井岡 邦仁 (KEK)
共同研究者: 川中宣太 (KEK)
Adriani+ 08
Positron excess above the predicted secondary
ExpectedSecondary
PositronExcess
⇒ Primary sources - Dark matter? - Astrophysical?
⇒ Many papers >400
Jul 06 - Feb 08151672 e-, 9430 e+
Solar modulation
An Excess also in (e++e-) Spectrum
Abdo+ 09
ATIC/PPB-BETSPeak+Cutoff~600GeV DM?
FermiSmooth E-3
No peakAug 08 – Jan 094M e-
Aharonian+ 09
◉Consistent with Fermi◉No ATIC peak(but not rule out)◉Steep at >1TeV
Primary sources
有効面積大5×104 m2 @1TeV~8.5×107 m2 sr s (2004-2007)
視野・台数増 ⇒ 有効面積大 ⇒ より高エネルギー
計画 帯域(GeV)
E/E e/pExposure(m2 sr s)
CTA2013~
10~15,000
?? ~103-4?~109
(1 yr)
AMS-022010~
1~1,000~2.5%@100 GeV
~104
(×102 by TRD)
3×106
(1 yr)
CALET2013~
1~10,000~2%
(>100 GeV)
~105 4×106
(1 yr)
注 : シミュレーションで proton background の評価⇒ E~15% 不定性 ⇒ w/ LHCf ?
(proton)~1eV/cm3
~ 超新星残骸
(electron)~10-2eV/cm3
(positron)~10-3eV/cm3
~ 0.1% of p起源が不明ガンマ線、電波0903.1987
-2.7
ee±± cooling coolingWe are here
Positron sourced<~1kpc
Our galaxy
e± lose energy (cool) via inverse Compton and synchroton
€
cut ~1
bt, b =
4σ Tc
3 mc 2( )
2
B2
8π+Uγ
⎛
⎝ ⎜
⎞
⎠ ⎟
Annihilation Decay
DM
DM
e
e
e
DM
Q ~ n2
Ecut ~ mDM
<v>~3x10-24cm3/s >3x10-26cm3/s boost factor ~100
Q ~ nEcut ~ mDM/2decay~1026sec (>H-1)
郡さんのトーク
Shen 70; Aharonian+ 95; Atoyan et al. 95; Chi+ 96; Zhang & Cheng 01; Grimani 07; Yuksel+ 08;Buesching+ 08; Hooper+ 08; Profumo 08; Malyshev+ 09; Grasso+ 09Kawanaka, KI & Nojiri 09;
Shen & Berkey 68; Pohl & Esposito 98; Kobayashi+ 04; Shaviv+ 09; Hu+ 09; Fujita+KI 09; Blasi 09; Blasi & Serpico 09; Mertsch & Sarkar 09;Biermann+ 09
PropagationDelahaye+ 08; Cowsik & Burch 09
Heinz & Sunyaev 02
KI 08GRB
SNR Pulsar
10-3 x 1050erg/SN~ (1sec pulsar)/SN~ 1050erg/103SN
Cosmic-ray Nuclei energy
Proton Comtami.Fazely+ 09; Schubnell 09
QSO
e
ee d
dE
e
2e
Power-law Spectrum
B
Burst-like injection
€
f =q0εe
−α
π 3 2ddiff3
1−btεe( )α −2e− d d diff( )
2
ddiff t,εe( ) ~ 2 K εe( )t[ ]1 2
€
b ~ 10−16GeV-1s−1
K εe( ) ~ 5.8 ×1028cm2s−1 1+εe
4GeV
⎛
⎝ ⎜
⎞
⎠ ⎟
1 3
€
∂∂tf t,εe,x( ) =K εe( )∇ 2 f +
∂
∂εebεe
2 f[ ] + q t,εe,x( )
For a single burst with
Atoyan+ 95, Shen 70
eq
€
cut ~1
bt
Power law spectrum
DiffusionEnergy loss byIC & synchro.
