Global hybrid simulations of interaction between interplanetary rotational discontinuity and bow shock/magnetosphere: Can ion‐scale magnetic reconnection be driven by rotational discontinuity downstream of quasi‐parallel shock?

2021 ◽  
Author(s):  
Zhifang Guo ◽  
Yu Lin ◽  
Xueyi Wang
Keyword(s):  
Magnetic Reconnection ◽  
Bow Shock ◽  
Rotational Discontinuity ◽  
Hybrid Simulations

scholarly journals Switch-off slow shock/rotational discontinuity structures in collisionless magnetic reconnection: What to look for in satellite observations

2017 ◽  
Vol 44 (8) ◽  
pp. 3447-3455 ◽  
Author(s):  
M. E. Innocenti ◽  
E. Cazzola ◽  
R. Mistry ◽  
J. P. Eastwood ◽  
M. V. Goldman ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Satellite Observations ◽  
Slow Shock ◽  
Rotational Discontinuity

scholarly journals Magnetic reconnection and kinetic waves generated in the Earth's quasi-parallel bow shock

2020 ◽  
Vol 27 (9) ◽  
pp. 092901
Author(s):  
N. Bessho ◽  
L.-J. Chen ◽  
S. Wang ◽  
M. Hesse ◽  
L. B. Wilson ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Bow Shock

scholarly journals Interaction of rotational discontinuities with energetic ions in the precursor of the Earth’s bow shock

2021 ◽  
Vol 2103 (1) ◽  
pp. 012015
Author(s):  
Julia A Kropotina ◽  
Anton V. Artemyev ◽  
Andrei M. Bykov ◽  
Dmitri L. Vainchtein
Keyword(s):  
Solar Wind ◽  
Energetic Particles ◽  
Bow Shock ◽  
Growing Up ◽  
Whistler Waves ◽  
Energetic Ions ◽  
Strongly Coupled ◽  
Earth’S Bow Shock ◽  
Hybrid Simulations

Abstract We combined in-situ solar wind observations by ARTEMIS and MMS missions with kinetic hybrid simulations to study the interaction of solar wind rotational discontinuities (RDs) with the foreshock of the Earth’s bow shock. We found that whistler modes excited by diffuse energetic particles were strongly coupled with RDs and lead to their temporary dissociation. At the same time, RDs trigger the steepening of whistler waves and the generation of ’shocklets’ - small localised shock-like structures, capable of trapping energetic particles and growing up by absorbing the particles energy.

scholarly journals Observational Evidence of Magnetic Reconnection in the Terrestrial Foreshock Region

2021 ◽  
Vol 922 (1) ◽  
pp. 56
Author(s):  
K. Jiang ◽  
S. Y. Huang ◽  
H. S. Fu ◽  
Z. G. Yuan ◽  
X. H. Deng ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Direct Evidence ◽  
Bow Shock ◽  
Shock Acceleration ◽  
Diffusive Shock Acceleration ◽  
Strong Energy ◽  
Magnetospheric Multiscale ◽  
Electron Distributions ◽  
Magnetospheric Multiscale Mission ◽  
The Magnetic Field

Abstract Electron heating/acceleration in the foreshock, by which electrons may be energized beyond thermal energies prior to encountering the bow shock, is very important for the bow shock dynamics. And then these electrons would be more easily injected into a process like diffusive shock acceleration. Many mechanisms have been proposed to explain electrons heating/acceleration in the foreshock. Magnetic reconnection is one possible candidate. Taking advantage of the Magnetospheric Multiscale mission, we present two magnetic reconnection events in the dawnside and duskside ion foreshock region, respectively. Super-Alfvénic electron outflow, demagnetization of the electrons and the ions, and crescent electron distributions in the plane perpendicular to the magnetic field are observed in the sub-ion-scale current sheets. Moreover, strong energy conversion from the fields to the plasmas and significant electron temperature enhancement are observed. Our observations provide direct evidence that magnetic reconnection could occur in the foreshock region and heat/accelerate the electrons therein.

scholarly journals Aspects of solar wind interaction with Mars: comparison of fluid and hybrid simulations

2007 ◽  
Vol 25 (1) ◽  
pp. 145-159
Author(s):  
N. V. Erkaev ◽  
A. Bößwetter ◽  
U. Motschmann ◽  
H. K. Biernat
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Hybrid Model ◽  
Field Enhancement ◽  
Bow Shock ◽  
Solar Wind Interaction ◽  
Plasma Parameters ◽  
Physical Reason ◽  
The Magnetic Field ◽  
Hybrid Simulations

Abstract. Mars has no global intrinsic magnetic field, and consequently the solar wind plasma interacts directly with the planetary ionosphere. The main factors of this interaction are: thermalization of plasma after the bow shock, ion pick-up process, and the magnetic barrier effect, which results in the magnetic field enhancement in the vicinity of the obstacle. Results of ideal magnetohydrodynamic and hybrid simulations are compared in the subsolar magnetosheath region. Good agreement between the models is obtained for the magnetic field and plasma parameters just after the shock front, and also for the magnetic field profiles in the magnetosheath. Both models predict similar positions of the proton stoppage boundary, which is known as the ion composition boundary. This comparison allows one to estimate applicability of magnetohydrodynamics for Mars, and also to check the consistency of the hybrid model with Rankine-Hugoniot conditions at the bow shock. An additional effect existing only in the hybrid model is a diffusive penetration of the magnetic field inside the ionosphere. Collisions between ions and neutrals are analyzed as a possible physical reason for the magnetic diffusion seen in the hybrid simulations.

Turbulence-driven magnetic reconnection in the magnetosheath downstream of a quasi-parallel shock：a three-dimensional global hybrid simulation

2020 ◽  
Author(s):  
Quanming Lu ◽  
Huanyu Wang ◽  
Xueyi Wang
Keyword(s):  
Magnetic Reconnection ◽  
Electromagnetic Waves ◽  
High Speed ◽  
Three Dimensional ◽  
Hybrid Simulation ◽  
Bow Shock ◽  
Ion Flow ◽  
Current Sheets ◽  
The Earth ◽  
Outflow Region

<p>Satellite observations with high-resolution measurements have demonstrated the existence of intermittent current sheets and occurrence of magnetic reconnection in a quasi-parallel magnetosheath behind the terrestrial bow shock. In this Letter, by performing a three-dimensional (3-D) global hybrid simulation, we investigated the characteristics of the quasi-parallel magnetosheath of the bow shock, which is formed due to the interaction of the solar wind with the earth’s magnetosphere. Current sheets with widths of several ion inertial lengths are found to be produced in the magnetosheath after the upstream large amplitude electromagnetic waves penetrate through the shock and are then compressed in the downstream. Magnetic reconnection consequently occurs in these current sheets, where high-speed ion flow jets are identified in the outflow region. Simultaneously, flux ropes with the extension (along the   direction) of about several earth’s radii are also observed. Our simulation shed new insight on the mechanism for the occurrence of magnetic reconnection in the quasi-parallel shocked magnetosheath.</p>

Sign in / Sign up

Export Citation Format

Share Document