RUNJOB and related topics
description
Transcript of RUNJOB and related topics
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RUNJOB and related topics
Toru ShibataINFN, Milano
(Aoyama-Gakuin University)
09/September/’04
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Contents :
1) RUNJOB performance
2) Procedure in RUNJOB data analysis2) Procedure in RUNJOB data analysis
=> Astrop. Phys. 16 (2001) 13, Apanasenko A.V. et. al.
3) RUNJOB results and comparison with other data
4) Theoretical implication of the experimental data
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RUssia-Nippon JOint Balloon experiment
M.Furukawa, V.I. Galkin, M. Hareyama, Y. Hirakawa, M. Ichimura,N. Inoue, E. Kamioka, T. Kobayashi, V.V. Kopenkin, S. Kuramata,
A.K. Managadze, H. Matsutani, N.P. Misnikova, R.A. Mukhamedshin,S. Nagasawa, R. Nakano, M. Namiki, M. Nakazawa, H. Nanjo,
S.N. Nazarov, S. Ohata,H. Ohtomo, D.S. Oshuev, P.A. Publichenko, I.V. Rakobolskaya,T.M. Roganova, C. Saito, G.P. Sazhina, H. Semba,
T. Shibata, D. Shuto, H. Sugimoto, R. Suzuki, L.G. Sveshnikova, R.Tanaka, V.M. Taran,N. Yajima, T. Yamagami, I.V. Yashin,
E.A. Zamchalova, G.T. Zatsepin, I.S. Zayarnaya
Faculty of Engineering, Aomori University, Aomori 030-0943, JapanDepartment of Physics, Aoyama Gakuin University, Tokyo 157-8572, JapanFaculty of Science and Technology, Hirosaki University, Hirosaki 036-8561, JapanSchool of Medicine, Hirosaki University, Hirosaki 036-8562, JapanP.N.Lebedev Physical Institute of Russian Academy of Sciences, Moscow 117924, RussiaPhysical Department of Moscow State University, Moscow 119899, RussiaD.V.Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119899, RussiaInstitute for Nuclear Researches of Russian Academy of Sciences, Moscow 117312, RussiaMultimedia Information Research Division, National Institute of Informatics The Ministry of Education, Tokyo 101-8430, JapanShonan Institute of Technology, Fujisawa 251-8511, JapanDepartment of Management, Urawa University, Urawa 337-0974, Japan
RUNJOBRUNJOB
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constructionearly May(ISAS, ICRR)
launchingmid. July
level flight at 32kmexp. time ~ 150hrs
recovery
dismountingearly August
process.mid. Aug.
Performance of RUNJOB experiments
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Balloon Trajectory
launchinglanding
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Balloon Altitude
RUNJOB1,2RUNJOB3,4RUNJOB8,9RUNJOB10,11
Average altitude ~ 32km ~ 10g/cm2
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RUNJOB detector
diffuser ( ~4cm)
target ( ~10cm)
thin EC( ~5c.u.)
spacer ( ~20cm)
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Procedure in RUNJOB data analysis:Procedure in RUNJOB data analysis:
1) Energy determination1) Energy determination
2) Charge determination2) Charge determination
3) Detection efficiency calculation3) Detection efficiency calculation
RUNJOB results and comparison with other data:
1) Light elements (p, He)
2) Heavy elements (CNO, NeMgSi, Fe)
3) 2-ry/1-ry ratio (B/C, sub-Fe/Fe)
4) All-particle spectrum and average mass
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( Moscow04)
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ATIC
10-3
10-2
10-1
100
101
102
103
101 102 103 104 105
SOKOLJACEE
CRNSANRIKURUNJOB
E2.
