For IMF Bz<0 MP moves inward :

1. The flow dynamic pressure compress the magnetic fieldat magnetopause (MP), which while reconnected, in turn, accelerates plasmaacross the flowtill Alfven speedby the magnetic stress, then:|B|2/8p ~niMiVA2/2 Re-connection [Sweet, P. А. (1958), in Lehnert, В. (ed.) Electromagnetic Phenomena и Cosmic Physics, 123, Cambridge Univ. Press, New York] [Parker, E. N., (1963), Phys. Rev., 107, 924 ] Z For IMFBz<0 MPmovesinward: Rs=11.3+0.25ВzRs–subsolar MP distances in Earth radii,‘В’,innT X Y

2. [Chapman & Ferraro, JGR, 36, 77, 1931] [Axfordet al., JGR, 70, 1231, 1965] [Stern, JGR, 90, 10,851,1985] [V. Pletnev, G. Skuridin, V. Shalimov, I. Shvachunov,"Исследования космического пространства" М.: Наука,1965] Distribution of surface currents

3. A question since 1978: Does TBL exist? There are 2 characteristic examples from Interball-1 Interball-1, May 26, 1996, 01-04 UT Bx Byz |B| Bx -spectra, 0.1 –10 Hz SW BS MSH TBL MP

5. cusp Generation of turbulent boundary layer in the process of interaction of hydrodynamic flow with obstacle (from [Haerendel, 1978]). “1” – marks open cusp throat, “2” – stands for high latitude boundary layer downstream the cusp. Reynolds number (for the cusp scale of 2-3 RE) Reri ~ 100-500

6. |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|)

7. Interball-1 OT summary • In summer outer cusp throat (OT) is open for the MSH flow.TBL (turbulent boundary layer) is mostly in MSH. • In winterOT is closed by smooth MP at larger distance. Inside MP ‘plasma balls’ (~few Re) contain reduced field, heated plasma & weaker TBL. • OT encounters on 98.06.19 at 10-11 UT by Interball-1 and Polar are shown

8. 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

9. 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)

10. 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

12. 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)

13. 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

14. 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

15. 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

16. 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)]

17. 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

18. 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

19. 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.

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

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

23. 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

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

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

33. TBL dipole tilt~19 deg. MSH Simultaneous Polar data in Northern OT cusp • From top: -Magnetic field • Red lines-GDCF model, difference with data is green shadowed • -energy densities of magnetic field, ion thermal & kinetic, • note deceleration in OT in average relative to GDCF model (red)& ~fitting of kinetic energy in reconnection bulges at 10-11 UT to GDCF. • -energetic He++ • at 10-11 UT energetic tails of the MSH ions reach ~200 keV, that infers local acceleration reconnection bulges GDCF model

35. 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)]

36. Ms~2 Ms~1.2 magnetosphere MSH

37. [Shevyrev and Zastenker, 2002]

38. 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-1G- Geotail; P- Polar Reconnection X Reconnection X Reconnection X

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

43. BS MP

44. Interball-1 outbound from cusp to TBL, stagnation region and MSH (April 2, 1996) • The jet with extra kinetic energy Ekin of 5 keV/сm3 requires magnetic field pressure (Wb) > than inside MP (which should be averaged with that in MSH!)

45. Fine structure of transition from stagnation regioninto streaming magnetosheath: magnetic barrier with the trapped ions • Energy per charge spectrogram for tailward ions (upper), and magnetic field magnitude |B| INTERBALL-1, April 2, 1996

46. Vortex street on April 2, 1996 in ion velocity (to the left) and in magnetic field (to the right)

47. Interball-1 MSH/stagnation region border encounter on April 21, 1996. • Comparison with switch-off slow shock [Karimabadi et al., 1995] displays strong magnetic barrier with pressure of the order of the MSH dynamic pressure. Inside ‘diamagnetic bubble’ ion temperature balances the external pressure

50. Polar, May 29, 1996, 10:00-10:45 UT