Particle Acceleration in the Magnetotail and Aurora

Birn, J.; Artemyev, А. V.; Baker, D. N.; Echim, Marius; Hoshino, Masahiro; Zelenyǐ, L. M.

doi:10.1007/978-1-4614-6455-6_3

Cited by 76 publications

(113 citation statements)

References 241 publications

Supporting

Mentioning

107

Contrasting

Order By: Relevance

“…Acceleration mechanisms in 3D kinetic simulations are less studied than in 2D, but are important for understanding how plasma is accelerated to high energies and which physical mechanisms regulate the dynamics of energetic particles during magnetotail magnetic reconnection (Birn and Priest 2007;Priest and Forbes 2007;Birn et al 2012). Our simulation results are in agreement with the results from previous simulations in 2D geometry and reduced physical models, corroborating previous studies in acceleration mechanisms in magnetic reconnection Egedal et al 2005).…”

Section: Introductionsupporting

confidence: 94%

“…in space, astrophysical and fusion device plasmas. In Earth magnetosphere, magnetic reconnection occurs in the magnetotail (Nagai et al 2001;Øieroset et al 2002a;Retinò et al 2008;Birn et al 2012;Nagai et al 2013) and in the dayside magnetopause (Sonnerup 1974;Daughton et al 2011). It regulates the exchange of energy and momentum between the solar wind and the inner magnetosphere.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Energetic particles in magnetotail reconnection

et al. 2014

View full text Add to dashboard Cite

We carried out a 3D fully kinetic simulation of Earth's magnetotail magnetic reconnection to study the dynamics of energetic particles. We developed and implemented a new relativistic particle mover in iPIC3D, an implicit Particle-inCell code, to correctly model the dynamics of energetic particles. Before the onset of magnetic reconnection, energetic electrons are found localized close to current sheet and accelerated by lower hybrid drift instability. During magnetic reconnection, energetic particles are found in the reconnection region along the x-line and in the separatrices region. The energetic electrons are first present in localized stripes of the separatrices and finally cover all the separatrix surfaces. Along the separatrices, regions with strong electron deceleration are found. In the reconnection region, two categories of electron trajectory are identified. First, part of the electrons are trapped in the reconnection region, bouncing a few times between the outflow jets. Second, part of the electrons pass the reconnection region without being trapped. Different from electrons, energetic ions are localized on the reconnection fronts of the outflow jets.

show abstract

Section: Introductionsupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Energetic particles in magnetotail reconnection

et al. 2014

View full text Add to dashboard Cite

show abstract

“…Rapid reconnection of magnetic fields of different topologies may happen in spontaneous current sheets or be due to an external driving force (see, e.g., Zweibel and Yamada 2009). Mechanisms of direct acceleration of charged particles by the reconnecting magnetic field were studied in detail both analytically and numerically (see, e.g., Zelenyi et al 1990, Hoshino 2005, Birn and Priest 2007, Drake et al 2006, Pritchett 2006, Lazarian and Opher 2009, Artemyev et al 2013, Birn et al 2012.…”

Section: Particle Acceleration and Non-thermal Radiation In Starburstmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

111

102

View full text Add to dashboard Cite

Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

show abstract

“…On top of the mean electric field variation, fluctuations on short timescales also are observed, as examined for instance by Nosé et al (2014). Under the effect of these large induced electric fields, ions may be subjected to prominent acceleration as examined in a variety of studies (e.g., Delcourt et al, 1990;Zhou et al, 2010;Ukhorskyi et al, 2013;Artemyev and Vasiliev, 2015; see review by Birn et al, 2012).…”

Section: Introductionmentioning

confidence: 99%

On the response of quasi-adiabatic particles to magnetotail reconfigurations

2017

View full text Add to dashboard Cite

Abstract. We investigate the response of quasi-adiabatic particles to dynamical reconfigurations of the magnetotail field lines. Although they travel through a sharp field reversal with a characteristic length scale smaller than their Larmor radii, these quasi-adiabatic particles experience a negligible net change in magnetic moment. We examine the robustness of such a quasi-adiabatic behavior in the presence of a large surging electric field induced by magnetic field line reconfiguration as observed during the expansion phase of substorms. We demonstrate that, although such a short-lived electric field can lead to substantial nonadiabatic heating, quasi-adiabaticity is conserved for particles with velocities larger than the peak ExB drift speed. Because of the timevarying character of the magnetic field, it is not possible to use the adiabaticity parameter κ in a straightforward manner to characterize the particle behavior. We rather consider a κ parameter that is averaged over equatorial crossings. We demonstrate that particles intercepting the field reversal in the early stage of the magnetic transition may experience significant energization and enhanced oscillating motion in the direction normal to the midplane. In contrast, particles interacting with the field reversal in the late stage of the magnetic transition experience weaker energization and slower oscillations about the midplane. We show that quasi-adiabatic particles accelerated during such events can lead to energy-time dispersion signatures at low altitudes as is observed in the plasma sheet boundary layer.

show abstract

Particle Acceleration in the Magnetotail and Aurora

Cited by 76 publications

References 241 publications

Energetic particles in magnetotail reconnection

Energetic particles in magnetotail reconnection

Nonthermal particles and photons in starburst regions and superbubbles

On the response of quasi-adiabatic particles to magnetotail reconfigurations

Contact Info

Product

Resources

About