5 dI/
dE [
m-2se
c-1sr
-1(G
eV/n
)1.5 ]
00
kinetic energy E [GeV/nucleon]0
CNO-group
×( 1/10)
NeMgSi-group
×( 1/100)
Iron-group
JACEE SOKOL&≧: Z 17
HEAO-3
(Moscow04)
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(summarized by V. Zatsepin)
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Summary on RUNJOB data (1)
・ 95% of all data was analyzed.・ The spectra cover the energy range 10 -1000 TeV for proton 5 - 100 TeV/n for helium 1 - 70 TeV/n for CNO 1 - 20 TeV/n for NeMgSi 0.5 - 8 TeV/n for iron・ Proton spectrum doesn’t’ show any tendency of steeping in observed energy range.・ Helium flux is lower (about half) than JACEE , SOKOL ATIC, but consistent with MUBEE and Grigorov data.・ Proton and helium spectra are nearly parallel
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・ CNO spectrum has no indication of enhancement in > 10TeV/n region.・ Iron spectrum is consistent with other groups within statistical error ・ 2-ry/1-ry ratio was shown in TeV/n region.・ All particle spectrum and average mass covers the energy range from 30 to 1000TeV/particle.・ All particle flux is lower than other direct measurement, but seems to be consistent with ATIC (Moscow04)・ The Spectrum shape is similar to other direct measurement => flattering before knee ?・ Average mass is nearly constant in our observation region, 30-1000 TeV with <ln A> ~1.5 (helium)
Summary on RUNJOB data (2)
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Procedure in RUNJOB data analysis:Procedure in RUNJOB data analysis:
1) Energy determination1) Energy determination2) Charge determination2) Charge determination3) Detection efficiency calculation3) Detection efficiency calculation
RUNJOB results and comparison with other data:RUNJOB results and comparison with other data:1) Light elements (p, He)1) Light elements (p, He)2) Heavy elements (CNO, NeMgSi, Fe)2) Heavy elements (CNO, NeMgSi, Fe)3) 2-ry/1-ry ratio (B/C, sub-Fe/Fe)3) 2-ry/1-ry ratio (B/C, sub-Fe/Fe)4) All-particle spectrum and average mass4) All-particle spectrum and average mass
Theoretical implication of the experimental data:0) Motivation1) Model of CR propagation 2) 2-ry/1-ry ratio, isotope, diffusiveγ-ray, anti-p, ……
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Present status of C.R. direct obs. in GeV-PeV region
observables: physics: ◎1-ry nuclei (p, He, ….., Fe) : accel. limit, source spectrum ◎2-ry nuclei (LiBeB, sub-Fe) : path length, residence time - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
◎ultra-heavy nuclei : r-process, s-process ◎anti-particle (p, e+, ……) : novel source, path length ◎isotopes (Be10, Al26, Cl36, …) : life time of C.R., gas density ◎electrons : nearby source, anisotropy ◎diffusive γ-rays : gas density, novel source
in harmony with each other ? if not, novel source ?
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Configuration of our Galaxy
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Our model
● gas density : )/||(exp)( nn zzrr0
/nrn
with
● CR source density : )/||/(exp)();(QQ
zzrrRR0
QQ r
RR00
QQ )(
● boundaryless Galaxy :
,r,(N |z|→∞ 0);R 0);Rz,(N →∞r
with
● diff. coefficient : )/||(exp)();(DD0
zzrrRR /D rD
vR00
DD )( αR
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Important parameters:
● 2.2 2.4~ γ
●
=
0
2
1
1
:
:
: ≪
≫
ν
nz
nz
nzDz
Dz
Dz
nzzD
1
1
γR Q:
●
: Kraichnan - type
: Kolmogorov- type
2
1
3
1 ααRD
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Practically, we presume
zD ≫ zn
(thin gas disk surrounded by a large diffusion space)
~ zn / zD ( ~
0.1)ν = 1 [1 + zD zn]
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× : source r0 (r0 , z0 )→: solar system ~ ~
→r (r 10kpc, z 0)
×
Φ ( r, E; r0 , E
0 ) : structure function
(r0 , E
0 )
→
(r, E )→
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0) structure function:
1) primary component:
2) secondary component
<= ApJ, Vol. 612 (Sep. , 2004), Shibata et. al.
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5 ) Energy distribution in TeV (ground-base)
Comparison with experimental data :
2 ) Longitudinal distribution (EGRET & COS-B)
3 ) Latitudinal distribution (EGRET)
4 ) Energy distribution in GeV region (EGRET)
0 ) Cosmic-ray data on 1-ry, and 2-ry/1-ry ratio
1 ) Cosmic-ray data on 10Be / 9Be ratio
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filled symbol: RUNJOB
cross symbol: ATIC
10-3
10-2
10-1
100
101
102
103
104
10-2 100 102 104 106
kinetic energy E0 [GeV/particle]
proton
helium(× 1/10)
CNO(× 1/100)
Ne-Si(× 1/1000)
iron(× 1/10000)
γ :
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
α = 1/3
filled symbol: RUNJOB
cross symbol: ATIC
10-3
10-2
10-1
100
101
102
103
104
10-2 100 102 104 106
kinetic energy E0 [GeV/particle]
proton
helium(× 1/10)
CNO(× 1/100)
Ne-Si(× 1/1000)
iron(× 1/10000)
γ :
2.2
2.3
2.4
2.2
2.3
2.42.2
2.3
2.4
2.2
2.3
2.4
2.2
2.3
2.4
α = 1/2
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10-3
10-2
10-1
100
10-1 100 101 102 103 104
JuliussonChappel & WebberSimon et al.Orth et al.HEAO-3Lezniak & WebberCaldwell & MeyerDwyerMaehl et al.ACEUlyssesVoyagerGarcia-Munoz et al.
