ICMs and the IPM: Birds of a Feather?
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1 ICMs and the IPM: Birds of a Feather? Tom Jones University of Minnesota 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 1
2 Outline: ICM plasma is the dominant baryon component in the biggest gravitationally bound structures in the universe ICMs are basic barometers of cosmic large scale structure formation dynamics and physics ICMs are difficult to study (remote, faint and have cosmological evolutionary timescales) The Solar Wind plasma - interplanetary medium (IPM) surrounds us and is available for in-situ study dynamical times are accessible Plan: Lay out in general terms similarities and contrasts of these two environments What insights can the IPM provide to the study of ICMs? What common questions of mutual interest can we identify? 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 2
3 ICMs are Very Hot, Very Dilute and Fully Ionized Plasmas ICMs are Dynamic: Exhibit large scale, structured flows Frequented by shocks Turbulent 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 3
4 ICMs are Very Hot, Very Dilute and Fully Ionized Plasmas ICMs are Dynamic: Exhibit large scale, structured flows Frequented by shocks Turbulent Fabian + 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 4
5 ICMs are Very Hot, Very Dilute and Fully Ionized Plasmas ICMs are Dynamic: Exhibit large scale, structured flows Frequented by shocks Turbulent Markevitch + 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 5
6 ICMs are Very Hot, Very Dilute and Fully Ionized Plasmas ICMs are Dynamic: Exhibit large scale, structured flows Frequented by shocks Turbulent Coma Schuecker November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 6
7 The IPM is Very Hot, Very Dilute and Fully Ionized Plasma The IPM is Dynamic: Exhibits large scale, structured flows Frequented by shocks Turbulent 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 7
8 The IPM is Very Hot, Very Dilute and Fully Ionized Plasma The IPM is Dynamic: Exhibits large scale, structured flows Frequented by shocks Turbulent Coronal Mass Ejection (CME) STEREO-HI 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 8
9 Solar Wind in Action: Note Shocks from CMEs STEREO-HI 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 9
10 The IPM is Very Hot, Very Dilute and Fully Ionized Plasma More Shocks: Bow Shocks The IPM is Dynamic: Exhibits large scale, structured flows Frequented by shocks Turbulent Earth s Bow Shock 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 10
11 The IPM is Very Hot, Very Dilute and Fully Ionized Plasma The IPM is Dynamic: Exhibits large scale, structured flows Frequented by shocks Turbulent 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 11
12 Compare Some (Rough) Primitive IPM & ICM Values: Measure: Solar Wind (IPM): R ~ 1 AU kt e (kev) ~0.01 ~1-10 ICM: Outside of cores n e (cm -3) ~ 1-10 ~ P e ~ nkt (dyne/cm 2 ) ~ B (µg)* B n e (1/2) (roughly) ~ ~ *1 µg = 0.1 nt 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 12
13 Some (Rough) Characteristic Micro-Lengths: I Both plasmas are collisionless! Length: IPM: ICM: Coulomb scattering length ~ AU ~ kpc λ coulomb ~0.2 pc T kev2 /n e electron thermal gyro radius: ~ 1 10 km ~ 300-4x10 4 km r ge =ρ e ~ 1300 km T (1/2) kev /B µg proton thermal gyro radius: ~ km ~ x10 6 km r gp =ρ I ~ 5.6x10 4 km T (1/2) kev /B µg (r sun ~ 10 6 km) IPM and ICM thermal gyroradii are very much smaller than λ coulomb 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 13
14 Some (Rough) Characteristic Micro-Lengths: II Length: IPM: ICM: electron skin depth*: λ e = c/ω pe ~ 5km n e (-1/2) Ion inertial length**: λ i = c/ω pi ~ 200km n i (-1/2) ~ 1-5 km ~ km ~60 200km ~ ,000 km Debye length: ~.01 km (~ 10 m) ~ km λ D ~ 0.24 km (T kev /n e ) 1/2 IPM λ i is comparable to r gp ICM λ i is smaller than r gp *EM field penetration length **Ions decouple from electrons 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 14
