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Transcript of Physics Opportunities with Supernova Neutrinos 周 顺 中科院高能所理论室...
Physics Opportunities withSupernova Neutrinos
周 顺中科院高能所理论室
中国科学技术大学交叉学科理论研究中心合肥, 2015-3-26
Outline
Supernova Neutrinos Physics Opportunities Neutrino Mass Scale WDM Sterile Neutrinos Summary and Outlook
Galactic SN 1054Distance: 6500 light years
(2 kpc)Center: Neutron Star
( R~30 km)Progenitor : M ~ 10 solar
masses
Red : Optical (Hubble)
Blue : X-Ray (Chandra)
Stellar Collapse and SN Explosion
Hydrogen Burning
Main-sequence star Helium-burning star
HeliumBurning
HydrogenBurning
© Raffelt
Onion structure
Degenerate iron core: r 109 g cm-3
T 1010 K MFe 1.5 Msun
RFe 8000 km
Collapse (implosion)
© RaffeltStellar Collapse and SN Explosion
Neutrino-driven Explosion
© Raffelt
Newborn Neutron Star
50 km
Proto-Neutron Star
r rnuc = 3 1014 g cm-3
T 30 MeV
Stellar Collapse and SN Explosion
Newborn Neutron Star
50 km
Proto-Neutron Star
r rnuc = 3 1014 g cm-3
T 30 MeV
Neutrino cooling by diffusion
Gravitational binding energy
Eb 3 1053 erg 17% MSUN c2
This shows up as 99% Neutrinos 1% Kinetic energy of explosion (1% of this into cosmic rays) 0.01% Photons, outshine host galaxy Neutrino luminosity
Ln 3 1053 erg / 3 sec
3 1019 LSUN
While it lasts, outshines the entire visible universe
© RaffeltStellar Collapse and SN Explosion
Raffelt, 1996
Kitaura, Janka & Hillebrandt astro-ph/0512065
Supernova Neutrinos: Theoretical Prediction
Supernova 1987A23 February 1987
Sanduleak - 69 202
Large Magellanic Cloud SN 1987A
Distance : 165 000 light yrs (50 kpc)
Center : Neutron Star (expected, but not
found)Progenitor : M ~ 18 solar
masses
Supernova Neutrinos: SN 1987A
Hirata et al., PRD 38 (1988) 448
Arnett et al.,ARAA 27 (1989)
Kamiokande-II (Japan): Water Cherenkov (2,140 ton) Clock Uncertainty ± 1 min
Irvine-Michigan-Brookhaven (US): Water Cherenkov (6,800 ton) Clock Uncertainty ±50 ms
Baksan LST (Soviet Union): Liquid Scintillator (200 ton) Clock Uncertainty +2/-54 s
Mont Blanc: 5 events, 5 h earlier
Supernova Neutrinos: SN 1987A
E b [1
053 e
rgs]
Spectral anti-νe Temperature [MeV]
Jegerlehner, Neubig & Raffelt astro-ph/9601111
Assumptions:
Thermal Equipart.
Conclusions: Collapse Ave.Ener. Duration
Problems : 24
events by
chance
Supernova Neutrinos: SN 1987A
Supernova Neutrinos: Astrophysics & Astronomy
Explosion Mechanism : Neutrino-driven Explosion
The prompt shock halted at 150 km,
by disintegrating heavy nuclei
Neutrinos deposit their energies via
interaction with matter; 1 % neutrino
energy leads to successful explosion
Simulations in 1D & 2D for different
progenitor masses observe explosions
3D simulation has just begun; but no
clear picture (resolution, progenitors)for a review, Janka, 1211.1378
For Optical Observations : SuperNova Early Warning System (SNEWS)
Arnett et al.,ARAA 27 (1989)
Super-K IceCube
LVD Borexino
http://snews.bnl.gov/
Alert @BNL
Neutrinos arrive several hours before photons
To alert astronomers several hours in advance
Supernova Neutrinos: Astrophysics & Astronomy
Gravitational waves from SN Explosions Locate the SN via neutrinos
Bounce
GWs from asymmetricneutrino emission
GWs from convective mass flows
ee
nepe
Müller, Rampp, Buras, Janka,& Shoemaker, astro-ph/0309833
“Towards gravitational wave signals from realistic core collapse supernova models”
Beacom & Vogel, astro-ph/9811350
SK
SK 30
90 %None
7.8° 3.2°
1.4° 0.6°
95% CL half-coneopening angle
Tomàs et al., hep-ph/0307050
n-tagging efficiency
Supernova Neutrinos: Astrophysics & Astronomy
Neutrino Mass Bound : Time delay of massive particles
22
eV 10
MeV 10
kpc 50 s 57.2
m
E
Dt
G. Zatsepin, 1968
Kamiokande-II data
IMB data
Estimate:
Take the first event A: (tA, EA)
Take the last event B: (tB, EB)
ABAB ttmEtmEt ),(),(
IMB eV 37
II-Kam eV 22
m
m
Assumptions: Instant.
