Supersymmetric dark matter with low reheating temperature ...
Transcript of Supersymmetric dark matter with low reheating temperature ...
Supersymmetric dark matterwith low reheating temperature of the Universe
Sebastian Trojanowski
National Center for Nuclear Research, Warsaw
COSMO 2014 – Chicago, August 29, 2014
L. Roszkowski, ST, K. Turzynski hep-ph/1406.0012
1/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
Motivation
What is the nature of dark matter (DM)?
⇒ Lightest Supersymmetric Particle(?)
LHC bounds ⇒ SUSY scale MS & 1 TeV⇒ popular higgsino DM with mχ ∼ 1 TeV. . .
. . .but what else? It’s difficult to get neutralino dark matterwith mχ > 1 TeV
Any prospects for discovery such heavy DM?
Gravitino DM – typically discussed upper limit on thereheating temperature TR . 107 − 108 GeV
What about lower limit on TR?
2/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
Reheating period in the evolution of the Universe
At the end of a period of cosmological inflation:
T ≈ 0
large potential energy of the inflaton field φ is transformed into thekinetic energy of recreated particles
then T (reheating)
If instantaneous reheating: Γφ = H =√
8π3M2
Plρφ and ρφ = ρrad(TR) ∼ T 4
R
Γφ =
√4π3g∗(TR)
45
TR2
MPldefines reheating temperature TR
If non-instantaneous reheating – Boltzmann equations:G. F. Giudice, E. W. Kolb, A. Riotto hep-ph/0005123, G. Gelmini et al. hep-ph/0602230
dρφdt
= −3Hρφ − Γφρφ inflaton field
dρRdt
= −4HρR + Γφρφ + 〈σv〉2〈EX 〉[n2X − (neq
X )2] radiation
dnXdt
= −3HnX − 〈σv〉[n2X − (neq
X )2] (+
b
mφΓφρφ
)dark matter
Radiation dominated (RD) epoch begins when T ∼ TR ,
before – the reheating period
3/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
Reheating period – evolution of the total supersymmetric yield
Y = ns with n =
∑i ni
T−−→ nχ
Y =
n / s
x = mχ / T
freeze-out
(low TR)
freeze-out
(high TR)
nn
χ
10-15
10-10
10-5 1
10-4 10
-2 1 102 10
4 106
dilution due to
fast expansion
RD epoch(low TR)
n ≈ neq
reheatingperiod
(low TR)
low TR
high TR
Dark matter particles freeze-out inthe reheating period:
freeze-out occurs at a slightlyhigher temperatures than inthe standard case
after freeze-out, but beforethe end of the reheatingperiod, the DM particles areeffectively diluted away
Ωχh2(low TR) ∼(TR
Tnewfo
)3 ( Toldfo
Tnewfo
)Ωχh
2(high TR)
G. F. Giudice, E. W. Kolb, A. Riottohep-ph/0005123
Ωχh2(low TR ) < Ωχh2(high TR )
(w/o inflaton decays to DM)
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Supersymmetric dark matter with low TR in the (N)MSSMthe lightest neutralino is natural DM candidate (R-parity conservation)depending on its composition it can be: bino, higgsino, wino, singlino(NMSSM) or a mixed statefor bino or singlino DM relic density can vary by several orders ofmagnitude for a fixed mχ
for bino DM ΩBh2(high TR) . g
−1/2∗,fo
(m
lm
B
)2 ( ml
460 GeV
)2
M. Drees et al. hep-ph/9207234, J. D. Wells hep-ph/9809504
for higgsino and wino DM Ωχh2 ∼ m2
χ, wino DM – Sommerfeld effect
ΩD
Mh
2 (
hig
h T
R)
mDM (TeV)
TR = 1 GeV
TR = 10 GeV
TR = 50 GeV
TR = 100 GeV
TR = 200 GeV
high TR
ΩDMh2 = 0.12 p10MSSM
bino
higgsino
wino
10-1
1
101
102
103
104
105
106
0 1 2 3 4 5 6
ΩD
Mh
2 (
hig
h T
R)
mDM (TeV)
1 GeV
TR = 10 GeV
TR = 50 GeV
TR = 100 GeV
TR = 200 GeV
high TR
ΩDMh2 = 0.12 p13NMSSM (95% CL)
singlino comp. > 99%
> 95%
10-1
1
101
102
103
104
105
106
107
108
0 1 2 3 4 5 6
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Higgsino DM
high TR
correct relic density for mχ ∼ 1 TeV
testable – DM direct detection σSIp
(Xenon1T)
low TR (w/o inflaton decays to DM)
correct relic density for mχ & 1 TeV
still testable
10-13
10-12
10-11
10-10
10-9
10-8
10-7
0 1 2 3 4 5
σpS
I (pb)
mχ1
(TeV)
p10MSSM (95% CL) high TR
LUX
Xenon 1T
bino
higgsino
σpS
I (pb)
mχ1
(TeV)
p10MSSM (95% CL) TR = 100 GeV
LUX
Xenon 1T
bino
higgsino
10-13
10-12
10-11
10-10
10-9
10-8
10-7
0 1 2 3 4 5
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Bino DM – high TR
correct relic density in the bulk region or with some specific conditions:(co)annihilations, resonances
only partly testable in DM direct detection experiments
possibly some hints from colliders (stau-coannihilation region)
Bino DM – low TR (w/o inflaton decays to DM)
correct relic density for wide range of mχ depending on TR
w/o specific mass patterns
σpS
I (pb)
mχ1
(TeV)
p10MSSM (95% CL) TR = 10 GeV
LUX
Xenon 1T
bino
10-13
10-12
10-11
10-10
10-9
10-8
10-7
0 1 2 3 4 5
σpS
I (pb)
mχ1
(TeV)
p10MSSM (95% CL) TR = 50 GeV
LUX
Xenon 1T
bino
higgsino
10-13
10-12
10-11
10-10
10-9
10-8
10-7
0 1 2 3 4 5
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Wino DM – high TR
correct relic density for mW ∼ 3 TeV (including Sommerfeld effect)
J. Hisano et al. hep-ph/0610249,A. Hryczuk et al. hep-ph/1010.2172
excluded by DM indirect detection (γ-ray line) for mW . 3.5 TeVT. Cohen et al. hep-ph/1307.4082, J. Fan et al. hep-ph/1307.4400, A. Hryczuk et al. hep-ph/1401.6212
Wino DM – low TR (w/o inflaton decays to DM)
correct relic density for heavy wino DM
testable – direct and/or indirect DM detection
σpS
I (pb)
mχ1
(TeV)
p10MSSM (95% CL) TR = 150 GeV
LUX
wino (ID excl.)
