Neutrino Probes of Dark Energy and Dark Matter

Transcription

1 March 25, 2010 Nutrino Probs of Dark Enrgy and Dark Mattr Shin ichiro Ando California Institut of Tchnology

2 Dark Enrgy and Dark Mattr No Big Bang SN Most of th nrgy in th Univrs is in dark componnts Dark Enrgy ~74% Causing cosmic acclration 0.5 BAO Flat CMB Kowalski t al., Astrophys. J. 686, 749 (2008) Dark Mattr ~22% Cannot b xplaind by ordinary mattr

3 Modls for Dark Enrgy and Dark Mattr Dark Enrgy (DE) Cosmological constant Λ Dynamical filds such as quintssnc Modifid gravity Etc. Dark Mattr (DM) Wakly intracting massiv particls (WIMP) E.g., SUSY nutralino Stril nutrinos Etc.

4 This Talk Effct of DE-nutrino intraction on nutrino oscillation Ando, Kamionkowski, Mocioiu, Phys. Rv. D 80, (2009) Intractions of kv stril nutrinos with mattr and implications for dirct dtction xprimnts Ando, Kusnko, arxiv: [hp-ph]

5 This Talk Effct of DE-nutrino intraction on nutrino oscillation Ando, Kamionkowski, Mocioiu, Phys. Rv. D 80, (2009) Intractions of kv stril nutrinos with mattr and implications for dirct dtction xprimnts Ando, Kusnko, arxiv: [hp-ph]

6 Quintssnc Homognous scalar fild Q slowly rolling down potntial V(Q) Equation of stat: w = p ρ = 1 2 Q 2 V (Q) 1 2 Q 2 + V (Q) Cf. EOS for cosmological constant: w = 1

7 Prcis Masurmnt of w Kowalski t al., Astrophys. J. 686, 749 (2008) w m BAO SN CMB CMB, SN Ia, BAO, gravitational lnsing, tc. Looking for dviation of w from 1 to xclud cosmological constant Currnt constraint: w 1 ± 0.1

8 Nutrino Probs of Dark Enrgy? If DE is mad of scalar fild, φ, thr might b scrt intraction with SM particls For xampl, if DE has som coupling with EM fild, it could chang propagation of photons in som way E.g., Carroll, Phys. Rv. Ltt. 81, 3067 (1998) If DE intracts with nutrinos, that may chang nutrino oscillation phnomnology

9 DE-Nutrino Intraction Intraction Lagrangian L int = νγ µ (a µ + b µ γ 5 )ν a µ,b µ µ φ Disprsion rlation H = [p 2 + m 2 + 2(a L ) µ p µ ] 1/2 p + m2 2 p + (a L) µ p µ p Apparnt Lorntz violation (a L ) µ = a µ + b µ

10 Nots on DE-nutrino intraction H = p + m2 2 p + (a L) µ p µ p In flavor basis, m2 is nondiagonal, inducing ordinary nutrino oscillation a L is in gnral nondiagonal in flavor basis Whn nutrino nrgy gts largr, th third trm bcoms mor and mor important For antinutrinos, sign of a L changs, so it is CPT violating Mor gnral discussion: E.g., Kostlcky and Mws 2004

11 Two-Flavor Oscillation i d dt νa ν b = m2 4E + m ff 2 cos 2θv sin 2θ v νa sin 2θ v cos 2θ v ν b cos 2θd sin 2θ d νa sin 2θ d cos 2θ d ν b Δm 2, θv: vacuum oscillation paramtrs mff, θd: ignvalu and mixing angl for al matrix How do w prob ths nw oscillation paramtrs rlatd to DE?

12 Highst-Enrgy Nutrinos Gorham t al., arxiv: [astro-ph.he] Guarantd population: cosmognic nutrinos Thy ar producd by UHECRs intracting with CMB photons Flux uppr limits ar obtaind by Augr, ANITA, tc.

13 Flavor Ratio of Cosmognic Nutrinos At production, typical flavor ratio is :μ:τ = 1:2:0 pγ CMB nπ + nµ + ν µ n + ν ν µ ν µ Aftr propagating long distanc, w xpct qual amount of μ and τ flavors according to ordinary oscillation If DE intraction coms into play at this nrgy rang, th flavor ratio might dviat from 1:1 Som xprimnts hav flavor snsitivity;.g., Augr can mainly dtct τ flavor using Earth-skimming vnts

14 Flavor Ratio of Cosmognic Nutrinos φ ντ φ νµ 1 sin 2 2θ d m 2 2E m ff For cosmognic nutrinos: m 2 2E 10 3 V GV = GV

15 Snsitivity for DE Intraction Ando, Kamionkowski, Mocioiu, Phys. Rv. D 80, (2009) Futur highst-nrgy nutrino xprimnts could improv currnt limits by ~7 ordrs of magnitud Currnt limits ar from atmosphric/acclrator nutrinos from Supr-K Ncssary nutrino vnts to obtain ths limits ar ~10 Systmatic uncrtaintis not includd in this analysis

16 Mattr-Inducd Oscillation If nutrinos propagat in mattr (.g., atmosphric nu), thn th mattr ffct will b inducd for flavor With th DE intraction at sufficintly high nrgis (E 50 GV), th rsonanc condition will b: m ff cos 2θ d = 2G F N For Earth, th RHS is ~10 22 GV, so if at sufficintly high nrgis, mff is largr than this th oscillation is dtrmind by DE trm; othrwis, it is supprssd du to larg mattr potntial This ffct is nrgy indpndnt as long as E 50 GV

