the global pulsar magnetosphere

Slides:

Advertisements

Similar presentations

Energy stored in Magnetic Fields

Advertisements

IAUS291 Beijing 24 Aug IAUS291 Beijing 24 Aug 2012.

Neutron Stars. Gradual compression of a stellar iron core  trans. [g cm -3 ] CompositionDegen. pressure Remarks Iron nuclei; nonrel. free e - nonrel.

Maxwell’s Equations The two Gauss’s laws are symmetrical, apart from the absence of the term for magnetic monopoles in Gauss’s law for magnetism Faraday’s.

AP Physics C Montwood High School R. Casao

Electromagnetic Waves

AS 4002 Star Formation & Plasma Astrophysics BACKGROUND: Maxwell’s Equations (mks) H (the magnetic field) and D (the electric displacement) to eliminate.

Pulsar High Energy Emission Models: What Works and What Doesn't “Standard” outer magnetosphere models - successes Shortcomings of the models Next steps?

Example: A negatively charged rod, of length l, has a total charge Q and is a distance b from a point P. The charge is uniformly distributed along the.

Study on polarization of high- energy photons from the Crab pulsar 〇 J. Takata (TIARA-NTHU/ASIAA,Taiwan) H.-K. Chang (NTH Univ., Taiwan) K.S. Cheng (HK.

Pulsars Basic Properties. Supernova Explosion => Neutron Stars part of angular momentum carried away by shell field lines frozen into solar plasma (surface.

The Phase-Resolved Spectra of the Crab Pulsar Jianjun Jia Jan 3, 2006.

Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions –Formation of elements (R, S process) –Neutron stars –Pulsars Formation of X-Ray.

State Assessment Review Physical Science S.HS.2B.3.5.

Earth’s Radiation Belt Xi Shao Department of Astronomy, University Of Maryland, College Park, MD

Neutron Stars and Black Holes PHYS390: Astrophysics Professor Lee Carkner Lecture 18.

Pei-Chun Hsu¹, Kouichi Hirotani², and Hsiang-Kuang Chang¹ 1 Department of Physics and Institute of Astronomy, National Tsing Hua University ASIAA/National.

A THREE-DIMENSIONAL OUTER MAGETOSPHERIC MODEL FOR GAMMA-RAY PULSARS : GEOMETRY, PAIR PRODUCTION, EMISSION MORPHOLOGIES, AND PHASE- RESOLVED SPECTRA K.S.CHENG,

A brief introduction- Outer gap model of r-ray pulsar Department of Physics National Tsing Hua University Lun-Wen Yeh

Magnetic reconnection at the termination shock in a striped pulsar wind Yuri Lyubarsky Ben-Gurion University, Israel In collaboration with: Jerome Petri.

Gamma-ray emission mechanism in pulsar magnetosphere – electrodynamics and models 徐佩君清大天文所.

Four equations (integral form) : Gauss’s law Gauss’s law for magnetism Faraday’s law Ampere-Maxwell law + Lorentz force Maxwell’s Equations.

Experimental Measurement of the Charge to Mass Ratio of the Electron Stephen Luzader Physics Department Frostburg State University Frostburg, MD.

Jaypee Institute of Information Technology University, Jaypee Institute of Information Technology University,Noida Department of Physics and materials.

Charged Particles In Circular Orbits

＠ FAN3 22 June To give the theoretical proof of the outer gap (the mechanism has been proposed) 2.To look for other particle acceleration sites;

Qiao,G.J. Dept. of Astronomy, Peking Univ. Collaborators: Zhang, B.( University of Nevada ), Xu, R.X.(PKU), Han,J.L.(NAOC), Lin,W.P.(SHO),Lee,K.J.(PKU)

Relativistic Outflow Formation by Magnetic Field around Rapidly Rotating Black Hole Shinji Koide （ Toyama University ） Black Hole 2003, October 29 (Wed),

P212c28: 1 Chapter 28: Magnetic Field and Magnetic Forces Iron ore found near Magnesia Compass needles align N-S: magnetic Poles North (South) Poles attracted.

Computational Model of Energetic Particle Fluxes in the Magnetosphere Computer Systems Yu (Evans) Xiang Mentor: Dr. John Guillory, George Mason.

Definition of physics the science of matter and energy and their interactions.

Book Reference : Pages To understand how to generate electricity using electromagnetic induction 2.To be able to establish the relative direction.

Chapter 32 Maxwell’s Equations Electromagnetic Waves.

Introduction A pulsar magnetosphere can be divided into two zones: The closed zone filled with a dense plasma co-rotating with the neutron star (NS), and.

IMPRS Lindau, Space weather and plasma simulation Jörg Büchner, MPAe Lindau Collaborators: B. Nikutowski and I.Silin, Lindau A. Otto, Fairbanks.

Non-Ideal MHD Structure of Pulsar Magnetospheres C. Kalapotharakos 1,2, D. Kazanas 1, A. Harding 1, I. Contopoulos 3 1 Astrophysics Science Division, NASA/Goddard.

The structure of the pulsar magnetosphere via particle simulation Shinpei Shibata (1), Shinya Yuki (1), Tohohide Wada (2),Mituhiro Umizaki (1) (1)Department.

Polarization of Light.

