相対論的磁気流体流中の星によって作られる衝撃波構造
Shuta Tanaka (Aoyama Gakuin U.)
on behalf ofTMT revolution
Tanaka, Matsumoto, Toma & Shoda
19, Oct. 2021, 高エネルギー現象で探る宇宙の多様性I @ ICRR/zoom

1Introduction
2

Relativistic JetCyg A (Chandra, HST, SDSS, VLA)

• Powered by NS or BH• Relativistic plasma outflow• High-energy (non-thermal) emission• Bipolar jets from engine

Jet

Common astrophysical phenomena phenomena in AGN, microquasar & GRBDisc• Gravitational energy (inflow -> outflow)
Same as pulsar wind
• Rotation powered?
• Role of magnetic field?

JetDisc• How to accelerates to relativistic flow?
• How to collimate jets?

3TTT18

hrµ (nuµ )i = 0, Tanaka&Toma20⇤radhrµ T µt i =,cb2 /2 ⇤radµ⌫hu⌫ rµ TFL i =,⌧disscb̄2 /2
1µ⌫↵,hb̄µ er⌫ F↵ i =2⌧convb̄2 /2
1b2 /2µ⌫↵h bµ er⌫ F↵ i =.
2
⌧conv ⌧diss

Turbulence Acceleration
Asada+17
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104103u<latexit sha1_base64="+JVXKEpRxyKQFVS5K/edvi2XuAQ=">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</latexit>

102101100102σ10110010-110B-2100u0<latexit sha1_base64="PEUYO+KoHvoHMNJrkFBwUEJ3AMI=">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</latexit>

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10-1

Tanaka&Toma20

10-210010110210310410510610710841091010Turbulence Formation?

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Cruz-Osorio+17

Matsumoto&Masada19

Khangulyan+13
Porth&Komissarov15

5

yranilimNumerical StudyerP

6

Set Up – 2D Rela. MHD
デカルト座標乱流加速の計算設定
43⇢jet = 1=

松本仁くんのスライド

free condition
Nx=Nz=400

jet = 1
jet = 0.4

Pjet
=⇢jet
2

jet jet=1

1 jet jet>0⇢clump = 1010 ⇢jet
Pclump = Pjet

clumpbx =vclump = 0s2Pjetjet⇠ 2.236

jet jet < 0.5

periodic

periodiczx

relativistic flow
jet = 3

vjet /c = 0.9428

7

Set Up – 2D Rela. MHD
松本仁くんのスライド一つにして詳しく調べる
8

Blob → Poleρ

parallel

次元性の効果?

BB

↑

↑

BB

B
B→→

⊗⊗

BB→

⊗• 磁場
• 速度場
• Poleの向き

undular

衝撃波面の発展interchange

9Hydrodynamic limit
ρvx

σ = 10-6, β = 102, Γ = 2
1

10-2-10-2

1contactP10

B-field Direction
ΦB = π/2ΦB = 0PP

σ = 10-1, β = 10-2, Γ = 2B

B

↑⊗

B

B→→11

Reconnection Region

σ = 10-1, β = 10-2, Γ = 21

ΦB = π/2Bz

BB↑⊗

10-1-10-11

ΦB = 0

1Bz

B

B→→

10-1-10-1

112

Summary• 超音速流に乱流を起こしたかった．
Kavli IPMU

• Numerical studyでBlobを置くのは最善ではないかも．
• 2D shock tube problem• 磁場の方向とshock形状やReconnection領域• Gamma-ray binaryやLaboratory Experiments?
13