Dark energy and its connections to neutrino, baryo/leptogenesis and dark matter

Xinmin Zhang Institute of High Energy Physics Beijing Outline of the talkI. Current status on determination of the equation of state

of dark energy and Quintom ModelII. Interacting dark energy and mass varying neutrino

III. A unified model of dark energy, dark matter and baryo

genesis

IV. Searching for CPT violation with CMB

V. Summary

Dark Energy:* Negative pressure:

)3(3

4/ p

Gaa

0a 3/1/ 03 pwp* Smoothly distributed, (almost ) not clusteringCandidates:* Cosmological constant (or vacuum Energy)

g

GT

8

1/ pw eV10~m

)102(8

3-

43

eVG

p

12010~/ obth cosmological constant problem!

* Dynamical Field: Quintessence, K-essence, Phantom etc

)(2

1QVQQL

VQpVQ QQ 22

2

1,

2

1

11 Qw

Constraints on the Dark Energy

A quantity characterizing the property of Dark Energy:

Equation of state: w(Z)=P/ρ

For example :

* Vacuum Energy: w=-1

* Quintessence:

* Phantom:

Using the recent 157 Supernova data

published by Riess et al. (astro-ph/0402512)

* Within 2 σ, the cosmological constant fits well the data

* Data mildly favors a running of the W across -1

Model independent analysis with the following parameterization： 1 ， w(z)=w_0 + w_1* z

2 ， w(z)=w_1 + w_a*z/(1+z)

Feng, Wang & Zhang

Astro-ph/0404224

Huterer & Cooray

Astro-ph/0404062

z

w

Implication in model building of dark energy If the running of w(Z), especially a transition across –1, confirmed

in the future, big challenge to the model building

* Vacuum : w=-1

* Quintessence: ( 精质 )

* Phantom: （幽灵） * K-essence: or but cannot across -1 A new scenario of Dark Energy : Quintom （精灵） (Zhang et al. Astro-ph/0404224) For ex:

single scalar:

multi-scalar:

Quintom Model building: Why challeQuintom Model building: Why challenges?nges?No-Go Theorem:No-Go Theorem: Equation of State W can not Equation of State W can not cross over w=-1 if the following cross over w=-1 if the following conditions are satisfied:conditions are satisfied:

I. Einstein GravityII. Minimal CouplingIII. Single Scalar Field IV. Without higher derivative

Examples of Quintom-like Models: 1. two scalar field 2. single scalar field with higher derivative 3. including vector field …… 4. Nonminimal Coupling ……..

Vikman Phys. Rev. D 71, 023515 (2005)Gong-Bo Zhao et al. astro-ph/0507482

Bo Feng et al. astro-ph/0404224

…….Hao Wei, PhD Thesis

Detailed study on: Two-field models of Quintom Dark Energy -Xiao-fei Zhang ,Hong Li, Yunsong Piao and Xinmin Zhang

I. Quintom model with two scalar fields:

II. Quintom model with Phantom field and neutrino:

Astro-ph/0501652

Quintom with Single scalar field and Higher Derivative

Forequivalent to two fields

Mingzhe Li, Bo Feng, Xinmin Zhang, hep-ph/0503268

astro-ph/0407259, Steen Hannestad, Edvard Mortsell

Adding CMB,LSS data

Include DE perturbation when Include DE perturbation when parametrizing the EOSparametrizing the EOS

Seljak et alAstro-ph/0407372

Ch. Yeche et alAstro-ph/0507170

Neglect DE perturbations

Including DE perturbation only when w>-1

BIASED!!

How to calculate the How to calculate the fluctuationfluctuation of Dark Energy ?? of Dark Energy ??

Difficulty:Difficulty:

, 0 ,1 ww

Perturbation of DE continuous never diverge!

Zhao et.al PRD 72,123515

Dark Energy Perturbation in two-field Quintom model

Our strategy to handle perturbations Our strategy to handle perturbations when w crosses -1 for parametriz when w crosses -1 for parametriz

ed EOSed EOSI. Quintessence – like perturbation;

II. Phantom – like perturbation;

III.

1)(zw

1)(zw

1)(1 zw

0 ,0

Constrains on dark energy with SN Ia (Riess) + SDSS + WMAP-1

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

Jun-Qing Xia, Gongbo Zhao, Bo Feng, Hong Li and Xinmin Zhang Phys.Rev.D73, 063521, 2006

)1/(*1 zzwww 0

WMAP+SDSS+Riess WMAP+SDSS+SNLS

Comparision of global fitting results with SN Ia (Riess) and SNLS

Constrain on dark energy by WMAP group (importance of perturbation)

Current constrains on dark energy1. Cosmological constant fit the data well

2. Dynamical model are not ruled out

3. Quintom is mildly favored

Short summary :

Features of Quintom ( “ 精灵 ” ) Dark Energy Model

I. Challenges to Model building: A lot of recent studies on the models of Dark Energy with equation of state across -1

II. Dark energy perturbation well defined: Implications in CMB, LS

S ……

III. Different from cosmological constant, Quintessence and Phantom in the determination of the evolutions and the fate of the universe

Oscillating Quintom

Oscillating Quintom and the Recurrent Universe: astro-ph/0407432 Bo Feng, Minzhe Li, Yunsong Piao, Xinmin Zhang

Parameterization: Astro-ph / 0605366

Bump-like dark energyBump-like dark energy

EoS with feature:

Probing this feature with GRB??

