WIMPS & Neutrinos
description
Transcript of WIMPS & Neutrinos
WIMPS & Neutrinos
G.G.Ross, Edinburgh, 9th February 2005
What do we know about
?
They exist!
Massive
3 neutrinos
Mixing angles large
Limited room for sterile neutrino – wait for MiniBoone
2 21LSNDm eV
Neutrinos
WIMPS & Neutrinos
What do we know about
?
WIMPS ?
WIMPS & Neutrinos ?
Neutrinos : Majorana or Dirac?
Hierarchical or nearly degenerate?
Inverted hierarchy or normal hierarchy?
Origin of small mass - seesaw?
(Non-Abelian) family symmetry?
mixing lepton # violation?
What we don’t know about
WIMPS & Neutrinos
What we don’t know about
?
Dark Matter : Does it exist? MOND alternative
Milgrom, Beckenstein
- Only visible mattergives structure seen
- Gravitational lensing
- Density perturbations?
WIMPS & Neutrinos
What we don’t know about
?
Dark Matter : Does it exist?
Where is it?
3110
The jury is still out -
Recent study shows one can get
excellent description of our galaxy
with local DM density < 0.3GeV/cm
Basel group astro-ph/0212516,0312461
. .spiral galaxy rotation curves...c f
astro-ph/0403154
CDM successful at large scales (or MOND)
WIMPS & Neutrinos
What we don’t know about
?
Dark Matter : Does it exist?
Where is it?
What is it?
Can we find it?
Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
(WIMPS)
WIMPS & Neutrinos ?
Neutrinos : Majorana or Dirac?
Hierarchical or nearly degenerate?
Inverted hierarchy or normal hierarchy?
Origin of small mass - seesaw?
(Non-Abelian) family symmetry?
mixing lepton # violation?
What we don’t know about
Dirac or Majorana? MajoranaHH
M
0<H > Diracc
If Dirac why is so small?
Propagate in new space dimensions - small due to flux spreading
Right-handed in the bulks
4 ( ) ( ) ( , 0)L Rd x x H x x y
*
/1,2
( ) iny RR nRM
n
x e
* *4.10Planck
HM TeV
M Mm eV
Dirac see-saw
L RR
L
DMH
DD
m HM
R No cosmological problem as
not produced in early universe
2.05 tritium -decaym eV
0.23 anisotropiesm eV CMB
A degenerate spectrum is indicative of a non-Abelian family symmetry
still room …
. . (3) : m i ie g SO Barbieri, Hall, Kane, GGRAntush, King
?u GUTM M
?d lGUTM M
(2) (2) ?L RSU SU(2) (2) ?L RSU SU
Family?Family?
Symmetries Coherent picture of quark and lepton masses and mixing?
DATA :
iu?
1GeV
i id il
1210 910 610 310 310
Masses
Mixing
1 0.218 0.224 0.002 0.005
0.218 0.224 1 0.032 0.048
0.004 0.015 0.03 0.048 1CKMV
0.72 0.89 0.45 0.69 0.2
0.24 0.58 0.39 0.76 0.52 0.84
0.24 0.58 0.39 0.76 0.53 0.84MNSV
2 13 3
1 1 16 3 2
1 1 16 3 2
0
10-1
10-2
10-3
10-4
eV
Bi-Tri Maximal Mixing …
HarrisonScott
Non AbelianStructure?
D
3
8 3 4 3 4
3 4 2 3 2 3
3 4 2 3
Mm
1
a a
a
Vacuum alignment
3
0
0
1
23
0
1
1
2123
1
1
1
Barbieri, Hall, Kane, GGRDe Madeiros, GGR
0 0
3 23
i i
23 123
45 33
SU(
3) SU(2) ..
SU(3) SU(2)
' ..
q , l
i
???
1 i 3 3 2 i 23 23 3 i 123 23 4 i 23 123P= c c c ci i i i
(3), SU(3)SO
D
3
8 3 4 3 4
3 4 2 3 2 3
3 4 2 3
Mm
1
a a
a
Vacuum alignment
3
0
0
1
23
0
1
1
2123
1
1
1
0 0
3 23
i i
23 123
45 33
SU(
3) SU(2) ..
SU(3) SU(2)
' ..
q , l
i
(3), SU(3)SO1
2
3
1 2 3
M
M
M
M
M M
M
M
b e a
1M
TD DM MM M
Neutrinos?
WIMPS & Neutrinos
What we don’t know about
?
Dark Matter : Does it exist?
Where is it?
What is it?
Can we find it?
Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
(WIMPS)
Sterile neutrinos?
Axions?