kinetic energy; E0 (GeV/nucleon)
● : RUNJOB [Li+Be+B]/[C+N+O]
ν :0.40
0.20
0.10
0.05
σ = 12.23 mb○●
(a) α = 1/3
10-3
10-2
10-1
100
10-1 100 101 102 103 104
JuliussonChappel & WebberSimon et al.Orth et al.HEAO-3Lezniak & WebberCaldwell & MeyerDwyerMaehl et al.ACEUlyssesVoyagerGarcia-Munoz et al.
kinetic energy; E0 (GeV/nucleon)
● : RUNJOB [Li+Be+B]/[C+N+O]
σ = 6.11 mb○●
ν :0.40
0.20
0.10
0.05(b) α = 1/2
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10-3
10-2
10-1
10-1 100 101 102 103 104
RUNJOBSANRIKU opening-angle methodSANRIKU E-W asymmetry methodHEAO-3(1990)HEAO-3(1988)ACE
kinetic energy; E0 (GeV/nucleon)
ν :
0.40
0.20
0.10
0.05
(a) α = 1/3
σ = 12.23 mb○●
10-3
10-2
10-1
10-1 100 101 102 103 104
RUNJOBSANRIKU opening-angle methodSANRIKU E-W asymmetry methodHEAO-3(1990)HEAO-3(1988)ACE
kinetic energy; E0 (GeV/nucleon)
ν :
0.40
0.20
0.10
0.05
(b) α = 1/2
σ = 6.11 mb○●
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● 0σ = 2
D0
0
czn
D
0σ = mb34.9 )(
ppσ
:x,x average path length)(
for
0D = 2810 seccm2 at R GV1=
=
= kpc1
0n 3cm1
Dz
: gas density at Galactic center
: scale height of diffusion coeffi.
1-
00 σ
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η η/0 0 0
= 0.5
= 1.0= 1.0
ν: 0.2: 0.1: 0.0
α = 1/3σ /0 σ 00 = 2
ISOMAX (2001)ACE (1999)Ulysses (1998)Voyage (1994)IMP7/8 (2001)ISEE-3 (1980)
kinetic energy E (GeV/n)
Be
B
e R
ati
o1
09 /
0
.1
.2
.3
.4
.5
.6
10 10 10 10-2 -1 0 1 210
0
(preliminary)
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● 0η =
0η = 3.73 η
0D
610 1.6
00
τ
Dz
for
0D = 2810 seccm2 at R GV1=
=
= kpc1 Dz
: life time of 10Be
: scale height of diffusion coeffi.
y
0
τ0
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5 ) Energy distribution in TeV (ground-base)
Comparison with experimental data :
2 ) Longitudinal distribution (EGRET & COS-B)
3 ) Latitudinal distribution (EGRET)
4 ) Energy distribution in GeV region (EGRET)
00 )) Cosmic-ray data on 1-ry, and 2-ry/1-ry ratioCosmic-ray data on 1-ry, and 2-ry/1-ry ratio
11 ) ) Cosmic-ray data on Cosmic-ray data on 1010BeBe // 99Be ratioBe ratio
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3)γ-ray component
2Lπ4
dVσvn )(r
z
x
y0
l
Earth
line of sight
L
b
γγp)(rpN
ApJ, vol. 612 (‘04, sep.)
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1 10 100 1000
(Galactic center)
(Solar system)
r (kpc) 0
5
10
15
20
.5
.2
kinetic energy E0(GeV/nucleon)
I p(r
; E
0)/I
p(0
; E
0)
.1
1
.05
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③ 400 ~ 2000 GeV : Neuhofer et al. (1972)
① E0 ~ 1 GeV : Bugg et al. (1964) ② 10 ~ 300 GeV : Jaeger et al. (1975)
④ 30 ~ 700 TeV : Chacaltaya (1980) , (UA7)
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(in CMS)
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*η = ln tan- /2θγ*
0 2 4 6 8-2-4-6-8
η*
dσ d/
(
)
ppσ
1 /(
)
.
(1 N
0 )
/
.
0
2
4
6
1
3
5= 0
1
10
100
τ ≡ T / p0 0 0 <= isotropic dist. in CMS
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(mb
)N γσ
pppp→γ
σ∫
∞
0(E
0,E
)dE
γ
γ=
-
○ : experimental data (compiled by Dermer)
kinetic energy of proton; E0 (GeV)
100 101 102 106
104
102
101
100
103 104 105
103●: our empirical curve
● : expected from pseudo-rapidity density by UA5, UA7, and Chacaltaya experiments
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: = 0.5
: τ = 0.00
dEγ
σ d/
(
)pp
σ1 /(
)
.
