| B |

1. |B| on MHD model MP Bin Bout |B| small large MP from[Maynard, 2003] -last closed field linesfor the northern axis of dipole, deflected by 23 degrees anti-sunward(colored by - |B|)

2. Energy transformation in MSH Magnetosheath (MSH) niTi +niMi/2(<Vi>2+(<dVi2>)+|B|2/8p {1}> {2}{3} Low latitude boundary layer (LLBL) niTi +niMi/2(<Vi>2+(<dVi2>)+|B|2/8p {1} > {2}<<{3}niMiVA2/2 Turbulent Boundary Layer (TBL) and outer cusp niTi +niMi/2(<Vi>2+(<dVi2>)+|B|2/8p+|dB|2/8p {1} ~{2} >> {3} <{4} macro RECONNECTION micro RECONNECTION

3. MSH MP BIMF Bin Fx ,u magnetosphere Fz Relation ofviscous gyro-stressto that of Maxwell: ~ const u/ B03 where ru- directed ion gyroradius, and L – the MP width. Forb ~ 1-10 near MPthe viscous gyro-stressis of the order of that of Maxwell.Velocityu, rises downstream of the subsolar point, magnetic field B0 - has the minimun over cusp, i.e.the gyroviscousinteractionis most significantat the outer border of the cusp, that results in the magnetic flux diffusion (being equivalent to the microreconnection)

4. Cluster OT crossing on 2002.02.13 theta L ~ RE En • Quicklook for OT encounter (09:00-09:30 UT) Energetic electrons & ions are seen generally in OT, not in magtosphere, they look to be continuous relative to the lower energy particles. Note also the maximum in energetic electrons at the OT outer border at ~09:35 UT. The upstream energetic particles are seen to 10:30 UT. magnetosphere OT MSH dipole tilt~14 d phi energetic ions |B| ions energetic electrons Surface charge decelerates plasma flow along normal and accelerates it along magnetopause tailward electrons cusp MSH MP

5. Plasma jet interaction with MP niMiVi2/2 < k (Bmax)2 /m0 [k ~ (0.5-1) – geometric factor] niMiVi2/2 > k (Bmax)2/m0 The plasma jets, accelerated sunward, often are regarded asproof for a macroreconnection; while every jet, accelerated in MSH should be reflected bya magnetic barrier forniMiVi2< (Bmax)2/m0in the absence of effective dissipation(that is well known in laboratory plasma physics)

6. Resonance interaction of ions withelectrostaticcyclotron waves Diffusion across the magnetic field can be due to resonance interaction of ions withelectrostaticcyclotron waves et al., Part of the time, when ions are in resonance with the wave - perpendicular ion energy s that can provide the particle flow across the southern and northern TBL, which is large enough i.e. for populating of the dayside magnetosphere

7. Measurements of ion-cyclotron waves onPrognoz-8, 10, Interball-1in the turbulent boundary layer (TBL) over polar cusps. Maximums are at the proton-cyclotron frequency. Shown also are the data fromHEOS-2 (E=1/c[VxB]),and from the low-latitude MPAMPTE/IRMandISEE-1. Estimation of the diffusion coefficient due toelectrostatic ion-cyclotron wavesdemonstrates thatthe dayside magnetosphere can be populated by the solar plasmathrough the turbulent boundary layer

8. Plasma percolation via the structured magnetospheric boundary Percolationis able to provide the plasma inflow comparable with that due to electrostatic ion cyclotron waves [Galeev et al., 1985, Kuznetsova & Zelenyi, 1990]:Dp~0.66(dB/B0)ri2 Wi~const/B02~(5-10)109m2/s ----------------------------------------------------------------------------------------------------------------- One can get a similar estimate for thekinetic Alfven waves (KAWin[Hultquist et al., ISSI, 1999, p. 399]): DKAW~k^2ri2Te/Ti VA/k||(dB/B0)2~~const/B03 ~1010m2/s

9. Interpretation of the early data from Prognoz-8in terms of the surface charge at MP Ion flux magnetosphere re ~ MSH [Vaisberg, Galeev, Zelenyi, Zastenker, Omel’chenko, Klimov И., Savin et al.,Cosmic Researches, 21, p. 57-63, (1983)]

