Rela%vis%c Nonthermal Par%cle Accelera%on in Magne%c Reconnec%on

Similar documents
Radia%ve Magne%c Reconnec%on. in Astrophysical Plasmas. Dmitri Uzdensky. (University of Colorado, Boulder) collaborators:

PLASMOIDS IN RELATIVISTIC RECONNECTION: THE BLOBS OF BLAZAR EMISSION? Maria Petropoulou Purdue University

arxiv: v1 [astro-ph.he] 1 Aug 2018

Magnetic dissipation in pulsar winds

Cosmic Ray Acceleration by Magnetic Reconnection

Reconnection and the Formation of Magnetic Islands in MHD Models

Plasmoids in relativistic reconnection, from birth to adulthood: first they grow, then they go

Vladimir Zhdankin, JILA/CU-Boulder US-Japan Magne>c Reconnec>on Workshop, 3/7/2016

Magne&c Dissipa&on in Rela&vis&c Jets

Kinetic Plasma Simulations in Astrophysics. Lorenzo Sironi

Relativistic reconnection at the origin of the Crab gamma-ray flares

Mechanisms for particle heating in flares

Hard Electron Spectra and Polariza2on Proper2es of Rela2vis2c Jets

Magnetic reconnection in high-lundquist-number plasmas. N. F. Loureiro Instituto de Plasmas e Fusão Nuclear, IST, Lisbon, Portugal

arxiv: v2 [astro-ph.he] 18 May 2016

Electron heating in shocks and reconnection

Explosive reconnection of the double tearing mode in relativistic plasmas

Particle acceleration during 2D and 3D magnetic reconnection

Particle Acceleration by Reconnection and VHE emission Around Black Holes and Relativistic Jets

3D hybrid-kinetic turbulence and phase-space cascades

Explosive X-point reconnection & Crab flares. Maxim Lyutikov (Purdue U.)

Simulations of relativistic reconnection in pulsar wind nebulae and pulsar winds

Gyrokinetic Simulations of Tearing Instability

Modeling of Pulsar Wind Nebulae

Crab flares - explosive Reconnection Events in the Nebula

Magnetic Reconnection: Recent Developments and Future Challenges

Transition From Single Fluid To Pure Electron MHD Regime Of Tearing Instability

Radiative Magnetic Reconnection in Astrophysics

Particle acceleration at relativistic shock waves and gamma-ray bursts

Acceleration of Particles in Gamma-Ray Bursts

Rela%vis%c Reconnec%on in Pairs: Mass Transport (Accelera%on?)

Diffusive shock acceleration: a first order Fermi process. jan.-fév NPAC, rayons cosmiques E. Parizot (APC)

Single- and Two-Component GRB Spectra in the Fermi GBM-LAT Energy Range

arxiv: v2 [astro-ph.he] 26 Nov 2018

arxiv: v1 [astro-ph.he] 23 Oct 2018

Low energy effec,ve theories for metals. Sung-Sik Lee McMaster University Perimeter Ins,tute

Self-organization of Reconnecting Plasmas to a Marginally Collisionless State. Shinsuke Imada (Nagoya Univ., STEL)

UHECR from Pulsars/Magnetars based on An Auroral Accelerator Model for Gamma Ray Pulsars

PULSAR WIND NEBULAE AS COSMIC ACCELERATORS. Elena Amato INAF-Osservatorio Astrofisico di Arcetri

Magnetic Reconnection in Laboratory, Astrophysical, and Space Plasmas

Magnetic Reconnection: explosions in space and astrophysical plasma. J. F. Drake University of Maryland

School and Conference on Analytical and Computational Astrophysics November, Angular momentum transport in accretion disks

Forced hybrid-kinetic turbulence in 2D3V

Diversity of Multi-wavelength Behavior of Relativistic Jet in 3C 279 Discovered During the Fermi Era

Tsvi Piran The Hebrew University

Scaling of Magnetic Reconnection in Collisional and Kinetic Regimes

- Covered thus far. - Specific Intensity, mean intensity, flux density, momentum flux. - Emission and absorp>on coefficients, op>cal depth

Magnetic Reconnection in Space Plasmas

Stellar dynamo: new insights from the Kepler mission. Alfio Bonanno INAF Catania Astrophysical Observatory

