「銀河のダスト」研究会

2009年10月8-10日

大阪産業大学

太陽風3次元構造とダスト粒子軌道の解析
鷲見治一, G. P. Zank, Q. Hu（アラバマ大）田中高史（九大理）

3D MHD + Test Particles

V1-TScrossing:at 94
AU?
Whereis the
Termination
Shock

Asymmetric structure
Time-varying effect

V2-TS crossing: at 84 AU
105

V1

100

AU

95

V2

90
85
80
75

2001.5 2002 2002.5 2003 2003.5 2004 2004.5 2005 2005.5 2006 2006.5 2007 2007.5 2008 2008.5 2009

YEAR

InterstellarMedium

Z

Termination Shock

V1

YSUN

V2

HELIOPAUSEX

内容
１． 太陽圏、恒星圏（SN1987A、PN）の構造ー MHDシミュレーション
２．銀河宇宙線、荷電ダスト粒子の太陽圏内部への輸送ー （MHD＋テスト粒子）シミュレーションの準備
３． 太陽圏構造とダイナミックス
ー Voyager観測を基礎として

poleMagnetic Pressure Force
BMAXsunequatorSN1987A

http://swoops.lanl.gov/lasco_swoops.html

High-speed Polar Wind observed by Ulysses and IPS
North Pole

High-speed

Low-speed

Low-speed

High-speed
South PoleTanaka &Washimi (Science 2001)Density

Pram/Pb

Both the SN1987A progenitors andthe AGB star should have magnetic
field and the high-speed polar winds

BComparative Outer-Gas Structures
Outer Heliosphere

SN1987A Global Structure

Bipolar-Planetary NebulaStarStructure-Type
Mass of Star
Stellar CycleDominant Effects

Sunnose-cone
1 Msun22 years

Red and Blue Super-Giants
3-ring> 8Msun> several 103 years

Asymptotic Giant Blanchbipolar< 8Msun> 103 years

ISM & IS-Magnetic Field

Yes

NoNoTime-Varying Stellar-WindYes

Yes (from RSG to BSG)

No

High-Speed Polar Stellar-Wind Yes

Yes

Yes

Interplanetary Mganetic Field

Yes

Yes

(Nonlinear Effect)?

内容
１． 太陽圏、恒星圏（SN1987A、PN）の構造
ー MHDシミュレーション
２．銀河宇宙線、荷電ダスト粒子の太陽圏内部への輸送
ー （MHD＋テスト粒子）シミュレーションの準備
３． 太陽圏構造とダイナミックス
ー Voyager観測を基礎として

Problem of ananomalous anti-protonabundance,a result of dark-matterannihilations ?

PAMERA Obs.

Orbit analysis of 500 GeV proton
this Larmour radius corresponds
to the dust grain of velocity = 25 km/s,(M/Q)dust ~ 107 (M/Q)proton

dust-grain transit time for 1AU moving ~ 70 days
B (μG)
Larmour Radius (AU)Period (year)

0.33
334
400

1.0111
133

3.037
44.7

3. 3D-MHD plus test-particles program (T. Tanaka)
Dodecahedron

division into triangles

2nd subdivision

3rd subdivision

1st subdivision

4th subdivisionunstructured grid
5th subdivision
7682 grids

X-Z Plane
1 GeV Inv_B
0k step
datafrs4000

X-Z Plane
1 GeV Inv_B
80k step
datafrs3080

X-Z Plane
1 GeV Inv_B
160k step
datafrs3160

X-Z Plane
1 GeV Inv_B
340k step
datafrs3340

X-Z Plane
1 GeV Inv_B
80k step
datafrs3080

X-Z Plane
1 GeV Inv_B
160k step
datafrs3160

X-Z Plane
1 GeV Inv_B
340k step
datafrs3340

Fine Structure in the heliosheath:
Magnetic Wall
Plasma Sheet & Current Sheet

Washimi & Tanaka 1996

Y-Z Plane X=500 AU
1 GeV Inv_B
80k step
datafr1s3080

Y-Z Plane X=500 AU
1 GeV Inv_B
280k step
datafr1s3280

Y-Z Plane X=500 AU
1 GeV Inv_B
340k step
datafr1s3340

内容
１． 太陽圏、恒星圏（SN1987A、PN）の構造
ー MHDシミュレーション
２．銀河宇宙線、荷電ダスト粒子の太陽圏内部への輸送
ー （MHD＋テスト粒子）シミュレーションの準備
３． 太陽圏構造とダイナミックス
ー Voyager観測を基礎として

V1-TScrossing:
at 94
AU?
Whereis theTermination
Shock

Asymmetric structure
Time-varying effect

V2-TS crossing: at 84 AU
Interstellar
Medium
V1105
100

AU95

V290
85
8075

2001.5 2002 2002.5 2003 2003.5 2004 2004.5 2005 2005.5 2006 2006.5 2007 2007.5 2008 2008.5 2009

YEAR

Interstellar
MediumZTermination ShockV1YSUN

V2HELIOPAUSEXFine Structure in the heliosheath:
Magnetic Wall
Plasma Sheet & Current Sheet

Washimi & Tanaka 1996

High-speed Polar Wind observed by Ulysses and IPS
North Pole

High-speed

Low-speed

Low-speed

High-speed
South PoleNormalized V2 Obseved Ram-Pressure
Ram-Pressures after Aug 14, 2007 are assumed to be 1.0, 1.25, or 1.5 x Pram0 for forecasting
where Pram0 is ram-pressure when the speed 400km/s and density 5/cc at 1 AU10-9 Pa
1098765432102001.5 2002 2002.5 2003

2003.5 2004 2004.5 2005 2005.5 2006 2006.5 20072007.5 2008 2008.5 2009

High-speed Polar Wind:
An example which satisfies the V1-TS and V2-TS crossings simultaneously
North Pole

V1ram-pressure ratio = 1.5
θ = 30ºHigh-speed

Low-speed

Low-speed
30º

V2High-speed
South Pole

2. MHD Solution
When N0=5.10/cc at 1AU, and θ0=30°, both V1 and V2 crossing observed positions
are found to be reproduced simultaneously.
TS Position along Sun-V1 and Sun-V2 lines(Solar-Wind Ram-Pressure Anisotropy 1.5 at Latitude 30 degrees)
100

V195

AU90

V285

8075
2001.5

2002

2002.5

2003

2003.5

2004

2004.5

2005

2005.5

2006

2006.52007

2007.52008

Stone et al. 2008

AUV1

100

9590

AU

V185

V2+7AU80

V275
2001.5

2002

2002.5

2003

2003.5

2004

2004.5

2005

2005.5

2006

2006.52007

2007.52008

Magneto-sonic pulse is reflected at the lower boundary of plasma sheet.
When the returned pulse travels back and collides with TS, TS substatially decreses.

Story & Zank 1997
Fast shock (magneto-sonic pulse) isdriven downstream of TSFig. 5a

Plasma sheet is identified as red-color zone around 120-130 AU.
Below the plasma sheet yellow color zone is identified as magnetic wall.

Fig. 5b

Plasma sheet (yellow zone qround 120-130 AU) is identified as yellow zone whereheliosheath temperature sharply decreases with the distance from Sun.

Fig. 5c

Lower boundary of the plasma sheet is identified as yellow line around 120 AU from
where plasma density sharply increase.

Fig. 5dMagnetic wall region is identified as dark color where magnetic intensity is maximum inthe heliosheath. Yellow line aroud 122 AU is current sheet embedded in plasma
sheet.

Fig. 5e