Injection
← B/C ratio
d=1kpc
(a)0.9d50 erg2d5 yr=2.5(b) Harder0.8d50 erg5.6d5 yr=1.8(c) Older3d50 erg3d6 yr=1.8
We can fit the PAMELA data well
KI 08
ATIC/PPB-BETS & Fermi/HESSd=1kpc
(a)0.9d50 erg2d5 yr=2.5(b) Harder0.8d50 erg5.6d5 yr=1.8(c) Older3d50 erg3d6 yr=1.8KI 08
Due to cooling
€
tcool ∝εe−1
Independentof initial max
ATIC peakHESS cutoff
KI 08
200
spindown0/1
)( t
ELtQ tot
000
4ln exp
4ln )(
tE
tQ tot
2
2
0
2
32/30 exp1
)(),(
diff
t
ediff
ee r
rtb
r
tQtdtF
0
Case 1: pulsar-type decay
Case 2: exponential decay
0
Cutoff width cut
t~105yre-t decay
t~105yrt-2 decay
t~104yrt-2 decayKawanaka+ 09
Cutoff width
CTA
Kobayashi+ 04
CTA
現在見えているとは限らない。 t<104-5yr
分散
CTA
tcool~105yr @TeVtSN~105yr @<kpc
Kawanaka+ 09
A single source A relatively large anisotropy⇒
max
minmax
minmax
~@ 2
3~
3
ect
d
cf
fK
II
II
KI 08; Mao & Shen 72
ChallengingDM clump
Fermi~6×106 erg sr sCTA~109 erg sr s
Fujita, Kohri, Yamazaki, KI 09Blasi+ 09Anti-proton
fraction
SNR model:pp → → e+,e-
(w/ ISM/DC)
Inevitably ⇒ anti-proton
excess above~100 GeV
⇒ AMS-02
Colin+ 09
e-, e+, , anti-pMoon shadowの位置が異なる⇒ 分離可能
CTA: 150GeV~3TeVdetection<5hr
月の散乱光がbackground
Mertsch and Sarkar 09
Hadronic models Secondary Nuclei Excesses⇒
Titanium-to-iron ratio Boron-to-carbon ratio
Z=22 Z=5
Z~7-40 with Z/Z~5% for 10~1000TeV
Fe
CTA
PHYS-WP-heavy nuclei
balloon/space shower
Source #~100
1-10TeV e ⇒ IC ⇒ ~TeV
観測から電子ソースE>1048erg~0.5 Crab@2kpc
Fmin( 電子ソース )@ 20kpc
N R∝ 2 F∝ -1
閉じ込め~105yr
点源(カロリメトリック)⇔ 柴田さん: diffuse
N R∝ 2 F∝ -1
閉じ込め~10 4 yr
閉じ込め中エネルギーが大きい場合
Diffusioncoefficientなどにもよる
~PSR J1826-1334
電子・陽電子宇宙線の起源 Astrophysical? Dark Matter?
直接観測は今後進展有効面積: CTA >> AMS-02, CALET⇒ >TeV: Discreteness, Injection History 非等方性 : Single or Multiple pbar, Heavy: Hadronic or Leptonic
TeV電子ソース ⇒ TeVガンマ線ソース 閉じ込め時間は短い ? or DM? サーベイ、広がったソース
PHYS-WP 計 23人
Dark Matter / Fund. Physics
6
EBL / Cosmology 6
AGNs 9
CR / Clusters / Starbursts 8
MQ / Binaries 3
CR / SNRs / Mol. Clouds 11
PWNe 3
Pulsars / Glob. Clusters 3
MW / Transients / GRBs 7
Surveys / Sub-arrays 1
Extended / Diffuse Srcs. 4
Intensity Interferometry 0
DC Light / CR composition 1
◉ まずは、論文を書くときCTAについて議論◉ CTA-Japanは後発◉ 長期的には組織的に力を合わせたほうがいい◉ アイデアが必要- 論文を全員に回覧- CTA-Japan Paperを重要なものに関しては書くTask A, Bの日本版- …