Magnetohydrodynamic Turbulence: solar wind and numerical simulations

Formation of lamp-post coronae in Seyfert Galaxies and X-ray binaries

3D Reconnection of Weakly Stochastic Magnetic Field and its Implications

Approaching the GRE Physics

ブラックホール磁気圏での 磁気リコネクションの数値計算 熊本大学 小出眞路 RKKコンピュー 森野了悟 ターサービス(株) BHmag2012,名古屋大学,

Cosmic-ray Acceleration and Current-Driven Instabilities

Plasma Physics for Astrophysics

Bounce-averaged gyrokinetic simulations of trapped electron turbulence in elongated tokamak plasmas

Energy build- up & release erup3ons. MHD instabili3es Lecture 2 Jan. 23, 2017

Infernal modes and physical interpreta3on of the edge harmonic oscilla3ons in tokamak QH mode discharges

arxiv: v1 [astro-ph.he] 23 Jun 2016

High-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array

Ken Nishikawa. What is Plasma? 2. Simulation methods. 3. Fluid (GRMHD) Simulations Global Dynamics of Plasmas

Asymmetric Magnetic Reconnection in the Solar Atmosphere

Mikhail V. Medvedev (KU)

Asymmetric Magnetic Reconnection in the Solar Atmosphere

Fractal Structure (Turbulence) and SOC of a Current Sheet in a Solar Flare via Dynamic Magnetic Reconnection

Asymmetric Magnetic Reconnection and the Motion of Magnetic Null Points

Basic Mathema,cs. Rende Steerenberg BE/OP. CERN Accelerator School Basic Accelerator Science & Technology at CERN 3 7 February 2014 Chavannes de Bogis

Highlights from (3D) Modeling of Tokamak Disruptions

Strong collisionless shocks are important sources of TeV particles. Evidence for TeV ions is less direct but very strong.

MHD Simulation of Solar Chromospheric Evaporation Jets in the Oblique Coronal Magnetic Field

Can blazar flares be triggered by the VHE gamma-rays from the surrounding of a supermassive black hole?

NUMERICAL STUDY OF NON-THERMAL EMISSION FROM LAGRANGIAN PARTICLES IN AGN ENVIRONMENTS.

Non-Thermal Electron Energization from Magnetic Reconnection in Laser-Driven Plasmas. Abstract

Gyrokinetics an efficient framework for studying turbulence and reconnection in magnetized plasmas

High quality beam genera1on in density downramp injec1on and its early applica1ons

Review of electron-scale current-layer dissipation in kinetic plasma turbulence

On (shock. shock) acceleration. Martin Lemoine. Institut d Astrophysique d. CNRS, Université Pierre & Marie Curie

Radiative processes in GRB (prompt) emission. Asaf Pe er (STScI)

High Power Heating of Magnetic Reconnection for High-Beta ST Formation in TS-3 and UTST ST Merging Experiments

Relativistic MHD Jets

Nonlinear Fragmentation of Flare Current Sheets

arxiv: v1 [astro-ph.he] 3 Jan 2019

Simulation of Relativistic Jet-Plasma Interactions

Magnetohydrodynamic Turbulence

Polarization Swings Reveal Magnetic Energy Dissipation in Blazars

Magnetic Reconnection: dynamics and particle acceleration J. F. Drake University of Maryland

Bunch trains. Linear stability theory; IntegrodifferenQal. eqns; Pseudospectra?

Turbulent Magnetic Helicity Transport and the Rapid Growth of Large Scale Magnetic Fields

8.2.2 Rudiments of the acceleration of particles

Cosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation

Electron acceleration by strong DC electric fields in extragalactic jets

Models of Inefficient Accretion onto a Black Hole and Pair Production in Jets

Magnetically-dominated relativistic jets.

