March 28th 2017 - Annual NewCompstar Conference, Warsaw (Poland) Pulsar Magnetosphere: a New View from PIC Simulations Gabriele Brambilla NASA Goddard Space Flight Center (MD-USA) - Università degli Studi di Milano (Italy) I’m a PhD student and I work with: My Italian supervisor is: Pierre Pizzochero Kostas Kalapotharakos Andrey Timokhin Alice Harding Demos Kazanas Many of the figures are obtained using VisIt - Childs et al. 2012
Pulsars are expected to have a magnetosphere because their strong magnetic field overcomes gravity PULSAR B
Pulsars are expected to have a magnetosphere because their strong magnetic field overcomes gravity Ω PULSAR B
Pulsars are expected to have a magnetosphere because their strong magnetic field overcomes gravity inclination angle Ω PULSAR B
Pulsars are expected to have a magnetosphere because their strong magnetic field overcomes gravity inclination angle Ω E PULSAR B
Pulsars are expected to have a magnetosphere because their strong magnetic field overcomes gravity inclination angle Ω E PULSAR B Goldreich and Julian 1969
Pulsars behaves like a dynamo; currents dissipate, emitting light when particles are accelerated www.physicsforums.com Google images
Pulsars behaves like a dynamo; currents dissipate, emitting light when particles are accelerated www.physicsforums.com Google images
Pulsars behaves like a dynamo; currents dissipate, emitting light when particles are accelerated www.physicsforums.com Google images Particle’s acceleration produces light E · B ≠ 0 -> dissipation/resitivity
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° Contopoulos et al. 1999
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° Contopoulos et al. 1999 Magnetic reconnection see Magnetic Reconnection , by Priest & Forbes, 2000
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° Contopoulos et al. 1999 Magnetic reconnection see Magnetic Reconnection , by Priest & Forbes, 2000
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° inc. angle 60° Contopoulos et al. 1999 Spitkovsky 2006 Magnetic reconnection see Magnetic Reconnection , by Priest & Forbes, 2000
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° inc. angle 60° Contopoulos et al. 1999 Spitkovsky 2006 Magnetic reconnection see Magnetic Reconnection , by Priest & Forbes, 2000
Force-free simulations highlighted the presence of a current sheet, where particles could be accelerated by magnetic reconnection inc. angle 0° inc. angle 60° Contopoulos et al. 1999 Spitkovsky 2006 Magnetic reconnection see Magnetic Reconnection , by Priest & Forbes, 2000
Dissipative solutions also point to the current sheet for reproducing the emission of the gamma-ray pulsars Vela AKA J0835-4510 Abdo et al 2013
Dissipative solutions also point to the current sheet for reproducing the emission of the gamma-ray pulsars Vela AKA J0835-4510 Abdo et al 2013
Dissipative solutions also point to the current sheet for reproducing the emission of the gamma-ray pulsars Vela AKA J0835-4510 Abdo et al 2013
Dissipative solutions also point to the current sheet for reproducing the emission of the gamma-ray pulsars Vela AKA J0835-4510 Abdo et al 2013
Dissipative solutions also point to the current sheet for reproducing the emission of the gamma-ray pulsars Vela AKA J0835-4510 Brambilla et al 2015 Abdo et al 2013 Kalapotharakos et al 2014
In PIC codes, particles moved by the fields form the currents that act on the fields themselves
In PIC codes, particles moved by the fields form the currents that act on the fields themselves
In PIC codes, particles moved by the fields form the currents that act on the fields themselves
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill)
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill)
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill)
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill)
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill)
In PIC codes, particles moved by the fields form the currents that act on the fields themselves Birdsall & Langdon 1985 Plasma Physics via Computer Simulation (New York: McGraw-Hill) Pulsar & PIC Chen et al. 2014, Philippov et al. 2014, Belyaev 2015
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total IR 1GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total Force Free IR 1GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 1GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 1GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 1GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 10GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 20 GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 30 GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 40 GJ Kalapotharakos et al 2017 (in prep.)
With our PIC code we reproduced the force free limit once we inject enough particles everywhere J total PIC Force Free IR 50 GJ Kalapotharakos et al 2017 (in prep.)
We verified that the force free limit is well defined energetically FF PIC normalized Poynting flux Radius (RLC) Kalapotharakos et al 2017 (in prep.)
We verified that the force free limit is well defined energetically FF PIC normalized Poynting flux Radius (RLC) FF electrodynamics normalized Poynting flux Kalapotharakos et al 2017 (in prep.) Radius (RLC)
We verified that the force free limit is well defined energetically FF PIC Electromagnetic Energy Average Electromagnetic Energy density normalized Poynting flux [arbitrary units] FF electrodynamics approach Radius (RLC) FF electrodynamics normalized Injection Rate (GJ flux) Poynting flux Kalapotharakos et al 2017 (in prep.) Radius (RLC)
With PIC we can explore the different contribution to the currents of the different species J electrons J positrons Kalapotharakos et al 2017 (in prep.)
Tracking individual trajectories we see that the particles are accelerated in the current sheet
Tracking individual trajectories we see that the particles are accelerated in the current sheet
Tracking individual trajectories we see that the particles are accelerated in the current sheet
Tracking individual trajectories we see that the particles are accelerated in the current sheet
Tracking individual trajectories we see that the particles are accelerated in the current sheet
With a 3D pic code we can simulate pulsars with an arbitrary inclination angle 0° 30° ∇ E ∇ E [arbitrary] [arbitrary] 60° 85° ∇ E ∇ E [arbitrary] [arbitrary]
Different injection rates, periods and surface fields cover the range of cutoff energies and luminosities of the Fermi pulsar population [erg] [ev] 15 ° 75 ° PIC: different inclination angle and injection rate 45 ° FERMI gamma ray pulsars Kalapotharakos et al 2017 (in prep.)
We also obtained the force free limit injecting particles only from the surface and the current composition looks different All volume injection star surface injection J total Brambilla et al 2017 (in prep.)
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