Simulations of binary accretion and modeling of the ...2015年度の論文TM+ 2015,MNRAS, 449, 123...
Transcript of Simulations of binary accretion and modeling of the ...2015年度の論文TM+ 2015,MNRAS, 449, 123...
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-1000 -500 0 500 1000x (AU)
-1000
-500
0
500
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z (A
U)
t = 6.90213E+05 yr, step = 214000tp = 1.76021E+04 yr offset = (-2.84E+04, 1.05E+04) AU
500 AU
(c)
22.5 23.0 23.5 24.0 24.5log column density (cm-2)
Simulations of binary accretion and modeling of the heliosphere
(XC-B)
Matsumoto, T. (Hosei univ)
Saigo, K (Osaka-pref Univ), Takakuwa, S. (ASIAA) 、
Shiota, D. (Nagoiya Univ), Kataoka, R. (NIPR)Miyahara, H. (Musabi), Miyake, S. (Ibaraki-Col. NIT)
平成27年度CfCAユーザーズミーティング 2016年1月29日@国立天文台水沢キャンパス
2015年度の論文 TM+ 2015,MNRAS, 449, 123
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Binary Accretion
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Introduction: recent works
• Observations– Radio observations: dynamics of CBD
• Takakuwa+ 14 …. protobinary system, L1551 NE, ALMA• Dutrey+ 15 ....T Tauri binary system, GG Tau, ALMA
– We have to explain these observations.
• Simulations– The recent works are high-resolution two-dimensional sims.
• Artymowicz & Lubow 96 … 3D SPH (early work)• (snip)• Hanawa+ 10 … two-dimensional mesh• Young+ 15 …… two-dimensional SPH
– High-resolution three-dimensional simulation are required.
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Model and method
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12 1 Density
Ω = 1
SFUMATO AMR code
• Isothermal gas• Self-gravity is ignored• A circular orbit of stars• FMR in rotating frame• Up to 100 revolutions• Calculation: 512 cores, 1 week
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Results (a typical model)
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q = 0.2, jinf = 1.2,
cs = 0.1, finf = 1.0
mass ratio
sound speed
angular momentum of gas
injection of gas
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Ensemble average of 80 - 100 revolutions.Horseshoe orbit @ gap, accretion @ arms
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Horseshoe orbit
Horseshoe orbit
Accretion Accretion
Stream lines:velocity @ co-rot frame
Surfa
ce d
ensi
ty
c.f., Young+ 15
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Outflow along arm Horseshoe orbit at gap
Detected by ALMA Cycle 0
Summary of gas flows in CBD and gap
Accretion along arm
Will be detected by ALMA Cycle 2
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Non-axisymmetric pattern rotates irrespective of binary parameters
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80 - 84 revolution
C.f., UY AurHioki+ 07Tang+ 15
surfa
ce d
ensi
ty
Matsumoto in prep
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4h31m44s7 44s6 44s5 44s4 44s3Right ascension (J2000.0)
18°8′29″
30″
31″
32″
33″
34″D
eclin
atio
n (J
2000
.0)
300 AU
Takakuwa+ 14
ALMA Cycle-0Non-axisymmetric patrern?
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Modeling of the Heliosphere
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Grand minimum
西暦(年)
Maunderminimum
ThepaintofThames
Solar activity → GCR modulation → climate change
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An evidence of the little ice age
“The Frozen Thames, looking Eastwards towards Old London Bridge”Abraham Hondius 1677年 12
現在のテムズ川(1月)
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Motivation• To investigate relationship between modulation of CGR
and magnetic field in the heliosphere during grand minimums.
• To make a framework of MHD+GCR for space weather.
電流シート
終端衝撃波
太陽圏界面
弓状衝撃波
地球
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Solar wind model is obtained by B obs.
r = R⦿ Field lines (2nd order)
Br(Rs)
Br(R⦿)
Inner boundaryr = 25 R⦿
Source surfacer = 2.5 R⦿
Potential B-field fromWSO obs fs =
✓R�Rs
◆2 Br(R�)
Br(Rs),
Super-radial expansion factor
C.f., Kataoka+ 09, Shiota+ 14
obs day: 2015/5/5
𝑉"# 𝑓" , 𝜌 𝑓" , 𝑝 𝑓"
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Results of test calculation (cross section)
-200 -100 0 100 200x (Rsun)
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-100
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100
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z (R
sun)
t = 3.0000000E+02
|v| (km s-1)
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-200 -100 0 100 200x (Rsun)
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y (R
sun)
t = 3.0000000E+02
|v| (km s-1)
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z = 0 plane y = 0 planevelocity velocity
43 cells/block×163 blocks/level= 643 cells/level
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Results of test calculation (3d view)
200 R☉
Current sheetBallerina structure
|𝑥|, |𝑦|, |𝑧| ≤ 50×22max 𝑅⊙
𝑙max = 9 のとき 𝑅boundary = 25600𝑅⊙ = 120AU
10数レベルでヘリオポーズをカバーする
𝐵G = 0
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Strong scaling
1000 1200 1400 1600 1800 2000 2200Parallel number
400
500
600
700
800
900
1000El
apse
tim
e (s
econ
d)
Idealw/o RefinementRefinement interval = 16Refinement interval = 8Refinement interval = 1
Parallel number
Cal
cula
tion
time
(sec
)Scales up to ~1000 cores.The better performance when lower frequency of refinement.
5123 cells/level×10 levels, 512 steps
Calculation time is estimated to be 40 hours for 1 year of the heliosphere.
7.89E5 mesh / core / sec
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Summary
• Binary accretion– Gas flows in the CBD and gap was reproduced.– Gas flows in the CBD were observed by ALMA Cycle 0. – Gas flows in the gap will be resolved by ALMA-Cycle2
• A dynamical model of Heliosphere– A test calculation
• Rotating solar wind model.• Refinement criterion is distance from the Sun. • The current sheet produces ballerina sturcture.
– Performance• AMR level is 10 layers.• Calculations were scaled on 2,048 cores.• Parallel efficiency is estimated as 50% at 5,000 cores.• OpenMP should be implemented for >10,000 cores.