The solar wind interaction with Mars: Locations and shapes of the bow shock and the magnetic pile-up boundary from the observations of the MAG/ER Experiment onboard Mars Global Surveyor

2000 ◽  
Vol 27 (1) ◽  
pp. 49-52 ◽  
Author(s):  
D. Vignes ◽  
C. Mazelle ◽  
H. Rme ◽  
M. H. Acuña ◽  
J. E. P. Connerney ◽  
...  
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Mars Global Surveyor ◽  
Solar Wind Interaction ◽  
Pile Up

scholarly journals Simulated solar wind plasma interaction with the Martian exosphere: influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary

2006 ◽  
Vol 24 (12) ◽  
pp. 3403-3410 ◽  
Author(s):  
R. Modolo ◽  
G. M. Chanteur ◽  
E. Dubinin ◽  
A. P. Matthews
Keyword(s):  
Solar Wind ◽  
Reasonable Agreement ◽  
Solar Wind Plasma ◽  
Bow Shock ◽  
Species Hybrid ◽  
Mars Global Surveyor ◽  
Neutral Species ◽  
Plasma Interaction ◽  
Pile Up ◽  
Weakly Dependent

Abstract. The solar wind plasma interaction with the Martian exosphere is investigated by means of 3-D multi-species hybrid simulations. The influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary is examined by comparing two simulations describing the two extreme states of the solar cycle. The hybrid formalism allows a kinetic description of each ions species and a fluid description of electrons. The ionization processes (photoionization, electron impact and charge exchange) are included self-consistently in the model where the production rate is computed locally, separately for each ionization act and for each neutral species. The results of simulations are in a reasonable agreement with the observations made by Phobos 2 and Mars Global Surveyor spacecraft. The position of the bow shock and the magnetic pile-up boundary is weakly dependent of the solar EUV flux. The motional electric field creates strong asymmetries for the two plasma boundaries.

Modulation of the solar wind driven ion escape from unmagnetized planets by ultra-low-frequency foreshock waves in a global hybrid simulation

2020 ◽  
Author(s):  
Riku Jarvinen ◽  
Esa Kallio ◽  
Tuija Pulkkinen
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Low Frequency ◽  
Hybrid Simulation ◽  
Bow Shock ◽  
Upstream Region ◽  
Ulf Waves ◽  
Solar Wind Interaction ◽  
Ion Escape ◽  
A Charge

<p>We study the solar wind interaction with Venus in a 3-dimensional global hybrid model where ions are treated as particles and electrons are a charge-neutralizing fluid. We concentrate on large-scale ultra-low frequency (ULF) waves in the ion foreshock and how they affect the energization and escape of planetary ions. The ion foreshock forms in the upstream region ahead of the quasi-parallel bow shock, where the angle between the shock normal and the magnetic field is smaller than about 45 degrees. The magnetic connection with the bow shock allows backstreaming of the solar wind ions leading to the formation of the ion foreshock. This kind of beam-plasma configuration is a source of free energy for the excitation of plasma waves. The foreshock ULF waves convect downstream with the solar wind flow and encounter the bow shock and transmit in the downstream region. We analyze the coupling of the ULF waves with the planetary ion acceleration and compare Venus and Mars in a global hybrid simulation.</p>

scholarly journals A new method for solving the MHD equations in the magnetosheath

2013 ◽  
Vol 31 (3) ◽  
pp. 419-437 ◽  
Author(s):  
C. Nabert ◽  
K.-H. Glassmeier ◽  
F. Plaschke
Keyword(s):  
Solar Wind ◽  
Order Approximation ◽  
Bow Shock ◽  
Mhd Equations ◽  
Pile Up ◽  
Solar Wind Flow ◽  
Flow Deceleration ◽  
Solar Wind Parameters ◽  
Plasma Depletion ◽  
Geomagnetic Dipole

Abstract. We present a new analytical method to derive steady-state magnetohydrodynamic (MHD) solutions of the magnetosheath in different levels of approximation. With this method, we calculate the magnetosheath's density, velocity, and magnetic field distribution as well as its geometry. Thereby, the solution depends on the geomagnetic dipole moment and solar wind conditions only. To simplify the representation, we restrict our model to northward IMF with the solar wind flow along the stagnation streamline. The sheath's geometry, with its boundaries, bow shock and magnetopause, is determined self-consistently. Our model is stationary and time relaxation has not to be considered as in global MHD simulations. Our method uses series expansion to transfer the MHD equations into a new set of ordinary differential equations. The number of equations is related to the level of approximation considered including different physical processes. These equations can be solved numerically; however, an analytical approach for the lowest-order approximation is also presented. This yields explicit expressions, not only for the flow and field variations but also for the magnetosheath thickness, depending on the solar wind parameters. Results are compared to THEMIS data and offer a detailed explanation of, e.g., the pile-up process and the corresponding plasma depletion layer, the bow shock and magnetopause geometry, the magnetosheath thickness, and the flow deceleration.

