Electron heating and acceleration in two plasmas Electron heating - PowerPoint PPT Presentation

Workshop “Processus d'accélération en astrophysique IAP, Paris, October 4, 2012 Electron heating and acceleration in two plasmas Electron heating and acceleration in two plasmas colliding with sub-relativistic velocities colliding with sub-relativistic velocities S. Davis*, R. Capdessus, E. d'Humières, S. Jequier, I. Andryiash, V. T. Tikhonchuk Centre Lasers Intenses et Applications Université Bordeaux 1 – CNRS – CEA, Talence, France * Fulbright Scholar, United States Department of State, USA 1

Outline Outline  Instability analysis  Long term behavior and shock formation  Electron heating in the colliding plasmas  Single filament evolution GRB Workshop, IAP Paris, October 4, 2012 2

Colliding plasmas: sequence of instabilities Colliding plasmas: sequence of instabilities    u e u e First stage of interaction – electron-electron instability          Two-stream & Weibel e-e instabilities u v 0.5 k u E Te pe isotropization (mutualization)    and heating of electrons       u v u / c k u E Te pe    e u i u i Second stage of interaction – ion-electron instability    Filamentation ion-electron instability       , / , u v u c k u E filamentation of ion streams Te pi in a hot electron plasma, electron heating Ion acoustic instability – electrostatic turbulence           u c , ku , k u E s pi GRB Workshop, IAP Paris, October 4, 2012 3

Ion filamentation instability Ion filamentation instability Ion Weibel instability has attracted attention recently in relation with the GRB physics: Medvedev, Loeb, ApJ 1999, Lubarsky, Eichler, ApJ 2006 It is also of interest for ICF – RPA ions Growth rate is in the ion time scale, wavelength is on the electron spatial scale  2 2 2 k c x    k Dispersion equation xz x x   zz 2 xx j , j , E iz ez z    u u B     2 2 2 iz 0 2 2 2 2 y k u k c     pe pi pi z x 0 x i 1      2 2 2 2 k v 2 x Te In the limit  << kc 1/3       2 2 2 2 2 u u k u k c      pe pi     pe 0 0 2 x k 0 x i    ifi pi x   pi c c v 3   k v 2 pe Te x Te GRB Workshop, IAP Paris, October 4, 2012 4

Ion filamentation instability as an energy transformer Ion filamentation instability as an energy transformer Ion filamentation induces the charge separation x k     x u B v n j v iz y ix i iz ix j j E , , iz ez z     B E j  u u B y z ez iz 0 y z Instability is driven by phase difference between the electron and ion currents Saturation is due to the ion trapping → electron heating is important 1/3     u u     pe  pi  0 0 k        k u  ifi pi x c c v   tr ci x 0 ifi pe Te 1/3 1/3      2 m v B v m T   ix tr  e Te  y  e e     u k u m u  2 2 n m u  m m u  0 x 0 i 0 i i i 0 0 0 0 GRB Workshop, IAP Paris, October 4, 2012 5

Numerical simulations of ion filamentation instability Numerical simulations of ion filamentation instability Plasma collision with the solid wall Kato & Takabe, ApJ 2008 GRB Workshop, IAP Paris, October 4, 2012 6

Relativistic collisionless shock Relativistic collisionless shock Spitkovsky, ApJ 2008: collision of two identical relativistic plasmas with  = 15: efficient energy exchange – electron heating and magnetic field generation, but the mass ratio is small m i /m e ~ 16 – 100 Energy budget: ions are losing 40% of their initial energy, T e ~ T i , shock speed ~ c/2 electrons are gaining 35%, ~ Maxwellian energy distribution magnetic field energy raising to 15% at the shock front ~20 c/  pi GRB Workshop, IAP Paris, October 4, 2012 7

Simulation of collision of two sub-relativistic plasmas Simulation of collision of two sub-relativistic plasmas  = u p /c = 0.2  p ≈ 20 MeV 10 4  e plasma moving downstream for n 0 = 10 18 cm -3 T = 100 eV size 0.5×60 mm 2 Represents ISM time  pi -1 = 1 ps   = c/  pi = 220  m y Simulation of the plasma interaction in the center of mass reference frame in the ion filamentation-dominated regime   u c c m m / p s e i target plasma electron heating going from bottom ion slowing down to top T =10 keV magnetic field generation energy repartition in the upstream flow Represents external jet shock front formation 0 80  e 0 x GRB Workshop, IAP Paris, October 4, 2012 8

Ion phase space – time evolution Ion phase space – time evolution GRB Workshop, IAP Paris, October 4, 2012 9

Ion heating and slowing down Ion heating and slowing down Ion heating proceeds faster than slowing down – in the time scale of 200  pi -1 they are loosing less than 10% of their energy, while their temperature increases dramatically upstream downstream upstream GRB Workshop, IAP Paris, October 4, 2012 10

Global properties: filaments and fields Global properties: filaments and fields Plasma filamentation in the electron spatial scale c/  pe develops in the ion time scale 1/  pi  pi t = 10 current filaments are associated with strong small scale magnetic fields large amplitude charge density modulations producing strong electrostatic fields 11

Electron heating in the filaments Electron heating in the filaments Nonlinear evolution of filaments is associated with strong electron heating – by factor of 100 in the time scale of 10 – 20  pi -1  pi t = 9.3  pi t = 18.6  pi t = 28  pi t = 37 electron energy density GRB Workshop, IAP Paris, October 4, 2012 12

Temporal evolution of electron energy Temporal evolution of electron energy Probability distribution of the electron energy density  pi t = 10  pi t = 28  pi t = 37 Electron energy density saturates at the average level of 0.4 with a sharp cut-off at 1.5n 0 m e c 2 Electron temperature increases with time from 0.02 m e c 2 to 1.5m e c 2 in the time scale of 200  pi -1 GRB Workshop, IAP Paris, October 4, 2012 13

Continuous electron heating in filaments Continuous electron heating in filaments Hot electron temperature and their cut-off energy increase lineraly in time Stochastic heating process GRB Workshop, IAP Paris, October 4, 2012 14

Evolution of the ion energy density Evolution of the ion energy density Ion energy evolution is much slower – in the time scale of 200  pi -1 they are losing less than 10% of their energy. Filament rotation generates the parallel electric field that slows down the ions  pi t = 9.3  pi t = 18.6  pi t = 28  pi t = 37 GRB Workshop, IAP Paris, October 4, 2012 15

Evolution of the magnetic fields Evolution of the magnetic fields  u / c Magnetic fields follow essentially the filament evolution  ce 0   – their spatial scale and the volume increase with time.  1/3   u / v pe The amplitude agrees with the saturation level. pi pe Te 0 16

Single filament characterization Single filament characterization Zoom of a single filament at the time of 400  pe -1 very large compression by a factor of 6 ion density maximum is higher than the electron one very high energy of electrons in the filament strong magnetic field around the filament – high electric current strong electrostatic field due to the charge separation filament life time about 10 – 20  pi -1 GRB Workshop, IAP Paris, October 4, 2012 17

Conclusions Conclusions Similarity in the physics of laser plasma interaction and some phenomena in the GRBs – modeling of the collisionless sub- relativistic shocks in laser plasma interactions requires very big volumes, long times and high laser energies Electron heating is an important stage of the shock formation. This is a stochastic process that occurs due to the strong charge separation in filaments Energy transfer to magnetic fields in limited by the ion trapping in the filaments Parallel electric field is generated later in time in the downstream zone due to the filament rotation Radiation losses due to the electron synchrotron emission. Next step: photon – electron kinetics GRB Workshop, IAP Paris, October 4, 2012 18