15 Some (Rough) Dimensionless Plasma Measures Measure: Solar Wind: ICM: β = P/(B 2 /8π) = (6/5) c s2 /v A 2 ~ 8x10 4 n e T kev /B µg 2 Ion gyro/inertial length r gi /λ i = ρ i /λ I ~ β ~ ~ ~ ~ 7-30 N d = n e λ D3 ~ T kev (3/2) /n e (1/2) ~ ~ ICM is High β; IPM can be High β (border-line?) Both media are good plasmas N d >> 1 (support collective plasma wave families) 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 15
16 Some (Rough) Characteristic Velocities Velocity: IPM: ICM: Ion acoustic (sound) speed: c s = (5P/3ρ) ~ 500 T kev (1/2) km/s Alfven speed: v A = B/ (4πρ) ~ 2 B µg /n e (1/2) km/s ~ 50 km/s ~ km/s ~ km/s ~ km/s Turbulent velocities: δv ~ km/s ~ 300 km/s * Bulk flows: ~ km/s Up to ~ 2000 km/s *Assuming P turb ~ 0.1 c s Not measured directly Turbulence in both IPM and ICM should be compressional (δv/c s can be ~ 1) IPM turbulence should be MHD (δv <v A ) ICM turbulence (on large scales) should be HD (δv >v A ) (MHD for l < l A ~ L (v A /δv) 3 ) 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 16
17 Some (Rough) Shock Parameters Parameter: Solar Wind (IPM): ICM: M s = V s /c s < a few < a few M A /M s ~ β 1/2 ~ 1 ~ 10 Density compression ~ 2-3 ~ 2-3 IPM and ICM shocks have similar sonic (fast mode) Mach numbers ICM shocks (mostly) have higher Alfvenic Mach numbers than IPM shocks 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 17
18 That is: IPM Shocks are more highly magnetized than ICM shocks Magnetization: Spitkovsky 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 18
19 Intermediate Summary IPM and ICM plasmas both: are good plasmas (e.g., carry plasma waves) collisionless Coulomb collision lengths can approach system size have much smaller particle kinetic scales (e.g., gyro radii, inertial lengths) host compressible turbulence contain shocks with sonic Mach numbers of a few IPM magnetic field is relatively stronger, so: IPM turbulence is MHD on largest scales, while ICM turbulence is HD on largest scales, but probably MHD on smaller scales ICM shocks are less magnetized than IPM shocks, with larger Alfvenic Mach numbers 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 19
20 Some Shock Data: 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 20
21 Bullet Cluster Shock Profile M s ~ 3 Do not resolve shock discontinuity Markevitch November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 21
22 Earth s Bow Shock Profile (Quasi-Perpendicular) M s ~ 3.5 Thickness a few ion inertial lengths Schwartz November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 22
23 Some Turbulence Data: 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 23
24 Coma Cluster Density Fluctuations (Compressible Turbulence) In compressible turbulence (δρ) 2 ln( 1 + g 2 M 2 ) M = δv/c s g depends on forcing g = 1/3 solenoidal g = 1 compressive δρ l (1/3) Using g = 1/3 M ~ 0.5 Using g = 1 M ~ November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 24
25 IPM Turbulent Velocity Data f ~ 10-1 Hz -> 4000 km (10s of λ i ) Inertial range ~ 1000 km.01 AU Alexandrova + 13 (Salem + 09) 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 25
26 IPM Magnetic Field Turbulent Spectrum Steepens below ~ 10 λ i Alexandrova + 13 Note: Compressive modes predominantly slow mode (δb & δρ anticorrelated) 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 26
27 Summary The Solar Wind and ICMs have important common properties Shocks & Turbulence of similar strengths The Solar Wind is somewhat more magnetized That may influence details The physics of the Solar Wind is known in some detail Down to kinetic scales This may be helpful in understanding what may be important in ICM physics 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 27
28 감사합니다! 11 November, 2014 KAW8: Astrophysics of High-Beta Plasma in the Universe 28
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