emission Diff. only from
m
Schramm, CNPP 17 (1987) 239
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion & Matter Effects: Source ─ Prop. ─ Detector
Neutrino sphere
-310 cm g 10
High Matter Density:
High interaction rate
Flavors conserved
Vacuum MSW Collective
Wolfenstein, 78Mikheyev&Smirnov, 85Pantaleone, 92
Matter Effects:
Envelope
Shock wave
Earth matter
Mass ordering
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion: collective effects (accretion phase)
Duan, Fuller&Qian, 1011.2799
Fogli, Lisi, Marrone&Mirizzi, 0707.1998
Left:Sketch of
Collective
effects
Bottom:Inverted
+ Accretion
Supernova Neutrinos: Elementary Particle Physics
NH
IH
Dasgupta, Mirizzi, Tamborra&Tomàs, 1002.2943
Note: compare between accretion
and cooling results
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion: collective effects (cooling phase)
NH IH
Dighe & Smirnov, hep-ph/9907423
L – Resonance Res. for neutrinos Always adiabatic
12221 θ ,Δm H – Resonance
Res. for neutrinos (NH)
Res. for antineutrinos (IH)
13231 θ ,Δm
Adiabatic for
a ‘large’ 13
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion: MSW effects in the SN envelope
for
for
for
0eF
0eF0xF
e
e ,,,
00 )1( xee FpFpF 00 )1( xee FpFpF
000
4
1
4
1
4
2
4
1eexx F
pF
pF
ppF
Normal
Inverted
sin2(213)
≳ 10-3
Mass ordering
sin2(12)
0 cos2(12)
0
Case
A
B
Survival probabilities
)for(p e )for(p e
Dighe & Smirnov, hep-ph/9907423 Dighe, Kachelriess, Raffelt & Tomàs, hep-ph/0311172
Primary fluxes (+ collective)
Leaving the SN (+ Collective & MSW effects)
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion: MSW effects in the SN envelope
survival
02
02 )1( xeeee FPFPF
02
02 )1( xeeee FPFPF
L
E
mP
mmm
e12
122212
121212122
2 2sin4
2sinsin)22sin(2sinsin
L
E
mP
mmm
e12
122212
121212122
2 2sin4
2sinsin)22sin(2sinsin
Dighe&Smirnov, hep-ph/9907423Lunardini & Smirnov, hep-ph/0106149
NH:Matter Effects
-antineutrinos
Mass Ordering sin2 13 survival
NH
IH ≳ 10-3 cos2 12
e Earth matter e
Yescos2 12
0 No
Yes
Collective Neutrino Oscillations (accretion phase)
No Yes
IH:Matter Effects
- neutrinos
If IH is determined from oscillation experiments , Earth matter effects indicate collective effects.
Earth matter
Supernova Neutrinos: Elementary Particle Physics
Flavor Conversion: including Earth Matter Effects
for a ‘large’ 13
Extra energy-loss channels: Bound on particle physics models
50 km
Proto-Neutron Star
r rnuc = 3 1014 g cm-3
T 30 MeV
Cooling via Neutrino Emission
Exotic weakly-interacting particles
If exotic particles can be produced and escape from the SN core, then the energy carried awayby them should be at least smaller than that by neutrinos. Otherwise, the SN neutrino signal would be significantly reduced.