[]
GeV
-1 100
10-1
10-2
0.2 0.4 0.6 0.80
E (GeV)γγ -ray energy in LS ;
1
pT :
200 MeV
150
100
E0 = 0.97 GeV
(Bugg et al. 1964)
-
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: τ = 1.60
= 2.2:
with pT = 143 MeV-
●
:::
:
1.753610
°°
°°
θγ
16
27
:
:
°°
○
△
▲
□
■
E0 = 23.1 GeV
d2 σ
dEγ
Ωd[
]m
b sr
-1G
eV-1
103
0 4 8 12 1610
-1
E (GeV)γγ -ray energy in LS ;
102
101
100
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: τ = 5.00
= 7.0:
with pT = 151 MeV-
: τ = 0.20
= 0.5:
/dσ d
(mb
)x F
||
10-1
100
101
102
103
104
xF| | √γ2p L /* s| |=
0 .1 .2 .3 .4 0 .1 .2 .3 .4 .5
~~
a) 11.5 GeV b) 204.1 GeV
with pT = 133 MeV-
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b) 44.7GeV
10-4
10-3
10-2
10-1
100
101
0 1 2 3 4 0 1 2 3 4 5 0 1 2 3 4 5 6
~~ ~~
d2 σ
dEγ
Ωd*
*[
]sr
-1G
eV-1
σpp1
γ -ray energy in CMS ; E (GeV)γ*
c) 52.7GeVa) 30.2GeV
θγ*
: 10°: 16°: 24°: 90°
○
△
▽
□
: τ = 50
= 8:with pT = 142 MeV
: τ = 70
= 10:with pT = 140 MeV
: τ = 90
= 12:with pT = 144 MeV- - -
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0
= 5.0:: τ = 3.0: τ = 4.00
: = 6.0
: τ = 0.80
= 1.2:
b) E0 = 204.1GeVa) E0 = 11.5GeV
/dσd
(mb
)η
** /
dσd
(mb
)η
** /d
σ d(m
b)
η*
10-1
100
101
102
0-2-4 2 0-24 2 0-24 2 4
*η = ln tan- /2θγ*
~~ ~~
c) E0 = 299.1GeV
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Σ Eγ = 20 - 50 TeV Σ Eγ = 50 - 200 TeV
10-1
100
101
102
d f
σ d/
(
)pp
σ1/
(
)
.
γ
γfractional energy of - rays;
0 .2 .4 .6 .8 0 .2 .4 .6 .8 1
~~
Eγ Σ Eγ/f = γ
: τ = 40.00
= 70.0:
: τ = 80.00
= 120.0:
with pT = 166 MeV- with pT = 176 MeV-
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only relative value is compared !
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only relative value is compared !
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filled symbol: RUNJOB
cross symbol: ATIC
10-3
10-2
10-1
100
101
102
103
104
10-2 100 102 104 106
kinetic energy E0 [GeV/particle]
proton
helium(× 1/10)
CNO(× 1/100)
Ne-Si(× 1/1000)
iron(× 1/10000)
γ :
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
2.3
2.4
2.5
α = 1/3
filled symbol: RUNJOB
cross symbol: ATIC
10-3
10-2
10-1
100
101
102
103
104
10-2 100 102 104 106
kinetic energy E0 [GeV/particle]
proton
helium(× 1/10)
CNO(× 1/100)
Ne-Si(× 1/1000)
iron(× 1/10000)
γ :
2.2
2.3
2.4
2.2
2.3
2.42.2
2.3
2.4
2.2
2.3
2.4
2.2
2.3
2.4
α = 1/2
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20 < l < 55° °-2 < b < 2°°
↓↓↓
↓↓
↓
E2
γdN
/dE γ
[]
cm-2
s-1sr
-1 M
eV
γ-rayenergy; E (GeV)γ
10 0
10-1
10-2
10-3
10-4
10-5
10-6
100 101 102 103 104 105 106
Inner GalaxyEGRET
W
H T
T THA
γ = 2.3
2.4
2.5
cutoff energy
1 PeV ∞
α = 1/3
■ : Berezinskii et al.
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Outer Galaxy
140 < l < 225° °-2 < b < 2°°
↓T
↓T
↓T
↓↓↓
↓
E2
γdN
/dE γ
[]
cm-2
s-1sr
-1 M
eV
γ-rayenergy; E (GeV)γ
EGRET
10 0
10-1
10-2
10-3
10-4
10-5
10-6
100 101 102 103 104 105 106
CA
γ = 2.3
2.4
2.5
cutoff energy
1 PeV ∞
α = 1/3
■ : Berezinskii et al.
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● EGRET data are not in harmony with C.R. data :
1) Energy calibration ?
2) Subtraction of SNR ?
3) Novel sources ?
Conclusion
● 100 GeV ~ 100 TeV-γ are quite important
3) I.C. or Brems. Photons effective ?
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