A 3D Parametric Martian Bow Shock Model with the Effects of Mach Number, Dynamic Pressure, and the Interplanetary Magnetic Field

Wang, M.; Xie, Luhua; Lee, L. C.; Xu, Xiaokang; Кабин, К.; Lu, J. Y.; Wang, J.; Li, L.

doi:10.3847/1538-4357/abbc04

Cited by 21 publications

(31 citation statements)

References 59 publications

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“…Figures 3(e), (f) illustrate the modulations of IMF components on the subsolar induced magnetosphere and the subsolar plasma boundaries based on Cases 1-13. The variation in the bow shock location is consistent with previous studies (Chai et al 2014;Wang et al 2020). The IMB, the thickness, and field strength of the induced magnetosphere are not sensitive to the IMF B X but increase with increasing B Y .…”

Section: Control Of the Imf On The Venusian Induced Magnetospheresupporting

confidence: 90%

The Dependence of the Venusian Induced Magnetosphere on the Interplanetary Magnetic Field: An MHD Study

Zuo

et al. 2022

ApJ

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The influences of the interplanetary magnetic field (IMF) on the induced magnetosphere of Venus are investigated using a global multispecies magnetohydrodynamics (MHD) model. The simulation results show that the induced magnetosphere is controlled by the IMF components perpendicular to the solar wind velocity (B Y and B Z in the Venus Solar Orbital coordinate), rather than the IMF magnitude (∣B∣). With the increase of ( B Y 2 + B Z 2 ) 1 2 , the induced magnetosphere becomes stronger in field strength and thicker in spatial scale, and the bow shock locates farther from the planet. The parallel IMF component (B X ) has relatively small impacts on the magnetic barrier and the magnetotail, regardless of the various IMF magnitudes and orientations caused by different B X . The responses of the Venusian induced magnetosphere to the change of upstream IMF are also studied. The time-dependent MHD calculations show that the dayside magnetosphere responds quickly with a timescale of 10 s–10 minutes, depending on the considered magnetospheric region. For comparison, the timescale required for the adjustment of magnetotail as driven by an IMF rotation is derived to be ∼10–20 minutes.

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Section: Control Of the Imf On The Venusian Induced Magnetospheresupporting

confidence: 90%

The Dependence of the Venusian Induced Magnetosphere on the Interplanetary Magnetic Field: An MHD Study

Zuo

et al. 2022

ApJ

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“…The locations of the bow shock as well as of the MPB have been determined and parameterized in several studies (i.e., Edberg et al., 2008; Gruesbeck et al., 2018; Němec et al., 2020; Trotignon et al., 2006; Vignes et al., 2000; Wang et al., 2020). These boundaries though are not fixed in altitude or shape, and appear to have a dynamic relationship with various parameters, such as extreme ultraviolet (EUV) radiation, crustal magnetic fields, solar wind parameters, interplanetary magnetic field (IMF) orientation, Martian seasons and solar cycle (Brain et al., 2005; Edberg et al., 2008, 2009; Hall et al., 2016, 2019; Matsunaga et al., 2017; Ramstad, Barabash, Futaana, & Holmström, 2017).…”

Section: Introductionmentioning

confidence: 99%

A Two‐Spacecraft Study of Mars' Induced Magnetosphere's Response to Upstream Conditions

et al. 2022

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Mars has no intrinsic dipolar magnetic field with which to stand off the incoming solar wind. Instead its conducting ionosphere acts as an effective obstacle to the incoming solar wind and an induced magnetosphere is formed, the structure of which is determined for instance by the solar wind input, ultraviolet (UV) radiation, the Martian crustal magnetic fields and the underlying neutral atmosphere (Bertucci et al., 2011;Nagy et al., 2004). Many aspects of the Mars-solar wind interaction are outwardly comparable to those at Venus, as was extensively studied during the Pioneer-Venus era, and thus much of the understanding developed initially for Venus can be transferred to the Mars interaction, despite differences of scale, solar wind conditions, and so on (Luhmann & Cravens, 1991). Moreover, the Mars-solar wind interaction has been extensively studied in recent years by ESA's Mars Express (MEX) and NASA's Mars Atmosphere and Volatile EvolutioN (MAVEN) missions, and relevant aspects are summarized below.The Mars-solar wind interaction is typically characterized by the formation of several distinct plasma boundaries separating regions of differing plasma properties and compositions. At the largest distances, the bow shock is formed upstream from the planet, inside which the solar wind is slowed, heated and deflected around the

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“…The locations of the bow shock as well as of the MPB have been determined and parameterized in several studies (i.e., Edberg et al, 2008;Gruesbeck et al, 2018;Němec et al, 2020;Trotignon et al, 2006;Vignes et al, 2000;Wang et al, 2020). These boundaries though are not fixed in altitude or shape, and appear to have a dynamic relationship with various parameters, such as extreme ultraviolet (EUV) radiation, crustal magnetic fields, solar wind parameters, interplanetary magnetic field (IMF) orientation, Martian seasons and solar cycle (Brain et al, 2005;Edberg et al, 2008Edberg et al, , 2009Hall et al, 2016Hall et al, , 2019Matsunaga et al, 2017;.…”

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A two-spacecraft study of Mars induced magnetosphere's response to upstream conditions

Stergiopoulou¹,

Edberg²,

Andrews³

et al. 2024

Preprint

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We investigate the effects of the upstream solar wind magnetic field on the Martian induced magnetosphere. This is a two-spacecraft study, for which we use Mars Express (MEX) magnetic field magnitude data from the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) instrument and Interplanetary Magnetic Field (IMF) measurements and solar wind density and velocity from the magnetometer (MAG) and the Solar Wind Ion Analyzer (SWIA) on board Mars Atmosphere and Volatile EvolutioN (MAVEN), from November 2014 to November 2018. Equally temporally spaced echoes appear in MARSIS' ionograms from which the electron cyclotron frequency and eventually the magnitude of the local magnetic field can be calculated. At the same time solar wind magnetic field data and solar wind parameters from MAG and SWIA respectively are utilized, providing the solar wind input to the Martian system. We make real time comparisons of the IMF and the induced magnetic field in the environment of Mars and we test the ratio B(MEX)&#160;/B(MAVEN) &#160;against various parameters such as the solar wind dynamic pressure, velocity, density, Mach number as well as the Martian seasons, latitudes and heliocentric distances. Additionally, we search for disturbances in IMF which then can be traced in the induced field ultimately revealing the response time of the induced magnetosphere to the solar wind behaviour.&#160; MEX and MAVEN measurements combined allow us to investigate the response of the Martian induced magnetosphere to the solar wind magnetic field. Real time comparisons of the IMF and the induced field could help us understand the mechanisms controlling the structure of the Martian induced magnetosphere.&#160;

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A 3D Parametric Martian Bow Shock Model with the Effects of Mach Number, Dynamic Pressure, and the Interplanetary Magnetic Field

Cited by 21 publications

References 59 publications

The Dependence of the Venusian Induced Magnetosphere on the Interplanetary Magnetic Field: An MHD Study

The Dependence of the Venusian Induced Magnetosphere on the Interplanetary Magnetic Field: An MHD Study

A Two‐Spacecraft Study of Mars' Induced Magnetosphere's Response to Upstream Conditions

A two-spacecraft study of Mars induced magnetosphere's response to upstream conditions

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