Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic

Masatoshi Koshiba Raymond Davis Jr.

The Nobel Prize in Physics 2002The Nobel Prize in Physics 2002

"for pioneering contributions to astrophysics, in particular for the detection of cosmic neutrinos"

S. P. MikheyevINR RAS Moscow

S.P.Mikheyev INR MoscoS.P.Mikheyev INR Moscow w

Erice 7 July 2004Erice 7 July 2004 33

e

p

pp

p

e

e+ e+

n n

4He



1964 - Original Motivation

“… to see into the interior of star and thus verify directly the hypothesis of nuclear energy generation in star.”

4p 4He + 2e+ + 2e + 26.73 MeV

4R2 = 71010 sec-1cm-22 Lsun

26.73 MeV

1



Ј 15.0 MeV

B ЮBe* + e+ + e

pp – chain

p + p ЮH + e+ + e

p + e- + p ЮH + e

H + p ЮHe +

He + He Ю He+ 2p He + He ЮBe + He + p ЮHe + e+ + e

Be + e- ЮLi+ e

Be + p ЮB+

Li+ p Ю2 Be* Ю2

Ј 0.420 MeV

1.442 MeV

Ј 18.77 MeV

MeV, MeV

99.6%0.4%

0.002%

99.87% 0.13%

15%85%



CNO – chainC + p ЮN +

N ЮC + e+ + e

Ј 1.199 MeV

C + p ЮN +

N + p ЮO + O ЮN + e+ + e

Ј 1.732 MeV

N + p ЮC +

N + p ЮO +

O + p ЮF + F ЮO + e+ + e

Ј 1.740 MeV

O + p ЮN +

99.9%

0.1%



Bahcall & PinsonneaultPRL (2004)

Neutrino Energy (MeV)

Neu

trin

o F

lux

(cm

-2 с

s-1 M

eV-1)

Standard Solar Model (SSM)



e

e-

nn

p

np

ppp

nn

p

nn

p

np

ppp

n

Charge Current Reaction

+ ZA e- + Z+1A

ZA Z+1A

pn

e-

W+

2H 37Cl71Ga7Li

115In



e-

Neutrino Electron Scattering

+ e- + e- e-

W+

e-

e-

Z0

e-

ee,,NC CC/6



nn

p

np

ppp

nn

ZA

Neutral Current Reaction

+ N + N*

ZA ZA*

N

Z0

N*

e,,



+ 37Cl e- + 37Ar (B. Pontecorvo 1946)


Neu

trin

o F

lux

(cm

-2 с

s-1 M

eV-1)

7Be

8B

Threshold 0.814 МэВ



Davis’s experiment

C2Cl4



+ 37Cl e- + 37Ar


Neu

trin

o F

lux

(cm

-2 с

s-1 M

eV-1) Threshold 0.814 МэВ

Rexp

RSSM

= 0.335 0.029

Rexp = 2.56 0.23 SNU



RSSM = 7.6 + 1.3 SNURSSM = 7.6

– 1.1

+ 71Ga e- + 71Ge


Neu

trin

o F

lux

(cm

-2 с

s-1 M




SAGE experiment (Baksan)

GALLEX/GNO experiment

(Gran Sasso)



RSSM = 7.6 + 1.3 SNURSSM = 7.6

– 1.1

+ 71Ga e- + 71Ge


Neu

trin

o F

lux

(cm

-2 с

s-1 M


RSSM = 128 + 9 SNURSSM = 128 – 7

Rexp

RSSM

= 0.584 0.039



e

e + e- e + e-



４０ｍ

４１

．４

ｍ

Kamiokande/Super-Kamiokande



22385 solar events

(14.5 events/day)

e + e- e + e-



The Sun by Neutrinograph

e + e- e + e-



DataSSM

= 0.465+0.016-0.015 0.005

e + e- e + e-





1000 tones D2O

Support Structure for 9500 PMTs, 60% coverage

12 m Diameter Acrylic Vessel

1700 tonnes InnerShielding H2O

5300 tonnes Outer Shield H2O

Sudbury Neutrino

Observatory



e + d p + p + e- CC

x + e- x + e- ES

x + d x + p + n NC

FCC = 1.59+0.08(stat)+0.06(syst)-0.08-0.07

FEC = 2.21+0.31(stat) 0.10(syst)-0.26

FNC = 5.21 0.27(stat) 0.38(syst)

Detector SNODirection

Kinetic Energy

Position



Detector SNO



Bahcall, Gonzalez-Garcia, Bahcall, Gonzalez-Garcia, Pena-Garay, PRL2003Pena-Garay, PRL2003