Stellar Magnetospheres part deux: Magnetic Hot Stars. Stan Owocki

Magnetic Fields in Blazar Jets

Stability of strong waves and its implications for pulsar wind shocks

arxiv: v1 [astro-ph.he] 19 Oct 2017

On the physics of shear flows in 3D geometry

The correlation between magnetic flux and jet power

Transcription:

Rela%vis%c Nonthermal Par%cle Accelera%on in Magne%c Reconnec%on Dmitri Uzdensky (University of Colorado Boulder) Thanks to Univ. Colorado Theore9cal Plasma Astrophysics Group: Greg Werner Vladimir Zhdankin Mitch Begelman (support by NSF, NASA, DOE) 3 rd Purdue Workshop, May 8, 2018 D. Uzdensky 5/8/2018 1

OUTLINE: Theory of NTPA In Magne>c Reconnec>on Physical Picture and AssumpQons. Empirical (numerical) Knowledge Base. Key Ingredients of the KineQc EquaQon: AcceleraQon by reconnecqon electric field; MagneQzaQon by reconnected magneqc flux: (power-law slope) Trapping in plasmoids: (high-energy cutoff) Effects of Guide magneqc Field Conclusions (RadiaQve Turbulence) D. Uzdensky 5/8/2018 2

Physical Picture: Reconnec>on Plasmoid-dominated magneqc reconnecqon plasmoid chain, characterized by a plasmoid distribuqon funcqon F(w) and a cumulaqve distribuqon N(w): ReconnecQon may or not be relaqvisqc. ReconnecQon rate: E rec = β rec B 0 = ε V A B 0 /c = ε β A B 0 V A = cβ A = c σ h 1+σ h Hot magneqzaqon: σ h = B 02 /(4π nh); h = relaqvisqc enthalpy per parqcle. rel. limit: σ h >>1 à V A ~ c non-rel. limit σ h << 1 à β A = V A /c ~ σ h 1/2 << 1. I will also use cold σ = B 02 /(4π n b mc 2 ) But parqcles under consideraqon are ultra-relaqvisqc. D. Uzdensky 5/8/2018 3

Self-similar hierarchical plasmoid chain Cerun et al. 2013 Bhakacharjee et al. 2009 Two Phases of Reconnected MagneQc Field: - of order B1 = εb0 = 0.1 B0 in current sheets - of order B0 in plasmoids D. Uzdensky 5/8/2018 4

Dimensionality Real world is 3D. However, recent PIC simulaqons of relaqvisqc pair-plasma reconnecqon (Werner & Uzdensky 2017, also Sironi & Spitkovsky 2014, Guo et al. 2015) show that 2D and 3D give the same NTPA. (However, for non-relaqvisqc electron-ion plasma reconnecqon, 2D and 3D NTPA may be different, see Dahlin et al. 2015-2017.) Thus here we will consider 2D reconnecqon. DirecQon perpendicular to current sheet: parqcles confined to the sheet by reconnecqng magneqc field à consider only moqon along the sheet. D. Uzdensky 5/8/2018 5

Basic Picture While they are unmagneqzed, energeqc parqcles are accelerated by the main reconnecqon electric field E rec. This steady acceleraqon proceeds unql a parqcle is captured by the reconnected magneqc field. Reconnected magneqc field is bimodal: ~ B 1 ~ ε B 0 ~ 0.1 B 0 in inter-plasmoid current layers; ~ B 0 in circularized plasmoids [with size distribuqon F(w)] We will treat magneqzaqon in B 1 and trapping in plasmoids separately. D. Uzdensky 5/8/2018 6

Empirical Numerical Proper>es of Reconnec>on-driven rela>vis>c NTPA Power-law index p p scales with σ h as p(σ) 2.2 p ~ C 1 + C 2 /σ h 1/2 High-energy cutoff (Werner et al. 2016) 2.0 1.8 1.6 1.4 1.2 1.0 10 0 10 1 10 2 10 3 pair plasma: Werner et al. 2016 electron-ion plasma: Werner et al. 2018 Two high-energy cutoffs: - exp(- γ/γ c1 ); γ c1 ~ 4σ, (guide magneqc field suppresses NTPA, see below) - exp[-(γ/γ c2 ) 2 ]; γ c2 ~ 0.1 L/ρ 0 (ρ 0 = m e c 2 /e B 0 ) D. Uzdensky 5/8/2018 7

