暗能量和宇宙学CPT破坏（PPT讲稿，南京大学物理系：李明哲）

暗能量和宇宙学CPT破坏 李明哲 南京大学物理系 粒子-核-宇宙学联合研究中心

暗能量和宇宙学CPT破坏 李明哲 南京大学物理系 粒子-核-宇宙学联合研究中心

Outline 1, Brief review on dark energy models, cosmological constant or dynamical dark energy, current status 2, Interacting dark energy direct coupling: l(yy, Fa Fpo, Ggo,. propagates long range force, spoils the flatness of the potential of dark energy derivative coupling oo(y, Foa, gas) spin-dependent force, shift symmetry, guarantee the flatness of the potential, cosmological CPT violation 2 3, Model: L-0,W(B-D)L (B-LL F Fkt Av FuU em F 12 3 (B-L儿L (1/2) B-L) 1/2 B-L) Leptogenesis Anomaly for CMB 4. Conclusion

Outline 1, Brief review on dark energy models, cosmological constant or dynamical dark energy, current status 2, Interacting dark energy: direct coupling: propagates long range force, spoils the flatness of the potential of dark energy derivative coupling: spin-dependent force, shift symmetry, guarantee the flatness of the potential, cosmological CPT violation 3, Model:    B L L L J ~  ( − ) Leptogenesis Anomaly for CMB 4, Conclusion ( , , ,...)     O  F G ( , , ,...)    L  F F G G

Brief Review on Dark Energy Supernova Cosmology Project Accelerating Universe ->Dark Energy Knop et al. (2003) 1 王王到 班王 Supe Projec SN Ia sCP, hzt Calan/Tololo redshift Z LRG SS(2dfGRS SDSS.) 三 己 k [h Mpe-l1

SN Ia (SCP, HZT….) LSS (2dfGRS, SDSS…) Brief Review on Dark Energy Accelerating Universe ->Dark Energy

1965 Penzias and CMB experiments 1992 COBE WMAP Multipole moment I 10 00 布4000 1000 0.5° Angular Size

CMB experiments

1.0 0.8 74% Dark Energy 22% Dark Matter 0.2 4 Atoms 0.0 0.00.20.40.60.81.0 No antimatter Dark matter? Dark energy Why no antimatter?

Dark matter? Dark energy? Why no antimatter? …… No antimatter

a 4G (P+3 P)>0 W≡p/p<-1/3 Negative pressure Candidates Cosmological constant T=As W=p/= Cosmological constant problem! P~(10e)4~10-123m S Weinberg RMP(1989)

Candidates: 1, Cosmological constant w p = = − / 1  Cosmological constant problem! 3 4 123 4 ~ (10 ) ~10 mpl eV − −  T  = g  ( 3 ) 0 3 4 = − + p  G a a    w  p /   −1/ 3 Negative pressure S. Weinberg, RMP (1989)

2, Dynamical dark energy*o Quintessence: L=(80)-Vo 1/202-T 1≤w≤1 1/2p-+1 ≈"()≤H0~10-3 ek Flat po otential Phantom: L=-(8P)2-v( w Cannot cross -1 no-go theorem Feng, Wang Zhang, PLB(2005); Vikman, PRD(2005); Zhao, Xia, Li, Feng Zhang, PRD(2005); Xia, Cai, Qiu, Zhao &Zhang, IJMPD (2008) Quintom: w crosses-1 L=(ao)-(ap)-voe) feng, Wang& Zhang PLb(2005) C L=(p)+,n2(Oy)2-V() i, Feng Zhang, JCAP (2005) M L=-v(D)1-a2do9+Bo2o Cai, i, Lu, Piao, Qiu&Zhang, PLB(2007)

2, Dynamical dark energy 1 2 ( ) ( ) 2 L V =  −   2 2 1/ 2 1/ 2 V w V   − = + Quintessence: −   1 1 w w 0 Phantom: 1 2 ( ) ( ) 2 L V = −  −   w −1 meff V H eV 33 ''( ) 0 ~10−    K-essence: L L( , )  =       w w  −  − 1, 1 Cannot cross -1, no-go theorem Feng, Wang & Zhang, PLB(2005);Vikman, PRD(2005);Zhao, Xia, Li, Feng & Zhang, PRD(2005); Xia, Cai, Qiu, Zhao &Zhang, IJMPD(2008) Quintom: 2 2 1 2 1 2 1 1 ( ) ( ) ( , ) 2 2 L V =  −  −     Feng, Wang & Zhang, PLB(2005) 2 2 2 2 1 ( ) ( ) ( ) 2 c L V M =  +  −    Li, Feng & Zhang, JCAP(2005) w crosses -1 ……… Flat potential 2 2 2 2 1 ( ) ( ) ( ) 2 c L V M =  +  −            2 L = −V( ) 1− '  + ' Cai,Li,Lu,Piao,Qiu&Zhang, PLB(2007)

It is important to determine w of de by cosmological observations Parameterization of equation of state A)W=W0+w 1z(for small z B)W=W0+w 1Z/(1+z(used mostly in the literature) C)W=W0+w 1 sin(w_ 2 In(a)+w 3)

It is important to determine w of DE by cosmological observations! Parameterization of equation of state: A) w=w_0+w_1 z (for small z) B) w=w_0+w_1 z / (1+z) (used mostly in the literature) C) w=w_0+w_1 sin(w_2 ln(a)+w_3)

Current constraint on the equation of state of dark energy 2,0 Quintom A Quintom A Quintessence 1.5 Quintessence 1.0 0.5 phantom WMAP5+BAO+ =0.5 sN③307)+BBN WMAP+BAO+SN+BEN QuintomB Phantom Quintom B 1,0 1315-1413-12-11-1 09-08-07-06-0.5 0.8 Xia, Li, Zhao, Zhang PRd(2008 WMAP5 result E. Komatsu et al. arXiv: 0803 0547 Status: 1) Cosmological constant fits data well 2)Dynamical model not ruled out; 3)Best fit value of equation of state slightly w across-1> Quintom model

Current constraint on the equation of state of dark energy WMAP5 result E. Komatsu et al., arXiv:0803.0547 Xia, Li, Zhao, Zhang, PRD(2008) Status: 1) Cosmological constant fits data well; 2) Dynamical model not ruled out; 3) Best fit value of equation of state: slightly w across -1 → Quintom model Quintessence phantom Quintom A Quintom B

Interacting Dark Energy Dynamical dark energy is expected to have interactions to the rest of the world besides the gravity Two types of couplings: direct derivative 1, direct coupling ling c l(yv, Fog Fp,Goog ng ·· 10-3e A Long range force M C>m MMAA 4M

Dynamical dark energy is expected to have interactions to the rest of the world besides the gravity. Two types of couplings: direct & derivative 1, direct coupling Interacting Dark Energy ( , , ,...)       L F F G G M c m eV 33 10−   10 ( ) 4 M pl M c −  A. Long range force Constrained tightly! S.M. Carroll, PRL(1998) B. Instability under quantum corrections     eV m M m    −7 2 ~ 10 4 M M pl  ~ ew ~