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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)
4/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
5/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
6/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
7/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
8/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
9/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
10/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
11/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”
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
12/12 ”Supersymmetric dark matter with low reheating temperature of the Universe”