Xinmin Zhang Phys. Lett. B620(2005)27
??
???? in the future CMB polarization
experiments will be
Tested.
????
?baryogenesis
47Searching For CPT Violation With WMAP And
BOOMERANGastro-ph/0601095
- Bo Feng, Mingzhe Li, Jun-Qing Xia, Xuelei Chen,
Xinmin ZhangVersion accepted by PRL - We search for signatures of Lorentz and CPT
violations in the cosmic microwave background
(CMB) temperature and polarization anisotropies
by using the WMAP and the 2003 flight of
BOOMERANG (B03) data. We note that if the Lorentz
and CPT symmetries are broken by a Chern-Simons
term in the effective lagrangian, which couples
the dual electromagnetic field strength tensor to
an external four-vector, the polarization vectors
of propagating CMB photons will get rotated.
Using the WMAP data alone, one could put an
interesting constraint on the size of such a
term. Combined with the B03 data, we found that a
nonzero rotation angle of the photons is mildly
favored \Delta \alpha -6.04.0_-4.0
3.9_-3.7 deg (1, 2 \sigma).
48Cosmology and collider physics
- Baryogenesis two Higgs models, left-right
symmetric SUSY anomalous top,Higgs
couplings------tested by LHC - Dark matter Neutralino --------tested by LHC
- Dark energy inflation (scalar fields
quintessence, quintom inflaton) Higgs tested at
LHC
49 ?????,?????,??????????? ????????,????????????
50Thanks !