17 ffiffiffi Mattr-Inducd Oscillation ffiffiffi Ando, Kamionkowski, Mocioiu, Phys. Rv. D 80, (2009) 1 m ff =10-21 GV m ff =10-22 GV 0.8 m ff =5 x10-23 GV E = 50 GV θd = 45 o P(ν µ ν ) Oscillation du to DE is supprssd by mattr ffct for smallr mff cosθ

18 Dirctional Dpndnc m ff also dpnds on dirction of nutrino bam (a L ) µ p µ ( µ φ)p µ φ(1 v ˆp) Evn though such an ffct is furthrmor supprssd, this could giv mor complling vidnc on DE-nutrino intraction

19 Summary for DE-Nutrino Intraction Som crtain form of DE-nutrino intraction modifis nutrino oscillation probability Such an ffct is in particular important at high nrgy rang W show that th futur cosmognic xprimnts can improv th currnt limits by 7 ordrs of magnitud Th sam intraction might b sn in nrgyindpndnt rsonanc condition in Earth or dirctional dpndnc of oscillation probability

20 This Talk Effct of DE-nutrino intraction on nutrino oscillation Ando, Kamionkowski, Mocioiu, Phys. Rv. D 80, (2009) Intractions of kv stril nutrinos with mattr and implications for dirct dtction xprimnts Ando, Kusnko, arxiv: [hp-ph]

21 Evidnc of Stril Nutrino Dark Mattr Lownstin, Kusnko, arxiv: [astro-ph.he] pulsar kick (MSW) too much dark mattr (xcludd) dark mattr (max) mass (kv) Chandra lin dark mattr (min) pulsar kick (off rsonanc) 3.0!9!9!9!9 0.5"10 1.0"10 1.5"10 2.0"10 sin 2! Dcay lin in X-rays from dwarf galaxy Willman 1 Infrrd paramtrs: m νs =5kV, sin 2 θ = 10 9

22 How Likly Ar Thy Dtctd Dirctly? Ando, Kusnko, arxiv: [hp-ph]! s Z!, µ, " Stril nutrinos hav small fraction of activ nutrino componnt! p,n, s W p,n,! Thrfor, thy can intract with SM particls through Z, W- xchang diagrams Ths ar vry straightforward to comput

23 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0

24 Charactristic Kinmatics Initial Stat Final Stat ν s E νs p νs v = m νs v E = m p =0 ν

25 Charactristic Kinmatics Initial Stat Final Stat E m ν s E νs p νs v = m νs v E = m p =0 ν

26 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat E m ν E ν

27 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat E m ν E ν p ν

28 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat ν E m p E ν p ν

29 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat ν E m p E ν p ν Kintic nrgy givn to a targt lctron is ~ ms 2 /2m ~ 25 V

30 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat ν E m p E ν p ν Kintic nrgy givn to a targt lctron is ~ ms 2 /2m ~ 25 V Thrfor, th targt atoms will b ionizd

31 Charactristic Kinmatics Initial Stat ν s E νs p νs v = m νs v E = m p =0 Final Stat ν E m p E ν p ν Kintic nrgy givn to a targt lctron is ~ ms 2 /2m ~ 25 V Thrfor, th targt atoms will b ionizd Enrgy spctrum of th ionizd lctron is sharply distributd

32 Scattring Cross Sction and Rat σ νs = cm 2 m 2 νs sin 2 θ v 1 5 kv R scattring =0.4 yr 1 m νs sin 2 θ Mdt Z 5 kv kton 25 ~1 kton yr xposur in background-fr dtctor is ncssary This is trmndously challnging, but might b possibl in th futur

33 Summary for Stril Nutrino Intraction W considrd scattring of kv stril nutrinos and atoms Evn though th cross sction is vry small, th intraction yilds obsrvabl signatur: ionization of atoms Th ncssary xposur for th background-fr dtctor is ~1 kton yr Th sam intraction also flips th nuclar spins; on could us this, by stting targts in magntic filds to dtct this spin flip

34 Appndix

35 Constraint to Intraction Modl Bfor closing, w discuss, for illustration, th implications of a masurmnt of a particular valu of th Lorntzinvarianc violating ffctiv mass paramtr m ff in trms of a spcific modl of DE-nutrino coupling. Prhaps th simplst intraction of this kind has th form L int M ð1 5 Þ ; (24) whr is a quintssnc fild, is a coupling-constant matrix, and M is som mass scal. Thus, a L ðtþl _ =M, and m ff ðtþ=m _, whr is th diffrnc btwn ignvalus of th matrix. For quintssnc, on xpcts _ M Pl H 0 ð1 þ wþ 1=2 (.g., Rf. [3]), whr M Pl is th Planck nrgy scal. In this cas, th mass scal M corrsponding to a givn m ff is 1 þ w 1=2 M 10 6 m ðþ ff 0: GV; (25) GV to th mass scal that controls th DE-nutrino intraction. Th ultra-high-nrgy - oscillation ffcts w hav discussd thus prob up to mass scals M 10 6 GV. Th - oscillations inducd by th mattr ffcts w discussd prob up to mass scals M 100 MV.