Precise Hubble diagram from SNe IaPrecise Hubble diagram from SNe Ia From Dr. Xiao Feng Wang’s Hangzhou talk ( May, 2006)From Dr. Xiao Feng Wang’s Hangzhou talk ( May, 2006)

Interacting Dark Energy

Current data favors Quintom

Quintom Dark Energy is described by dynamical scalar fields

Expected also to interact with the matter directly. Open new possibilities for the detection.

* Direct coupling with ordinary matter

Constraint from the limits on the long-range force

* Interacting with DM (Peebles et al )

* Interacting with neutrinos ---Mass varying neutrinos

* Derivatively couplings----Cosmological CPT violation CMBPol

M

llQ

RcR NNQ

m

Xinmin Zhang etal. PRD68, 087301 (2003)

Dark Energy and neutrinos：

Any connection between Dark Energy and neutrinos?

1. ΛCDM:

2. QCDM:

443 )()10( mev

plQ M

meVm

23310

If yes, very interesting: 2 of the biggest discoveries in the recent years Predictions : neutrino masses vary and cosmological CPT violation

Where, Corresponding the formula for the neutrino mass upper limit now is:

Astro-ph/0309800

New features of neutrino Dark Energy model:

I. Unlike the ordinary matter

the massive neutrino has equation of state

II. Neutrino plays an important role in the evolution

of the universe

III. Mass varying neutrinos effects on CMB, LSS

IV. Testing mass varying neutrinos with GRB

V. Testing mass varying with neutrino oscillations

0w

Cosmological evolution of Interacting Dark Energy models with mass varying neutrinos hep/ph/0412002 -Xiaojun Bi, Bo Feng, Hong Li, Xinmin Zhang

Astro-ph/0503349

Testing mass varying neutrino with short GRB -Hong Li, Zigao Dai, Xinmin Zhang: hep-ph/0411228

Neutrino oscillation probes of Dark Neutrino oscillation probes of Dark EnergyEnergy

D.B. Kaplan D.B. Kaplan et al.et al., PRL 93,09180, PRL 93,091801 (2003);1 (2003);

V. Barger V. Barger et al.,et al., hep-ph/0502196; hep-ph/0502196;M. Cirelli M. Cirelli et al.et al., hep-ph/0503028., hep-ph/0503028.

Basic idea ：

given by

)()()( ieff VV

)()( 0 Mmmeff

)(effV

Solar Neutrino oscillationNeutrino oscillation ：

ee rA

UrMmrM

rMrMmU

Edr

di

00

0)(

))(())((

))(())((

2

12

202

23

23

21

01

npei ,,,

Derivative couplings: A unified model of dark energy, dark matter and baryon matter

1) A unified model of baryogenesis and dark energy ----Quintessential baryo/leptogenesis

2) Probing CPT violation with WMAP and Boomerang

3) When SUSYing, Quintessino is dark matter particle ----A unified model of dark matter and dark energy

M.Li, X.Wang, B.Feng, X. Zhang PRD65,103511 (2002) M.Li & X. Zhang ， PLB573,20 (2003)

BJ

M

QcL

intIn thermo equilibrium

Cosmological CPT violation baryogenesis Quintessential Baryo(Lepto)genesis

M

TQgc

TO

T

Tg

dEmEEg

nn

bbbb

TETEm

bbbB bb

6])([

6

][)(2

n

23

3

]/)exp[(11

]/)exp[(11

2/122

2

32

45

2Tgs

MTg

Qgcsn b

B

24

15/

Cohen & Kaplan

The value of depends on the model of Quintessence

Cosmological CPT violation!

Searching for CPT Searching for CPT violationviolation

Cosmological CPT violation: predicting <TB> and <EB>

Bo Feng, Mingzhe Li , Jun-Qing Xia, Xuelei Chen and Xinmin ZhangPhys. Rev. Lett. 96, 221302 (2006)

(Note here the notation: G ~ E, C~ B)

Quintessino As Dark Matter•If susying the Quintessence: Quintessence: Q; Squintessence: σq ; Quintessino:

Similar to : Axion, Saxion, Axino Majoron, Smajoron, Majorino

•If is lighter than , could serve as Dark matter

•Susying the following interaction (H: SU(2) doublet)

gives

gives

* Prediction: long-lived charged particle:

(R. Mohapatra and Zhang)

(X. Bi, M. Liand Zhang)

* Non-thermal production of Quintessino:

Summary

I. Quintom Dark Energy Models:

Current data consistent with the cosmological constant

but mildly favor the Quintom: a dynamical dark energy with

Equation of state evolving and crossing -1

need more data and model building of Quintom dark energy

II. The massive neutrino might have connection with

dark energy; open up a possibility of detecting dark energy

non-gravitationally

need more study

III. Derivative couplings --A unified model of dark energy, dark matter and ba

ryogenesis: Quintessino as dark matter particle

IV. Cosmological CPT Violation: Predicting <TB> and <EB>

need more data

Thanks !Thanks !