Solar wind interaction with the Earth's magnetic field: 2. Magnetohydrodynamic bow shock

1973 ◽  
Vol 78 (19) ◽  
pp. 3731-3744 ◽  
Author(s):  
V. Formisano ◽  
P. C. Hedgecock ◽  
G. Moreno ◽  
F. Palmiotto ◽  
J. K. Chao
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Bow Shock ◽  
Earth’S Magnetic Field ◽  
Solar Wind Interaction ◽  
Earth's Magnetic Field

scholarly journals Energetic protons at Mars: interpretation of SLED/Phobos-2 observations by a kinetic model

2012 ◽  
Vol 30 (11) ◽  
pp. 1595-1609 ◽  
Author(s):  
E. Kallio ◽  
S. McKenna-Lawlor ◽  
M. Alho ◽  
R. Jarvinen ◽  
S. Dyadechkin ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Kinetic Model ◽  
Energetic Particle ◽  
Particle Energy ◽  
Bow Shock ◽  
Solar Wind Interaction ◽  
Flux Enhancement ◽  
Field Environment ◽  
Electric And Magnetic Fields

Abstract. Mars has neither a significant global intrinsic magnetic field nor a dense atmosphere. Therefore, solar energetic particles (SEPs) from the Sun can penetrate close to the planet (under some circumstances reaching the surface). On 13 March 1989 the SLED instrument aboard the Phobos-2 spacecraft recorded the presence of SEPs near Mars while traversing a circular orbit (at 2.8 RM). In the present study the response of the Martian plasma environment to SEP impingement on 13 March was simulated using a kinetic model. The electric and magnetic fields were derived using a 3-D self-consistent hybrid model (HYB-Mars) where ions are modelled as particles while electrons form a massless charge neutralizing fluid. The case study shows that the model successfully reproduced several of the observed features of the in situ observations: (1) a flux enhancement near the inbound bow shock, (2) the formation of a magnetic shadow where the energetic particle flux was decreased relative to its solar wind values, (3) the energy dependency of the flux enhancement near the bow shock and (4) how the size of the magnetic shadow depends on the incident particle energy. Overall, it is demonstrated that the Martian magnetic field environment resulting from the Mars–solar wind interaction significantly modulated the Martian energetic particle environment.

Solar Wind Interaction with Earth's Bow Shock

2021 ◽  
pp. 123-135
Author(s):  
Georges. K. Parks ◽  
Ensang Lee ◽  
Zhongwei W. Yang ◽  
Naiguo Lin ◽  
Suiyan Y. Fu ◽  
...  
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Solar Wind Interaction ◽  
Earth’S Bow Shock

scholarly journals The spectral scalings of magnetic fluctuations upstream and downstream of the Venusian bow shock

2020 ◽  
Author(s):  
S. D. XIAO ◽  
M. Y. Wu ◽  
G. Q. Wang ◽  
Y. Q. Chen ◽  
T. L. Zhang
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Energy Cascade ◽  
Kinetic Regime ◽  
Magnetic Fluctuations ◽  
Solar Wind Interaction ◽  
Large Dispersion ◽  
Key Factor ◽  
Bow Shocks ◽  
Statistical Results

Abstract We statistically investigate the spectral scalings of magnetic fluctuations at the upstream and downstream regions near the Venusian bow shock and perform a differentiation by shock geometry. Based on the Venus Express data, 115 quasi-parallel (Q ∥ ) bow shock crossings and 303 quasi-perpendicular (Q ⊥ ) bow shock crossings are selected. The statistical results suggest that the bow shock tends to modify the upstream spectra flatter to 1/f noise in the magnetohydrodynamics (MHD) regime and steeper to turbulence in the kinetic regime after the magnetic fluctuations crossing the bow shock, and this modification for the Q ∥ and Q ⊥ bow shock is basically consistent. While the upstream spectral scalings are associated with the shock geometry. The changes of the spectral scalings of magnetic fluctuations near the Q ∥ bow shocks are not as significant as near the Q ⊥ bow shock crossings. That might result from the fluctuations generated by the backstreaming ions which can escape across the Q ∥ bow shock into the foreshock. Our results suggest that the energy cascade and dissipation near Venus can be modified by the Venusian bow shock, and the Q ∥ bow shock plays an important role on the energy injection and dissipation in the solar wind interaction with Venus. The large dispersion of spectral scalings indicates that this fluctuation environment is complicated, and the shock geometry is not the only key factor in the fluctuations across the Venusian bow shock. Other possible factors in the shock modification to the upstream fluctuations will be explored in future.

Ultra-low frequency foreshock waves at Venus and Mercury in a global hybrid simulation

2020 ◽  
Author(s):  
Riku Jarvinen ◽  
Esa Kallio ◽  
Tuija I. Pulkkinen
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Large Scale ◽  
Low Frequency ◽  
Hybrid Simulation ◽  
Bow Shock ◽  
Upstream Region ◽  
Ulf Waves ◽  
Solar Wind Interaction ◽  
Low Frequency Waves

<p>We study the solar wind interaction with Venus and Mercury in a 3-dimensional global hybrid simulation where ions are treated as particles and electrons are a charge-neutralizing fluid. We concentrate on the formation of large-scale ultra-low frequency (ULF) waves in ion foreshocks and their dependence on the solar wind and interplanetary magnetic field conditions. The ion foreshock forms in the upstream region ahead of the quasi-parallel bow shock, where the angle between the shock normal and the magnetic field is smaller than about 45 degrees. The magnetic connection with the bow shock allows backstreaming of the solar wind ions leading to the formation of the ion foreshock. This kind of beam-plasma configuration is a source of free energy for the excitation of plasma waves. The foreshock ULF waves convect downstream with the solar wind flow and encounter the bow shock. We compare the waves between Venus and Mercury, and analyze the coupling of the ULF waves with the planetary ion acceleration at Venus.</p> <p>References:</p> <p>Jarvinen R., Alho M., Kallio E., Pulkkinen T.I., 2020, Oxygen Ion Escape From Venus Is Modulated by Ultra-Low Frequency Waves, Geophys. Res. Lett., 47, 11, doi:10.1029/2020GL087462</p> <p>Jarvinen R., Alho M., Kallio E., Pulkkinen T.I., 2020, Ultra-low frequency waves in the ion foreshock of Mercury: A global hybrid modeling study, Mon. Notices Royal Astron. Soc., 491, 3, 4147-4161, doi:10.1093/mnras/stz3257</p>

Sign in / Sign up

Export Citation Format

Share Document