1. ISSI - 2

2. Solar Wind Interaction Q1: Scope of the applicability of different modelling approach Q2: Adequacy in reflecting important physics Q3: How important is the IMF and solar wind variability

3. Q1 Hydrodynamic modelling vs MHD Single-fluid MHD vs. multi-fluid MHD MHD vs. hybrid kinetic simulations Stationary models vs. time-dependent models

4. Ion Pileup region at comet Halley Haeberli et al. (1995 )

5. 2D density profile of cometary ionosphere

6. Electron temperature variation Ion pileup region @ comet Halley. Collisional roto- vibrational excitation of water molecules. Electron cooling. Reduced electron recombination dissociation rate. Haeberli et al. (1995 )

7. Electron temperature variation Ion pileup region @ comet Halley. Collisional roto- vibrational excitation of water molecules. Electron cooling. Reduced electron recombination dissociation rate.

8. Ion-pileup region @ 1 AU Critical distance (r c ) for the ion pile-up region. Neutral gas density: n c ~ 3x10 6 H 2 O cm -3 at 1 AU. What about 67P? r c ~ Q ½ r c ~ 3000 km/10 ~ 300 km for Q ~ 2x10 27 H 2 O/s. Bockelee-Morvan et al. (2004 )

9. Ion-pileup region @ 3.25 AU For Q ~ 3x10 24 H 2 O s -1, r c ~ 15 km. Rosetta s/c will probably be in and out of the Hot electron zone/ion-pileup region. c/w p = 250 km Motschmann and Kuehrt (2006)

10. Ionospheric structures Ion kinetic effect: For magnetic field B ~ 10 nT and flow velocity ~ 5 km s -1, Ω ~ 0.052 rad s -1. and gyroradius R g ~ 100 km. No clear ionospheric boundary. Large variability in ionospheric structure (IMF direction dependence).

11. Can 67P ionosphere standoff solar wind at rendez-vous? Lorentz force = neutral gas drag force @ ionospheric boundary (Ip and Axford, 1982). At max. magnetic field, dB/dR ~ 0, R max ~ 1.1x10 -22 (Q 3/4 /a 1/2 /B max ) km

13. Sizing the cometary ionsphere… Q ~ 3x10 24 H 2 O s -1 and B max ~ 50 nT (max?), R max ~ km (for cold and hot electrons)! No magnetic field – free cavity. R max ~ 90 km @ perihelion, for Q ~ 3x10 27 H 2 O s -1.

14. Energetic pickup ions in the inner coma Eviatar et al. (1989)

15. Q3

16. 日冕物質在行星際空間擴張傳輸的模擬 http://www.theaustralianweatherforum.com/forum/viewtopic.php?p=56698

17. Ion tail turning caused by solar wind CIR

18. Additional physics to be considered Nucleus surface and dust coma could be subject to strong sputtering effect by energetic ions during quiet solar wind condition. Much more so during solar events. Effect of enhanced ionization by X-ray/EUV emission in solar flares. How about outbursts from the nucleus?

19. Neutral Coma Q4: Scope of the applicability of different modeling approach Q5: Adequacy in reflecting important physics Q6: How to obatin a consistent picture of the neutral coma

20. Neutral gas coma The surface outgassing pattern is controlled by composition and thermal inertia distributions.

21. Neutral coma @ 3.0 AU

22. Neutral coma @ 2.5 AU

23. Neutral coma @ 1.5 AU

24. CN jets of comet 2004 Q2 Machholz

25. Hybrid coma with distributed source? H 2 O + CO 2 (+icy grains) H 2 O + POM grains H 2 CO  CO CO CN (jets) Eberhardt et al. (1987) Thermo-degradation

26. Polyoxymethylene (H 2 CO) n Moore and Tanabe (1990)

27. PICCA mass peaks Huebner et al. (1987)

28. CO abundance is a mystery A’Hearn et al. (2013)

29. Chemical network Haider and Bhardwaj (2005)

30. Coupled dynamics and ion chemistry model calculations http://www.swissinfo.ch/media/cms/images/r db/2012/07/17774412-33077260.jpg

31. Electrostatic charging of the nucleus surface http://www.bibliotecapleyades.net/imagenes_ universo/electuniv17_10.jpg

32. Electrostatic charging of dust http://www.sciencedirect.com/science/article/pii/S157106451100087X Electrons

33. Dusty Plasma

34. Dusty plasma motion Wahlund et al. (2009)

35. Zonal structure of the dust coma @ 3.5 AU Dusty plasma zone λ D ~ 3-5 R N

36. Thanks