Standard Model Neutrinos?3
2
1 93
0.07
0.007
imheV
( 2.05 tritium -decay)m eV
( 0.23 anisotropies)m eV CMB
-No SM interactions apart from mixing
- 10 to avoid erasure of structures
m KeV
if thermally produced
What is dark matter?
a-m 0.01eV-18 20-very weakly interacting 10 10 EW
SUSY candidates
gravitinos, axinos – very weakly interacting, massive
With R-parity conservation LSP stable-nature of LSP model dependent
neutralinos, sneutrinos – (<)SM interactions
-32 -18 20 6 3 6 3EW10 , 10 10 ; 10 10 , 10 10EW GeV GeV
-3 10 2 310 10 ; 10 10EW GeV
1
0 0 321 2 03
1
02
0 cos sin sin sin
0 cos cos sin cos
cos sin cos cos 0
sin sin sin cos 0
Z W Z W
Z W Z WN
Z W Z W
Z W Z W
BM M MWM M M
M B W H HM M HM M
H
Neutralino mass matrix
LSP sensitive to parameters
0 1/ 2 2, , , , tan , im m M A CMSSM :
Ellis, Olive, Santoso, Spanos
CMSSM
0c ci i i
Q u Hdm m m m m
3 0c ci i id HQ u
m m m m m
3 3(1 0.2)Q Qim m
3 family symmetry brea king
Ramage,GGR
KK state For some compactifications LKP stable2
2 2. . / , /e g T Z S Z
For low scale of compactification LKP can make up dark matter :
1. . in SM with all states propagating in bulk can be LKPB e g
1
2
0.6v
( )B
pb
m TeV
1400: 1200Bm eVDM G
Wimpzilla 34DMm GeV v at unitarity bound and initial thermal abundance
1010DMm GeV non thermal production (e.g. gravitational)
Can we find WIMPS?
Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
Can we find WIMPS?
Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
Very low scattering cross sections
Can we find WIMPS?
Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
Neutralino interactions exhaustively studied
Ellis, Olive, Santoso, Spanos
CMSSM : Neutralino searches
spin independentN N contours
, 445 6MeV MeV
Ellis, Olive, Santoso, Spanos
CDMS II excluded
Kaluza Klein searches
1
2
0.6v
( )B
pb
m TeV not visible by current searches
Annihilation products ; .. 60%e e
.. 4%qq .. 35%
. . Neutralino de bcay to b, ...c f
Look for galactic annihilation production of , e
Signals could be visible if galactic cusps exist
– for LKP sharp cutoff on positron energy
WIMPS & Neutrinos ?
Neutrinos : Majorana or Dirac?
Hierarchical or nearly degenerate?
Inverted hierarchy or normal hierarchy?
Origin of small mass - seesaw?
(Non-Abelian) family symmetry?
mixing lepton # viola ? tion
What we could know about SUMMARY
?
?
Wimps Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
Indirect detection
Direct detection possible
Hierarchy : spontaneously broken family symm y etr
n
L RH M
spatial separ n atio
Yijk hqu n H2
DM , a a,ijk
dn e
Aijk n
2 e 2 i ijkn. #
Froggatt-Nielsen mixing
3 ( )R n R R
, structurequark leptonM M
, (specific string calc ulations + IRFP OK ) t bh gThird generation heavy
(?) b th h h (not expected to be precise with Wilson line break ing)
0.2
4 3 3
2
23
2
2
1
d
b
M
m
( , 0 0)dm S Q
0 0
( )
S Q
A
( )
CP
A
?Gauge mediat
S GRA
ion
U
Vives, GGR
( , )..
i j ci j aMP Q q H
Cannot align Yukawa and A terms
(3 ( , )) *c c
ij ij a ij ai j i jA Y Q q H i j P Y Q q H
, structurequark leptonM M
Similar structure for charged leptons Neutrino mixing not related to large RH mixing
WIMPS & Neutrinos ?
Neutrinos : Majorana or Dirac?
Hierarchical or nearly degenerate?
Inverted hierarchy or normal hierarchy?
Origin of small mass - seesaw?
(Non-Abelian) family symmetry?
mixing lepton # viola ? tion
What we could know about SUMMARY
?
?
Wimps Sterile neutrinos?
Little Higgs candidate?
Axions?
SUSY – neutralinos, sneutrinos, gravitinos, axinos
KK state?
Wimpzilla?
Cryptons,…
Indirect detection
Direct detection possible
CMSSM10 16/ 1.25, 0m m D
10 16/ 0, 0.4m m D Ramage, GGR
1
2
2 2 2 216 10, ,
2 2 2 216 10,
2 2 2 216 10
2 2 2 210 10
2 2 2 210 10
3
2
2
R R
R
R
Q u e
d L
e
H
H
m m g D
m m g D
m m g D
m m g D
m m g D
SO(10)