1. Energy production in Sun: pp chain is the dominant mechanism LCNO < 7.6% (3)

2. Neutrino fluxes in pp cycle :

BP04fi =

fit

fpp = 1.02 0.02 (1)

fB = 0.88 0.04 (1)

fBe = 0.91 0.25/0.62 (1) Bahcall, Pena-Garay, JHEP2003Bahcall, Pena-Garay, JHEP2003



p + e- n + e

n + e+ p + e

x

N + N N + N + x + x

e- + e+ x + x

e + e x + x

x

x

Neutronization burst:

e emitted during 10 ms

Cooling through neutrino emission:

e, e, , , , .99% of the SN energy emitted in neutrinos during 10 s



Neutrino energies

MeVE

MeVE

MeVE

e

e

)2520(

10

12

~,,~,

~



2 44 2~ 9.3 10e p e

E см

0.5eE МэВ

e + p e+ + n

Neutrino burst

Relic SN neutrinos



Neutrino burst search





23 February 7:36 UT



Confirmed the neutrino mechanism of Supernova cooling

• Obtained constrains on some Supernova parameters

• Obtained constrains on some neutrino properties (masses, charge, etc)



23 February at 2:52 UT

LSD Detected 5 Events in 7 second

1

10

100

10 100Time window (sec)

Nu

mb

er

of

bu

rsts

5 10 15

23 February 1 day

LSD DATA



February 23, 1987

Optical

Geograv

LSD

KII

IMB

BUST

1 3 5 7

2:52:35,4

2:52:34

2:52:34

7:36:00

7:35:35

7:35:41

7:36:06

44

43,8 19

47

:47

21

5

2(4)

1 6

2

12

8

v m =6vm =12 m

observations

2:52:36,8

m

9 11

February 23, 1987

1 3 5 7 9 11

mv=6mmv=12m

Geograv

LSD

KII

IMB

BUST

2:52:35,42:52:36,8

43,82:52:3

444

2:52:34

7:36:00

7:35:35

7:35:41

7:36:06

19474721

2

12

8

6

5

2

1

(4)

Chronology

Courtesy to O. Ryazhskaya



The Two-Staged gravitational collapse Model[Imshennik V.S., Space Sci Rev, 74, 325-334 (1995)]

12 MM

12

222 , JM

111, JM

e

ahead

aside

~,




Tc~5x1012

KTc~5x1010

K

The difference of neutrino yield between standard model and model of rotating

collapsar.

MeVE

MeVE

MeVE

e

e

)2520(

10

12

~,,~,

~

The main reaction – URCA-process:

MeVE

nep e

)5030(

e e

e~

~

~

e

e

e

e

e

314106.2~ smg

erg53~, 103.5 erg

eee

52~, 109.8




V.S.Imshennik, O.G.Ryazhskaya astro-ph/0401613



Liquid Scintillator Detector (LSD)

General view of LSD

Fe (2 sm)

Fe (10 sm)

H=5200 m.w.e. 72 counters 90 tons of СnH2n (n~9), 200 tons of Fe

4.5 m

8m

6 m




СnH2n

CoeFe e5656

СnH2n

CoeFe e5656

СnH2n

CoeFe e5656

МэВE 72.1

EEE oe

МэВE 82.1 МэВE 72.1

МэВE 4

МэВE 82.1

МэВE 7

e

МэВE 82.1EEE oe EEE oe

e

e




Energy spectrum of the particles, coming from iron plate of thickness 2,8 sm (Geant4 calculations; histogram – total energy deposit)

0 5 10 15 20 25 30 35 40Энергия, МэВ

106

105

104

103

102

10

1

Events

Energy range, registered by LSD

Courtesy to O. Ryazhskaya & V. Boyarkin



Many experiments stand Many experiments stand ready to observe the ready to observe the neutrinos of the next neutrinos of the next galactic supernova.galactic supernova.

• Baksan• MiniBooNE detector• LVD• AMANDA• KamLand• SNO• Super-Kamiokande

More detectors sensitive More detectors sensitive to SN neutrino are to SN neutrino are

planned or being built.planned or being built.

• Borexino• ICARUS• IceCube• HyperKamiokande• UNOand many others



In universe there is one supernova

explosion per second

There exist the flux of relic supernova There exist the flux of relic supernova neutrinos.neutrinos.



Super-Kamiokande published the Super-Kamiokande published the world’s best limits on relic world’s best limits on relic

supernova neutrinosupernova neutrino [M.Malek [M.Malek et al., Phys. Rev. Lett.et al., Phys. Rev. Lett.

9090 061101 (2003)]. 061101 (2003)].

1.3 cm-2s-1



GADZOOKS

adoliniumntineutrinoetectorealouslyutperformingldamiokande,uper !





Detection of relic supernova neutrinos will:

No detection of relic supernova neutrinos also is very interesting.

verify the basic picture of star formation and death;

constrain star formation history

Documents

Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic