Vladimir M. Gubchenko Institute of Applied Physics, Russian Academy of Science февраль 09, 2012 ОФН-2012, ФЕВРАЛЬ 6-10, 2012, ИКИ РАН, Москва К кинетическому описанию структуры «диффузной» области в нулевой точке, сформированной потоком плазмы

Chapman-Ferraro/Dangy problem (CF/DP) on inductive interaction of the plasma flow with the source of magnetization - induced 3D Magnetosphere and X points. DR in kinetics. B 0 =0 B0B0

1. Separated solar streamer and CME, Streamer belt. Sources of type III and type I radiobursts. V

2. 3D Magnetosphere under SW flow with VDF f(v). Does f(v) shape affect space weather? Sources of ULF e.m. noise. v i

3. Relativistic jets. Sources of MW and X/gamma ray e.m. emissions. V = ckT>>mc 2

4. Radar and Sonar cloak systems. Acoustic metamaterials? How to make a cloak for shock wave by e.m. action ?

5. HED (High Energy Density Plasma) = ФВПЭ – физика высокой плотности энергии

6. PIC magnetosphere by Buneman, Nishikava, Cai, Lembege. B 0 =0. Subrelativistic plasma. 3D e.m. PIC code Tristan. (3D PIC in LANL, LNL, SNL, NNSA etc !) v = 0.5c in the +x direction, representing the solar wind without an IMF. The electron and ion thermal velocities are v e = (T e /m e ) 1/2 = 0.2c and v i = (T i /m i ) 1/2 =0,05c m i /m e = 16 v i

What we have now in the LSK: postulated 1D (2D!) current sheets models and get the X line. 3D X pont topology? Diamagnetic spontaneus sheets (thick sheets). Harris like sheets. Resistive induced by SW flow sheets (thin sheets). Kropotkin, Zeleny, Malova, Artemyev, sheet with B n. 2D configurations as tearing and stratification modes in the 1D sheets (LS e.m. Weibel like instability) are related with shape as anisotropy of VDF. L S =?

People have been constructing substorm models for nearly forty years; thus it seems highly unlikely to be possible to introduce anything radically new at the field at this time… –Siscoe et al. Search for an onset mechanism that operates for both CMEs and substorm D LSK?? The future thrust of magnetospheric research should thus be to understand the microphysics and its coupling to meso- and macro-scales. This will also form an important to space weather studies- Paschman et al Directions Magnetospheric research: A report on ISSI forum, D LSK?? To the 3D LSK …… and to the 3D X points

Linear LSK parameters: Mach number M=v/c s – shock pressure. E.m. number G V – eddy T currents. Mach number M governs L fields topology –shape of the Mach cone. What is a number G v which governs TEM fields topology --- tailization and dipolization?. Resistive state G V >1 SW is as diamagnetic. G V a function of the SW VDF f(v) shape in collisionless plasma in kinetics?

Diffusion 3D region (DR) with resistive and diamagnetic eddy currents forming self consistent electro and magnetic field structure. Diffusion region –DR is a source of accelerated (energetic) particles (AP). AP are forming resistive current (in red). There are diamagnetic particles which form diamagnetic current (in blue).

Electrotechnical model of plasma for the hot regime. The quality G. Meso/macroscales in the 3D LSK. Plasma anisotropy parameters. Loss and reactivity angles and G v as number N of loops in coil

MHD to Vlasov/Maxwell? Hot regime. Is in a high beta X point - special LSK plasma ? Diamagnetic (front) and resistive (tail) boundary of the DR and TWO nonlinear parameters. Theory MHD (1 fluid, 2 fluid...) MHD+LS Kinetics (MAA+LZ) Selfconsistent LS Kinetics (Vlasov+Maxwell, Darwin..) Boundary of the DR

The metallic approach:Quasiparticle & media for C-F/D problem. Free particles in hot collisionless plasma with VDF f(v). Trapped and flyby particles in presence of the moving dipole with velocity v. The Internal magnetosphere is a Quasi particle as moving magnetization in the media having Magnetic Dipole and Magnetic Toroid moments. TheOuter Magnetosphere is inductive mode Cherenkov excitation in media.

Electric current in the «quasiparticle» and current in directly flowing «media». Trapped particles =quasiparticle form magnetic dipole and toroidal magnetization with postulated parameters and spatial distribution. Flyby particles=media are perturbed in their motion and are the subject of the selfconsitent Vlasov/Maxwell consideration.

On a Quasiparticle:Toroid orthogonal to Dipole, both are moving and are with gaussian spatial distribution. Parameter of toroidosity.

E.m. fields as combination of the dirivatives of the characteristic function M G. To B-normal!

Условие равенства нулю нормальной компоненты- координата «X точки». Сколько их?

3D mapping of the magnetic field lines near X points (…. 2D Андронов …3D???.. Cai….)

Характеристическая функция M G и её представления непосредственно по плоским волнам представление через цилиндрические гармоники –дальний хвост представление через сферические гармоники – ближний хвост представления через разложения в степенной ряд около Х точек.

Vlasov equation solution as dielectric (conductivity) tensor. Isotropic tensor. The egn. modes in media with isotropic VDF F(v). Denominator D T.

Thin (anomalous skin ) and thick (magnetic Debye) scales for LSK modeling induced by the SW flow. Meso/Macroscales from kinetics. Energy anisotropy Anomalous skin scale Diamagnetic Debye scale Momentum anisotropy The LSK limit appeared when: The DR is special high beta plasma

Quality G V depends only from the VDF shape and not (!) depends from plasma concentration. Ratio G w,k of diamagnetic to resistive current components in the media. Ratio G w,k = G kv,k = G V of diamagnetic to resistive current components for direct motion: Cherenkov process ω=kv.

2D characteristic function M G at hot regimes - magnetic Reynolds Re m =r 0 /r G and quality G V =r G /r DM are parameters! G V !! Re m =r 0 /r G

Shape: maxwellian VDF F(V) flow in DR.

Shape kappa VDF flow in DR: G V /G VM ratio as function of the parameter kappa of for power law VDF. Is G v a new space weather parameter together with Mach M !? Halo and Core kappa distributions of the SW VDF G V /G VM

Выводы Дано общее описание 3D магнитосфероподобных структур в кинетическом приближении Власова с учетом вида функции распределения потока для широкого класса плазм. Структура магнитного поля определяется двумя линейными масштабами пространственной дисперсии кинетической природы и линейными безразмерными параметрами число Маха и электромагнитная добротность. Введены два безразмерных нелинейных параметра для определения границ линейного описания поля в диффузионной области около Х точек. Получено уравнение и график для определения положения Х точек по данным об источнике и кинетических характеристик потока. Даны условия для определения структуры силовых линий около Х точек.

Diffusion region: 3D tail from MD part of magnetization. G V

Diffusion region: 3D tail from the MT part magnetization. G V

Values in the digits for the streamer: Scales of the AR Curr., Moments Velocity Scales ….

Values in the digits for Mag. PRC: Scales of the Mag Curr., Moments Velocity Scales ….