-1-333new scmerg1003 . E
The energy-loss argument has been applied to the SN 1987A, and restrictive bounds on particle physics models have been obtained: Axion , Majoron , keV sterile neutrino ,……
Supernova Neutrinos: Elementary Particle Physics
SN Detection: present and future experiments
Super-Kamiokande (104)KamLAND (400)
MiniBooNE(200)
LVD (400)Borexino (100)
IceCube (106)
Baksan (100)
Water / Ice
Cherenkov
Liquid
Scintillator
JUNO (104)
SN @10 kpc
Memphys
Hyper-K
DUSELLBNE
Megaton-scalewater Cherenkov
5-100 ktonliquid Argon
100 kton scale scintillator
LENAJUNOHanoHano
SN Detection: present and future experiments
Key Problem: where and When?
© Raffelt
(1) Estimate from SN statistics in other galaxies; (2) Only massive stars produce 26Al (with a half-life 7.2 105 years); (3) Historical SNe in the Milky Way; (4) No neutrino bursts observed by Baksan since June 1980
Key Problem: where and When?
SN Candidate: The Red Supergiant Betelgeuse (Alpha Orionis )
Distance: 425 ly (130 pc)
Type : Red Supergiant
Mass : ~ 18 solar masses
Expected to end its life as SN explosion
@ Super-K: 6 107 events
Detection of SN Neutrinos @JUNO
Main Channels in LSD
2015/1/10, Jiangmen, Guangdong
Goal: to pin down mass ordering
A typical SN @ 10 kpc
Neutrino Mass Bound: SN ModelKamiokande-II Data IMB Data Baksan Data
(1)Use the SN 1987A observations to extract the SN model param.
(2)Use all the information (ti Ei i )
Maximum likelihood
eeiieii
N
i
tRdttRfdEEGcEtR
BeeL di )(),,(
2
dd
1
)()(
d
Pagliaroli, Vissani, Costantini & Ianni, 0810.0466
Kam, IMB & Baksan
Every Event
Loredo & Lamb, astro-ph/0107260
Signal Events
eee dE
dEEEtE
d
dNEtR
e
)()(cos),()cos,(cos
)cos,,( ddIBD
p
Neutrino Flux Parametrization
Pagliaroli, Vissani, Costantini & Ianni, 0810.0466
)()(1)()( aca ttjtt ke
Accretion PhaseMa : initial mass
Ta : initial e+ temp.
a : accretion time
Cooling PhaseRc : -sphere
rad.Tc : initial
temp.c : cooling
time
e
Fit SN Model Parameters
s 55.0 s 7.4
MeV 4.2 MeV 6.4
22.0 km 16
58.017.0a
7.12.1c
6.04.0a
7.06.0c
sun68.015.0a
95c
TT
MMR
(1) Cooling: Thermal distr. of anti-e , and exp. decay of luminosity;
(2) Accretion: Anti-e only from e+ +n , and thermal distr. of positrons
Neutrino Mass Bound: SN Model
Neutrino Mass Bound: Events @JUNO
JUNO: 20 kt (12% p) liquid scintillator
),(ˆ)(),( IBDp EtENEtRe
)()(1)(1)(ˆaca
/ r ttjtet k
t
e
Best-fit values for SN model & r=100 ms
IBD events @JUNO: N = 4300
1. Generate n pairs of (t i , E
i) according to R (t , E)
Nn
en
NNnP
!),(
2. Denote e+ as (t i , Ee
i) corresponding to (t i , E
i)
1ttt ii ie
ie
ie EEE /03.0/
3. Label event by a relative time t i and energy Ee
i
2
2
ii
E
m
c
Dt
4. Extract SN model parameters and m from data
Pagliaroli, Rossi-Torres &Vissani 1002.3349
MeV 5.6th E
EEE /41.0023.0/
1987A SNfor CL @95% eV 8.5m
SN kpc 10 afor CL @95% eV 8.0m
@Super-K
Better ? @JUNO
Neutrino Mass Bound: Simulations
Neutrino Mass Bound @ JUNOFit for one single experiment
Jia-Shu Lu, Jun Cao, Yu-Feng Li, S.Z., 1412.7418
3000 simulations
for JUNO
3000 simulations
for Super-K
(1) Include numerical models, - systematic errors;
(2) Simulate a large number of experiments - stat. errors;
(3) Low-E, Early-t events help
Robust evidence for Dark Matter
Moore et al., 99’
Abundance of Cosmic Substructure
Cold or Warm DM ?
