taup2007 sep. 11-15, 2007 sendai, japan
DESCRIPTION
TAUP2007 Sep. 11-15, 2007 Sendai, Japan. Constraints of oscillation parameters through MSW effect of Supernova neutrinos. Shiou KAWAGOE The Graduate University for Advanced Studies (SOKENDAI) / NAOJ JSPS Research Fellow T. Kajino, - PowerPoint PPT PresentationTRANSCRIPT
TAUP2007Sep. 11-15, 2007 Sendai, Japan
Shiou KAWAGOEThe Graduate University for Advanced Studies (SOKENDAI) / NAOJ
JSPS Research Fellow
T. Kajino, The Graduate University for Advanced Studies (SOKENDAI) / NAOJ
H. Suzuki,Tokyo University of Science/NAOJ
K. Sumiyoshi,Numazu College of Technology
S. YamadaWaseda University
Outline
1 . Introduction
2. Purpose
3 . Result and Discussions ・ The adiabatic prompt explosion model ・ The observation of supernova neutrinos 4 . Summary
Gravitational Collapse
Shock wave
Supernova
Neutrino trapping
Neutrino
Introduction (1)Collapse-driven Supernova
,,,,, ee
・ All of kinds of neutrinos are generated.
・ The energy spectrum is different.
・ T < O(100) MeV → nnne
, ,,,x
xeeEEE
Introduction (2)Supernova Neutrinos
enp
epn
e
e
νe
νe
νx
Energy (MeV) F
lux
(co
un
t /
MeV
) Wilson’s model
・ The gravitational energy:
The mass squared difference The mixing angle
Inverted Normal
23
Introduction (3)Neutrino Oscillations
?
Introduction (4)The Matter (MSW) Effect
Inverted
L
H
Normal
L
H
● H-resonance :
● L-resonance :
adiabatic
non adiabatic
adiabatic
.
.
ne
m2
shock13
2 2sin
dr
dn
dr
dn
e
eIs large. and
Is small. or132 2sin Is large.
Is small.
ne
The shock wave is influenced on neutrino oscillation.
--MSW effect---
We estimate the supernova neutrino events which observed with Super-Kamiokande and SNO.
★We study how the influence of the shock wave appears in neutrino oscillations.
★Can we constrain θ 13 and the mass hierarchy?
Purpose
We succeeded in calculating propagation of shock waves
from iron core through the envelopes in single step.
D
ensi
ty
[g/c
m3]
R [cm] 1010
103
105・ Implicit lagrangian code for general relativistic spherical hydrodynamics Yamada et al. 1997•One-dimensional simulation•Adiabatic prompt explosion model•15Msolar star Woosley and Weaver,1995
The Adiabatic Prompt Explosion Model
Target number
Efficiency
Distance of supernova → 10kpc
Spectrum ( 5 < E < 60MeV)
Cross section
☆Survival Probability of neutrino
☆Neutrino spectra
☆Event number
spectra Original spectra
The Calculation of Event Number
eeFee rnG
U
E
EUdt
di
000
000
00)(2
00
00
0001
31
21
Normal hierarchy Inverted hierarchy
☆target : pure water (32,000 t )☆ enpe
☆inverted mass hierarchy → The event rates are depending on the parameters.
Event rate of Super-Kamiokande
Time [s]
213
2 102sin
413
2 102sin 5
132 102sin
313
2 102sin
Eve
nt
Rat
e [/
s]
Eve
nt
Rat
e [/
s][s
ho
ck
/ n
o s
ho
ck]
[sh
oc
k /
no
sh
ock
]
Time [s]
213
2 102sin
413
2 102sin 5
132 102sin
313
2 102sin
Normal hierarchy Inverted hierarchy
213
2 102sin
413
2 102sin 5
132 102sin
313
2 102sin
Event rate of SNO ・・・ has stopped (≧ ω≦ ) .
☆heavy water (1,000 t) ☆ eppde
213
2 102sin
413
2 102sin 5
132 102sin
313
2 102sin
☆normal mass hierarchy → The event rates are depending on the parameters.
Eve
nt
Rat
e [/
s][s
ho
ck
/ n
o s
ho
ck]
Result
☆The event rates of SK change greatly. → θ13 is large and the hierarchy is inverted.
☆The event rate of SNO change greatly. → θ13 is large and the hierarchy is normal.
☆The event rates of SK and SNO decrease simply. → θ13 is small.
Summary
☆The event rates are different depending on the value of θ13. →There is possibility that we can constrain the parameters whether θ13 is large or small.
☆θ13 is large. →The influence of the shock wave appears to the event rates. → We can suggest the mass hierarchy by the observation.
☆We will calculate other detector .
☆Improvement underway Detailed studies of the cooling effect of the proto-neutron star are underway.