scholarly journals 3D hybrid simulations of the interaction of a magnetic cloud with a bow shock

2015 ◽  
Vol 120 (8) ◽  
pp. 6133-6151 ◽  
Author(s):  
L. Turc ◽  
D. Fontaine ◽  
P. Savoini ◽  
R. Modolo
Keyword(s):  
Magnetic Cloud ◽  
Bow Shock ◽  
Hybrid Simulations

A magnetic cloud with unusual structure and bow shock movement observed on May 13, 1995

2000 ◽  
Vol 25 (7-8) ◽  
pp. 1397-1400
Author(s):  
T Takeuchi ◽  
T Araki ◽  
R.P Lepping ◽  
T Mukai ◽  
Y Saito ◽  
...  
Keyword(s):  
Magnetic Cloud ◽  
Bow Shock ◽  
Unusual Structure

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 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.

scholarly journals Ion distribution dynamics near the Earth's bow shock: first measurements with the 2D ion energy spectrometer CORALL on the INTERBALL/Tail-probe satellite

1997 ◽  
Vol 15 (5) ◽  
pp. 533-541 ◽  
Author(s):  
Yu. I. Yermolaev ◽  
A. O. Fedorov ◽  
O. L. Vaisberg ◽  
V. M. Balebanov ◽  
Yu. A. Obod ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Bow Shock ◽  
Time Interval ◽  
Angle Distribution ◽  
Ion Distribution ◽  
Ion Energy ◽  
The Earth ◽  
Earth’S Bow Shock ◽  
Tail Probe

Abstract. The dynamics of the ion distribution function near the Earth's bow shock is studied on the basis of quasi-3D measurements of ion energy spectra in the range of 30–24200 eV/q with the Russian-Cuban CORALL instrument on the INTERBALL/Tail-probe satellite. The instrument was designed for observations of magnetospheric plasma and measures ions, in an angular range of 36°–144° from the Earth-Sun direction. Ion populations generated by the Earth bow shock are often observed upstream from the bow shock. In the solar-wind stream compressed and heated by the passing of very dense magnetic cloud (CME), two types of these ion populations were measured upstream and before the bow shock crossing on 25 August 1995 at 07:37 UT. Both populations were observed in the energy range above 2 keV. At ~06:20 UT, when the angle between the direction of the interplanetary magnetic field and normal to the bow shock VBn was ≃ 43° the instrument observed a narrow, fast (~800 km/s) field-aligned beam moving from the Earth. At ~07:30, when <vartheta>Bn ≃ 28°, the wide ion pitch-angle distribution was observed. A similar suprathermal ion population is observed in the magnetosheath simultaneously with the solar-wind ion population being heated and deflected from the Sun-Earth direction. The similarity of observations during the mentioned time-interval and under usual solar-wind conditions allows us to conclude that types of suprathermal ion populations upstream and downstream from the bow shock do not depend on the solar-wind disturbance generated by magnetic cloud.

scholarly journals Rosetta swing-by at Mars – an analysis of the ROMAP measurements in comparison with results of 3-D multi-ion hybrid simulations and MEX/ASPERA-3 data

2009 ◽  
Vol 27 (6) ◽  
pp. 2383-2398 ◽  
Author(s):  
A. Boesswetter ◽  
U. Auster ◽  
I. Richter ◽  
M. Fränz ◽  
B. Langlais ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Measurements ◽  
Bow Shock ◽  
Gravity Assist ◽  
Pile Up ◽  
Magnetic Field Model ◽  
Order Of Magnitude ◽  
Upstream Waves ◽  
Insight Into ◽  
Hybrid Simulations

Abstract. The Rosetta spacecraft flew by Mars at a distance of 260 km on 25 February 2007 during a gravity assist manoeuvre. During the closest approach (CA) the lander magnetometer ROMAP was switched on. The dataset taken during this swingby provides insight into the plasma environment around Mars: in addition to a pronounced bow shock crossing Rosetta recorded the signature of the pile up region of draped magnetic field. Also the Rosetta measurements showed signatures of crustal magnetic field anomalies which can be verified by results of a crustal magnetic field model. In order to understand the measured field morphology, multi-ion hybrid simulations were performed. Some of the input parameters for the simulations were obtained from Mars Express (MEX) data which were contemporaneously collected during the Rosetta swingby. These simulations reproduces ROMAP magnetic field measurements and show that the interplanetary magnetic field pointed northward during the encounter. A spectral analysis shows upstream waves ahead of the bow shock and indicates the presence of the magnetic pile-up boundary (MPB). The multi-ion model reproduces the ion fluxes measured by MEX/ASPERA-3 and is in agreement with the measurements to within one order of magnitude.

A study of kinematic relaxation at the Venus bow shock

2020 ◽  
Author(s):  
Simon A. Pope ◽  
Michael A. Balikhin
Keyword(s):  
Magnetic Field ◽  
Mach Number ◽  
Heavy Ions ◽  
Magnetic Cloud ◽  
Bow Shock ◽  
Primary Method ◽  
Low Mach Number ◽  
The Earth ◽  
New Type ◽  
Venus Express

&lt;p&gt;A new type of very-low Mach number shock in which the primary method of energy re-distribution is the kinematic relaxation of a non-gyrotropic ion population, was discovered at Venus early in the Venus Express mission. This led to the development of an associated theory and numerical analysis. The recent discovery of such a shock at the Earth using THEMIS data experimentally verified this theory using simultaneous magnetic field and plasma data. It also showed that the most favourable conditions for the formation of such a shock is the magnetic cloud phase of an ICME. Venus Express provides an excellent opportunity to study such shocks further. Here we present results from the duration of the mission, which identifies over thirty shock crossings showing evidence of kinematic relaxation. These shock crossings are investigated to understand how the upstream conditions and heavy ions (including pick-up ions) affect their formation.&lt;/p&gt;

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