High-Energy Power-Law Cutoff (Werner, Uzdensky, CeruI, Nalewajko, Begelman, ApJL 2016) 2.2 α * (σ h ) 2.0 1.8 1.6 1.4 Two high-energy cutoffs: exp (- γ/γ c1 ); γ c1 ~ 4σ, - independent of L; γ c1 ~ 10 <ε> 1.2 σ h 1.0 10 0 10 1 10 2 10 3 exp [-(γ/γ c2 ) 2 ]; γ c2 ~ 0.1 L/ρ 0 - independent of σ. γ c1 c1 10 4 10 3 10 2 L/ 0 = 25 L/ 0 = 50 L/ 0 = 100 L/ 0 = 200 L/ 0 = 400 c1 =4 σ 10 10 1 0 10 1 10 2 10 3 available voltage drop ε max ~ e E rec L ~ 0.1 e B 0 L (Hillas, extreme accelera>on) (ρ 0 = m e c 2 /e B 0 ) Large-system regime: (γ c1 < γ c2 ): L/ρ 0 > 40 σ 10 2 10 3 10 4 10 5 L/ 0 D. Uzdensky 5/8/2018 8 γ c2 c2 10 4 10 3 10 2 10 1 = 1000 = 300 = 100 = 30 = 10 =3 γ c2 =0.1L/ 0 L/ρ 0

Why is there a γ c 4σ cutoff? Cutoff comes from small laminar elementary interplasmoid layers at the bokom of the plasmoid hierarchy (marginally stable to tearing). ParQcles are accelerated in these layers but then become trapped inside plasmoids. Cerun et al. 2013 l Zenitani & Hoshino 2001 (ρ 0 =m e c 2 /e B 0 ) σ = B 02 /(4π nmc 2 ) δ Cutoff: γ c = e E rec l /m e c 2 0.1 e B 0 l /m e c 2 = 0.1 l /ρ 0. Layers are marginally stable to tearing à l ~ 100 δ. Layer thickness: δ ρ (<γ>) = <γ> ρ 0 (σ /3) ρ 0. Thus, l /ρ 0 100 δ/ρ 0 30 σ => γ 0 = 3 σ. Further parqcle acceleraqon is possible, e.g., in plasmoid mergers, but this 2nd-stage reconnecqon acceleraqon occurs with lower sigma and smaller L. D. Uzdensky 5/8/2018 9

Rela>vis>c e-i reconnec>on: Key PIC Sims Results I Werner et al., MNRAS 2018; arxiv:1612.04493 Systema%c 2D PIC study: (no guide field, m i /m e =1836) Energy par>>oning between electrons and ions (useful prescripqon for GRMHD models of BH accreqon flows) Reconnec>on rate: v in /c = E/B 0 ions ce V A B 0 electrons V A = c σ i B 0 4πn i m i c 2 + B 0 2 = c σ i 1+σ i D. Uzdensky 5/8/2018 10 σ i In semi-rela%vis%c case ions gain 3 %mes more energy than electrons.

Rela>vis>c e-i reconnec>on: Key PIC Sims Results II Par>cle Accelera>on: - electrons: - ions? Electron power-law index p and cutoff γ c : p e σ i Observed blazar p e ~2-3 imply σ i ~1, consistent with expectaqons from MHD jet models. γ c /σ i Werner et al. 2018 D. Uzdensky 5/8/2018 11 σ i

Kine>c Equa>on Key Ingredients: AcceleraQon by main reconnecqon electric field: - independent of γ MagneQzaQon by reconnected B-field (--> power-law): Trapping by large [w > ρ L (γ)] plasmoids (à cutoff): τ tr controlled by plasmoid distribuqon funcqon (below) D. Uzdensky 5/8/2018 12

Steady State Kine>c Equa>on Since γ acc is independent of γ, we get SoluQon: where D. Uzdensky 5/8/2018 13

Magne>za>on by Reconnected Field and NTPA power law EnergeQc parqcle passes right through small plasmoids. Distance a parqcle travels before being magneqzed l mag (γ) ~ρ L (γ, B 1 ) = (B 0 /B 1 ) ρ L (γ, B 0 ) = ε -1 ρ 0 γ magneqzaqon Qme-scale Balance magneqzaqon with acceleraqon in kineqc eqn: power-law soluqon f(γ) ~ γ -p power-law index: ultra-rel (σ h >>1): p à const (cf. Zenitani & Hoshino 2001) non-rel. case (σ h >>1): p ~ σ h -1/2 (c.f., Werner et al. 2018) D. Uzdensky 5/8/2018 14

