639 research outputs found
Triggering an aurora
Ambient ionospheric electron density studied as triggering mechanism of aurora
A limit on stably trapped particle fluxes
Limits of stably trapped particle fluxes - behavior of Whistler and ion cyclotron noise mode
Investigation of magnetospheric physics Technical status report, period ending 31 Mar. 1967
Magnetospheric physics - auroral zone structur
Fan-shaped jets in three dimensional reconnection simulation as a model of ubiquitous solar jets
Magnetic reconnection is a fundamental process in space and astrophysical
plasmas in which oppositely directed magnetic fields changes its connectivity
and eventually converts its energy into kinetic and thermal energy of the
plasma. Recently, ubiquitous jets (for example, chromospheric anemone jets,
penumbral microjets, umbral light bridge jets) have been observed by Solar
Optical Telescope on board the satellite Hinode. These tiny and frequently
occurring jets are considered to be a possible evidence of small-scale
ubiquitous reconnection in the solar atmosphere. However, the details of three
dimensional magnetic configuration are still not very clear. Here we propose a
new model based on three dimensional simulations of magnetic reconnection using
a typical current sheet magnetic configuration with a strong guide field. The
most interesting feature is that the jets produced by the reconnection
eventually move along the guide field lines. This model provides a fresh
understanding of newly discovered ubiquitous jets and moreover a new
observational basis for the theory of astrophysical magnetic reconnection.Comment: 11 pages, 4 figures, Accepted for publication in The Astrophysical
Journal Letter
Experiments with Magnetohydrodynamically Supported Shock Layers
Shock tube experiments to determine interaction of hypersonic flow with magnetic fiel
Gamma-burst emission from neutron-star accretion
A model for emission of the hard photons of gamma bursts is presented. The model assumes accretion at nearly the Eddington limited rate onto a neutron star without a magnetic field. Initially soft photons are heated as they are compressed between the accreting matter and the star. A large electric field due to relatively small charge separation is required to drag electrons into the star with the nuclei against the flux of photons leaking out through the accreting matter. The photon number is not increased substantially by Bremsstrahlung or any other process. It is suggested that instability in an accretion disc might provide the infalling matter required
Resistive Magnetohydrodynamic Simulations of Relativistic Magnetic Reconnection
Resistive relativistic magnetohydrodynamic (RRMHD) simulations are applied to
investigate the system evolution of relativistic magnetic reconnection. A
time-split Harten--Lan--van Leer method is employed. Under a localized
resistivity, the system exhibits a fast reconnection jet with an Alfv\'{e}nic
Lorentz factor inside a narrow Petschek-type exhaust. Various shock structures
are resolved in and around the plasmoid such as the post-plasmoid vertical
shocks and the "diamond-chain" structure due to multiple shock reflections.
Under a uniform resistivity, Sweet--Parker-type reconnection slowly evolves.
Under a current-dependent resistivity, plasmoids are repeatedly formed in an
elongated current sheet. It is concluded that the resistivity model is of
critical importance for RRMHD modeling of relativistic magnetic reconnection.Comment: published in ApJ
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