Charging a Capacitor (instantaneous application of Kirchhoff’s rules to non-steady-state situation) Use lower case v, i, q to denote time-varying voltage,

After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008.

Parallel Plates.

The Structure of the Pulsar Magnetosphere via Particle Simulation S. Shibata (1), T. Wada (2), S. Yuki (3), and M. Umizaki (3) (1)Department of Phys.Yamagata.

Particle Acceleration by Relativistic Collisionless Shocks in Electron-Positron Plasmas Graduate school of science, Osaka University Kentaro Nagata.

Multiple Sheet Beam Instability of Current Sheets in Striped Relativistic Winds Inertial Parallel E in Neutron Star Magnetospheres: Return Cuurent Sheets.

Multiple Sheet Beam Instability of Current Sheets in Striped Relativistic Winds Jonathan Arons University of California, Berkeley 1.

Ускорение частиц вблизи массивных черных дыр Я.Н. Истомин ФИАН HEA 07.

Gamma-Ray Emission from Pulsars

A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.

Magnetized Shocks & Prompt GRB Emission

the global pulsar magnetosphere

PHYSICS 272 Electric & Magnetic Interactions

Pulsars: the Magnetosphere and the γ-ray emission

Observation of Pulsars and Plerions with MAGIC

The structure of the pulsar magnetosphere via particle simulation

Office: Science Bldg, Rm 137

Basic Properties By Dr. Lohse, University of Berlin

Inclined Pulsar Magnetospheres in General Relativity:

Magnetohydrodynamics of pulsar winds and plerions

Middleweight Stars 4-12 solar masses.

Edison Liang, Koichi Noguchi Orestes Hastings, Rice University

Magnetic Field Permanent magnet Charges in motion

Earth’s Ionosphere Lecture 13

Scattering by free charges

Phys102 Lecture 6 Electric Potential

Chapter 17, Section 1 and 2: Nature of Electromagnetic Waves

Intense Coherent Emission in Relativistic Shocks

ICRC2003 OG Calculation of Cosmic-Ray Proton and Anti-proton Spatial Distribution in Magnetosphere Michio Fuki, Ayako Kuwahara, Nozomi, Sawada Faculty.

Can we probe the Lorentz factor of gamma-ray bursts from GeV-TeV spectra integrated over internal shocks ? Junichi Aoi　(YITP, Kyoto Univ.) co-authors:

Magnetic Field Permanent magnet Charges in motion

G. A. Krafft Jefferson Lab Old Dominion University Lecture 1

Presentation transcript:

the global pulsar magnetosphere Particle simulations of the global pulsar magnetosphere Shinpei Shibata Department of Phys. Yamagata University shibata@sci.kj.yamagata-u.ac.jp Collaborators: Tomohide Wada and Shinya Yuki School of Science and Technology, Yamagata University

Rotation Power Pulsar wind magnetosphere Beamed radiation (gamma-ray) Bulk acceleration, MHD Kinetic energy + Poynting energy Beamed radiation (gamma-ray) Particle acceleration by E// magnetosphere How two distinctive accelerations take place in the same magnetosphere. Axisymmetric steady model GRAPE-6@nao.jp Special purpose computer for Astrononomical N-body Problem

Pulsar Nebula Pulsar e+e- Wind Observational facts:　Gaps and Wind High energy and radio pulsed emissions Gamma-ray pulses Pulsar Wind Polar Cap e+e- Outer Gap Pulsar Nebula Aim of particle simulation Particle accelerator (～1013eV) in the magnetosphere and pulsar wind (γ～106 in bulk motion with Poynting flux)

Prospect: basic physics Let us consider what happens around the rotating neutron star in the vacuum space.

Method of Solution 5. Free emission of particles We iteratively solve the Maxwell equations and equation of motion with 1. Fields being axisymmetry, and steady: 2. Source magnetic field is dipole 3. the star is a perfect conductor, i.e., BC: 4. equation of motion with drag force 5. Free emission of particles 6. Pair creation if E//>Ec Radiation reaction Creation rate = factor x (E// /Ec) 7. Initial state: a star in vacuum

magnetic field pair creation Step -1 dipole no Step -2 Yes (low rate) Step -3 Modification by J (high rate)

Result（１） Gap Formation Step-1 Dipole field + no-pair creation Magnetic field lines electrons Light cylinder star positrons

Result（１） Gap Formation Step-1 Dipole field + no-pair creation The final state is static clouds with the gaps (Krause-Polstorf and Michel 1985). Light cylinder electrons Field-aligned Electric field Gap Gap star positrons

Result（2） Pair Creating Gap + wind Map of field-aligned electric field electrons Particle distribution 粒子分布 positrons Outer gap Outer Gap : pair creating region with E// Outflow (equal amount of electrons and positrons are lost from the magnetosphere. Both Gaps and wind are formed ! 9

Result（3） Pair Creating Gap + wind + magnetic field modification Map of E/B Magnetic field Diple field Open magnetic flux Dissipataive Current sheet E>B Udzdensky 2003

summary Strong charge separation by emf of the star produces the outer gaps. The gaps persist and create pairs providing the particle source of the pulsar wind. If pair creation rate is high, then magnetic field is opened and pairs flow out along the open magnetic flux. This is the pulsar wind. If pair creation rate is low, then the wind is moderate, and some particles circulate in the magnetosphere with strong radiation drag (high Lorentz factor).