Sterile Neutrinos of keV Masses
Production of sterile neutrinos:Low matter density: neutrino flavor oscillations with matter
effectsHigh matter density: production & absorption via scattering processes
Occupation-number formalism:
jiij
ijij
dd
bb
Diagonal terms: just the usual occupation numbersNon-diagonal terms: encode the phase information
Equations of motion:
],[ ppp i Mass terms and matter potentials
n
i
ii
iii III
1
,2
1,
2
1pppp AP
h.c.)1(h.c.)1()2(2
13
3
aaaaaa
a
GGGGd
pppppppp
p
WW
Sterile Neutrinos in a SN Core
Two-flavor mixing case ],[ ppp i τPppp n
2
1
τBppp E2
1
ppp PBP
BpPp
z
yx
eff
22
2cos2
,0,2sin2
VE
m
E
m pB
Flavor polarization vectors rotate around magnetic fields
Matter EffectsWolfenstein, 78’; Mikheyev, Smirnov, 85’
22
2
,2
/)(2cos2sin
2sin2sin
rEE
where the resonant energy is
eff
2
2V
mEr
maximal mixing if E ~ Er cos 2θ
Sterile Neutrinos in a SN CoreWeak-damping
limit 24
2osc
keV10
2sin
10
MeV 30cm7.0~
4
sm
E
m
E
31423
Bmfp
cm g10MeV 30cm10
1
EN N
Oscillation length
Mean free path
BpPp
z
yx
Bp
z
yx
Pp
Neutrinos oscillate many times before a subsequent collision with nucleons
mfposc
Sterile Neutrinos in a SN CoreIn the weak-damping
limit τBBP ppppp ˆˆ
2
1~ n averaged over a period of oscillation
01
10
2
1
0
0~ppp
p
pp tff
f
f ss
Two independent parameters:occupation numbers fα
p & fsp
Simplified equations of motion:
a
sasaasss ffffd
gffsf )1()1()2(
)1(4
13
322
pppppppppppppp
pWWAP
further simplification if sterile neutrinos escape from the SN core
a
aas fd
gsf
pppppp
pWP
3
322
)2(4
1 set fsp = 0
Lepton-number-loss rate Energy-loss rate sf
dp
p 3
3
L2
N
ss fE
dp
p 3
3
2E
Sterile Neutrinos in a SN Core
Tau-sterile neutrino mixing
04212
BF
YYYNG
Vee
Initial conditions: Ye = 0.3, Yνe = 0.07, Yνμ
=Yντ=0
22
2
,2
/2cos2sin
2sin2sin
rEE
1. the MSW resonance occurs in the antineutrino channel;
2. asymmetry between tau neutrinos and antineutrinos.
Simple bound in the ‘vacuum limit’: Er >> E
Energy-loss rate
262
FB0
22FB2
2
2
42sin4
1
1/exp22
TGNdE
EGN
TE
EEs
E
Supernova Bound-1-333262
FB scmerg10034 .TGNs EE 82 10
Energy-loss Rate and SN Bound
*
G. Raffelt, S.Z., 1102.5124
Follow the time evolution of η and calculate the energy loss
Summary and Outlook
Neutrinos from next nearby supernova cannot be missed (a once-in-a-lifetime opportunity!)
Physics opportunities with SN neutrinos: stellar collapse, explosion mechanism, collective flavor conversion, matter effects, neutrino mass ordering, absolute neutrino mass,…
104 neutrino events @ JUNO for a typical galactic SN; to improve neutrino mass bound, & other possibilities; A lot of theoretical works to do while waiting for a real SN