bino
higgsino
wino
10-13
10-12
10-11
10-10
10-9
10-8
10-7
0 1 2 3 4 5
Xenon 1T
TR
[G
eV
]
mW~ [TeV]
p10MSSM (95% CL)ΩW~ h
2 = 0.12
with Sommerfeld effect
w/o Sommerfeld effect
120
140
160
180
200
3.6 3.8 4 4.2 4.4 4.6 4.8 5
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Gravitino G DM
superpartner of graviton
extremely weakly interacting massive particle (EWIMP) – interaction ratesuppressed by MPl ∼ 1018 GeV
not directly testable, but some hints from the LHC may be possible
cosmological constraints
Gravitino relic density
ΩGh2 = ΩNTP
Gh2 + ΩTP
Gh2 low TR' ΩNTP
Gh2 =
mG
mχΩχh
2
*
Non-Thermal Production
late decays of the next-to-LSP
Thermal production
scatterings of superparticles
in the thermal plasma
HHHH
HHY
Big Bang Nucleosynthesis (BBN) constraints
late-time decays of the next-to-LSP to gravitino initiate electromagneticand hadronic cascades that destroy light nuclei in the early Universe
→ this alters BBN predictions
constraints depend on the next-to-LSP’s lifetime τ and relic density Ωχh2
as well as on the hadronic branching fraction BhK. Jedamzik hep-ph/0604251, M. Kawasaki et al. hep-ph/0804.3745
K. Jedamzik hep-ph/0710.5153, M. Kawasaki hep-ph/0703122
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Gravitino DM – low TR ΩGh2 =
mG
mNLSPΩNLSPh
2
Bino next-to-LSP
Bh & 0.1
τ ∼m2
G
m5B
for mB mG
BBN requires τ . 0.1 s
⇒ mB & 1.4(
mG
GeV
)2/5
TeV
Slepton next-to-LSP
lower Ωlh2 ⇒ larger mG
low Bh
τ ∼m2
G
m5l
(1−
m2G
m2l
)−4
ΩLO
SPh
2 (
hig
h T
R)
mLOSP (TeV)
TR = 1 GeV
TR = 10 GeV
TR = 100 GeV
TR = 200 GeV
NTP high TR
ΩG~h
2 = 0.12 mG
~ = 10 GeV
bino
higgsino
wino
stau
sneutrino
10-1
1
101
102
103
104
105
106
0 1 2 3 4 5 6
BBN excl.
too low ΩG~h
2 ΩLO
SPh
2 (
hig
h T
R)
mLOSP (TeV)
TR = 100 GeV
TR = 200 GeV
NTP high TR
ΩG~h
2 = 0.12 mG
~ = 1 TeV
bino
higgsino
wino
stau
sneutrino
10-1
1
101
102
103
104
105
106
0 1 2 3 4 5 6
BBN excl.
too low ΩG~h
2
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Gravitino DM – lower limit on TR
BBN + relic density constraints ⇒ lower limit on TR
min
TR
(G
eV
)
mG~ (GeV)
bino LOSPmτ~ < 5 TeV
mτ~ < 10 TeV
mτ~ < 15 TeV
0
50
100
150
200
0.1 1 10
min
TR
(G
eV
)
mG~ (GeV)
sneutrino LOSP
stau LOSP
100
150
200
250
300
350
400
100 1000
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Conclusions
for low enough reheating temperature TR neutralino freeze-outmay occur before the RD epoch – in the reheating period. . .
. . .this opens up new regions with neutralino dark matter
regions with heavy higgsino or wino DM can be tested indirect/indirect detection experiments
wino DM can be again allowed
bino DM – correct relic density w/o specific mass patterns
gravitino DM in such scenario is only produced in non-thermalproduction
BBN constraints in case of gravitino DM introduce lower limitTR & 100 GeV
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