10. Mass and momentum transfer across MP of finite-gyroradius ion scale ~90 km  ri at 800 eV ~ along MP normal Cluster 1, February 13, 2001. (a) ion flux ‘nVix’, blue lines – full CIS energy range), black – partial ion flux for > 300 eV, red – for > 1keV ions; (b) the same for ‘nViy’; (c) the same for ‘nViz’; (d): ion density ni (blue), partial ion density for energies > 300 eV (black) and that of > 1 keV (red). dominant flow along MP

11. Cluster 1, February 13, 2001 Thin current (TCS) sheet at MP (~ 90 km) is transparent for ions with larger gyroradius, which transfer both parallel and perpendicular momentum and acquire the cross-current potential. The TCS is driven by the Hall current, generated by a part of the surface charge currentat theTCS dF ~300 V

12. Mechanisms for acceleration of plasma jets • Besidesmacroreconnectionof anti-parallel magnetic fields (where the magnetic stress can accelerate the plasma till niMiViA2 ~B2/8p),there are experimental evidences for: • Fermi-type acceleration by moving (relative the incident flow) boundary of outer boundary layer; • - acceleration at similar boundariesby inertial (polarization) drift.

13. Magneto sonic jet • Acceleration in the perpendicular non-uniform electric field by the inertial drift • Fermi-type acceleration by a moving boundary;

15. Bi-coherence&the energy source for the magnetosonic jet Fl + Fk = F mHz

16. Inertial driftVd(1) = 1/(M wH2) dF/dt = Ze/(M wH2) dE/dtd Wkin ~ d(nM(Vd(0))2/2) ~30 keV/сm3(28 measured)Vd(0) = с[ExB] ; J ~ e2/(MpwHp2)dE/dt Electric field in the MSH flow frame

19. Cherenkov nonlinear resonance1.4 +3 mHz = fl + f k = (kV)/2p ~ 4.4 mHzL =|V| /( fl + fk )~ 5 RE Maser-like ?

20. Comparison of the TBLdynamics andmodel Lorentz systemin the state of intermitten chaos

23. In the jets kinetic energyWkin rises from ~ 5.5 to 16.5 keV/cm3For a reconnection acceleration till Alfvenic speed VA it is foreseen WkA ~ ni VA2/2 ~ const |B|2that requires magnetic field of 66 nT(120 nT inside MP if averaged with MSH) [Merka, Safrankova, Nemecek, Fedorov, Borodkova, Savin, Adv. Space Res., 25, No. 7/8, pp. 1425-1434, (2000)]

24. Ms~2 Ms~1.2 magnetosphere MSH

25. [Shevyrev and Zastenker, 2002]

26. 23/04-1998, MHD model, magnetic field at 22:30 UT; blue – Earth field; red - SW; yellow - reconnected;right bottom slide – plasma density; I- Interball-1, G- Geotail; P- Polar Reconnection X Reconnection X Reconnection X

28. The jet is also seen by POLAR (~ 4 Re apart in TBL closer to MP)

31. BS MP

32. Conclusions • Penetration of solar plasma into magnetosphere correlate with the low magnitude of magnetic field (|B|) (e.g. with outer cusp and antiparallel magnetic fields at MP). • A mechanism for the transport in this situation is the ‘primary’ reconnection, which releases the energy stored in the magnetic field, but it depends on the IMF and can hardly account for the permanent presence of cusp and low latitude boundary layer. Instead, we outline the ‘secondary’ small-scale time-dependent reconnection. • Other mechanisms, which maximize the transport with falling |B|: • finite-gyroradius effects (including gyro-viscosity and charged current sheets of finite-gyroradius scale, • filamentary penetrated plasma (including jets, accelerated by inertial drift in non-uniform electric fields), • diffusion and percolation, • In minimum |B| over cusps and ‘sash’ both percolation and diffusion due to kinetic Alfven wavesprovide diffusion coefficients ~ (5-10) 109 m2/s, that is enough for populating of dayside boundary layers. Another mechanism with comparable effectiveness is electrostatic ion-cyclotron resonance. While the cyclotron waves measured in the minimum |B| over cusps on Prognoz-8, 10 and Interball-1 have characteristic amplitude of several mV/m, the sharp dependence of the diffusion on |B| provides the diffusion ~ that of the percolation.