Plasmoid Chain I: single power-law EnergeQc parqcles can be trapped in large plasmoids when w =w(γ) = ρ L (γ) = ρ 0 γ High-energy cutoff is controlled by plasmoid distribuqon funcqon F(w) = - dn/dw. τ tr = λ pl (w)/c where λ pl (w) is separaqon between plasmoids of size w: λ pl (w) = L/N(w) Thus τ tr = L/c N(w) (ρ 0 = m e c 2 /e B 0 ) D. Uzdensky 5/8/2018 15

Single-Power-law plasmoid chain Consider for illustraqon: F(w) ~ w -α for w < w max CumulaQve distribuqon: N(w) ~(w/w max ) 1-α [where N(w max ) =1] where γ max = w max /ρ 0 Special case α = 2: τ trap ~ γ (same as for magneqzaqon - later) Trapping rate overtakes magneqzaqon at For w max ~ εl: γ c ~ γ max D. Uzdensky 5/8/2018 16

Establishing Cutoff Balancing acceleraqon against trapping in plasmoids: Special case α ~ 1 (ignoring log-correcqons) where (can be < γ max, if β A < 1) Special case α=2: no cutoff but another power-law: For w max ~ εl: p ~ β A -1 (~same as without plasmoids) Combined with magneqzaqon: à steeper (by x2) power law. D. Uzdensky 5/8/2018 17

Plasmoid Chain II: Realis>c double-power-law Real simulaqons show double-power-law plasmoid distribuqons (Loureiro et al. 2012, Huang et al. 2013, Sironi et al. 2016, Petropoulou et al. 2018) For α 1 1: ~ γ c = w c /ρ 0 ~ γ c Most likely: α 1 1, α 2 2 Important QuesQon: What controls w c? If α 2 2: possible 2 nd (steeper) power law above spectral break at γ c D. Uzdensky 5/8/2018 18

Important Ques>on: What controls w c? Consider large-system regime: L >> δ ~ <ρ> ~ σ ρ 0 The plasmoid distribuqon break size w c may be anywhere between microscopic ~ σ ρ 0 and macroscopic ~ L. If w c ~ σ ρ 0, then γ c ~ σ, e.g., γ c 4σ (Werner et al. 2016) If w c ~ L, then γ c ~ L/ρ 0 -- extreme (Hillas) acceleraqon limit. D. Uzdensky 5/8/2018 19

Effect of Guide Magne>c Field (Werner & Uzdensky 2017 ApJL) Par>cle spectra for different B z /B 0 : L z /L x = 1 γ 2 f(γ) γ Par>cle accelera>on is nega>vely affected by strong guide field. Explana9on: Guide field s iner%a: Guide-field needs to be advected out of the layer with the plasma, so guide field s inerqa contributes B gz2 /4π to the enthalpy in the denominator of σ h : σ h,eff = B 02 /(B gz 2 + 4π nh) -- reduces in-plane V A, hence recn. ouƒlow speed, hence E rec D. Uzdensky 5/8/2018 20

Conclusions RelaQvisQc Nonthermal ParQcle AcceleraQon (NTPA) in reconnecqon is an interplay of: steady acceleraqon by reconnecqon electric field; checked by escape from acceleraqon zone: - (1) magneqzaqon by general reconnected magneqc field B 1 ~ 0.1 B 0 à power-law index p ~ (E rec /B 1 ) -1 ~ 1/ β A ~ [1+σ h )/σ h ] 1/2 - (2) capture/trapping by plasmoids with w ~ ρ L (γ) =γ ρ 0. à high-energy cutoff. - Cutoff depends on plasmoid-distribuqon funcqon, e.g., for α=1 it is simple exponenqal with γ c = w max /ρ 0. - RealisQc double-power-law F(w): cutoff at break size w c and - possible steeper power law (if α 2 2) above w c Guide field s inerqa B gz2 /4π adds to enthalpy, reduces effecqve σ h D. Uzdensky 5/8/2018 21