Effects of a dipole-like crustal field on solar wind interaction with Mars

Li, Shibang; Lu, Haoyu; Cui, Jun; Yu, Y.; Mazelle, C.; Li, Yun; Cao, Jinbin

doi:10.26464/epp2020005

Cited by 11 publications

(18 citation statements)

References 46 publications

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“…Figures 3 and 4 show that the crustal field can enhance the extrapolated terminator altitude of the Martian BS by several hundreds of km on average. This is in agreement with the large possible range mentioned in the literature, ranging from no or little influence (with e.g., about 100 km influence from MEX observations (Edberg et al [2009] or simple dipole based MHD simulations; Li et al [2020]) to ∼400 km altitude fluctuation according to XF17, and even above 1,000 km influence based on North versus South asymmetries (Edberg et al, 2008;Gruesbeck et al, 2018).…”

Section: The Influence Of Crustal Fields: Local Versus Global Influencesupporting

confidence: 92%

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The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

et al. 2022

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Previous missions underlined the complex influence of the crustal magnetic fields on the Martian environment, including the plasma boundaries. Their influence on the bow shock is however poorly constrained, with most studies showing North/South differences attributed to the crustal fields, with various conclusions from little to strong variabilities. We analyze for the first time in detail the influence of crustal fields on the Martian shock location based on a multi‐mission analysis (MAVEN and MEX). We introduce the angular distance to the strongest crustal field region in the southern hemisphere that induces the largest influence (but not unique, with a minimum pressure threshold analyzed). Its impact is at large scale (>40–60° around), is modulated by the local time of the strongest source region (with no influence beyond terminator), and maximizes when the Interplanetary Magnetic field (IMF) is stable during the preceding hours. We introduce a technique, that is, partial correlations, to provide a coherent picture for both MAVEN/MEX due to existing cross correlations with Extreme UltraViolet (EUV). A composite parameter is proposed, that represents the combined influence of EUV, magnetosonic mach number (two major drivers) and crustal fields, the latter having an impact of hundreds of km. The influence of crustal fields on the shock appears seasonal and correlated with the Total Electronic Content, revealing a large scale coupling between the crustal fields, the ionosphere and the shock. The crustal field influence on the shock is thus significant and complex, with a coupling to both the ionosphere below and the IMF above.

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Section: The Influence Of Crustal Fields: Local Versus Global Influencesupporting

confidence: 92%

“…[2009] or simple dipole based MHD simulations; Li et al. [2020]) to ∼400 km altitude fluctuation according to XF17, and even above 1,000 km influence based on North versus South asymmetries (Edberg et al., 2008; Gruesbeck et al., 2018).…”

Section: Resultsmentioning

confidence: 99%

The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

et al. 2022

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“…The equations used in the model is composed of Navier-Stokes equations, including continuity, momentum and energy equations for each ion species respectively, as well as a magnetic induced equation. The governing equation for each ion species can be expressed in nonconservative form as follows (S. Li et al, 2020Li et al, , 2022Najib et al, 2011): As for the source terms, 𝐴𝐴 𝐴𝐴𝐴𝐴𝑠𝑠∕𝐴𝐴𝛿𝛿 , 𝐴𝐴 𝐴𝐴𝐴𝐴𝑠𝑠∕𝐴𝐴𝛿𝛿 , and 𝐴𝐴 𝐴𝐴𝐴𝐴𝑠𝑠∕𝐴𝐴𝛿𝛿 represent the mass density, momentum and energy source term, respectively. Inelastic collisions including charge exchange, photoionization, recombination, and elastic collisions including ion-neutral and ion-ion collisions are considered in source terms.…”

Section: Model Descriptionmentioning

confidence: 99%

Effects of Force in the Martian Plasma Environment With Solar Wind Dynamic Pressure Enhancement

Song

Cao

et al. 2023

JGR Space Physics

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As a terrestrial planet, Mars possesses a series of spatial structures and atmospheric evolution processes which are similar to the ones on Earth. It is widely believed that studying the plasma environment and atmospheric erosion mechanisms of Mars has important meanings for understanding the climate change in Mars history, as well as the future evolution of Earth's atmosphere. Unlike Earth, Mars does not have a global magnetic field of internal origin, but possesses remnant crustal magnetic field located mostly in the southern hemisphere (Acuna

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“…variations due to particle collisions and chemical reactions among all the species for mass, momentum, and energy, respectively(Li et al 2020).The electric field E is defined as E u…”

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confidence: 99%

The Impact and Mechanism of the Magnetic Inclination Angle on O⁺ Escape from Mars

Cao

et al. 2022

ApJ

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Ion escape from the atmosphere to space is one of the most likely reasons to account for the evolution of the Martian climate. Based on three-dimensional multifluid magnetohydrodynamic simulations, we investigated the impact of the magnetic inclination angle on O+ escape at low altitudes of 275–1000 km under the typical solar wind conditions. Numerical results showed that an outward ion velocity in the direction opposite to the electromagnetic (EM) force results in weak outward flux and leads to ions becoming trapped by the horizontal magnetic field lines at the local horizontal magnetic equator. Much of the EM force can be attributed to the Hall electric force. In the region of high absolute magnetic inclination angle, the outward ion velocity has the same direction as the EM force, which increases the outward flux and causes ions to diffuse upward along open magnetic field lines to higher altitude. In addition, the EM force is mainly provided by the electron pressure gradient force and the motional electric force. Global results for the magnetic inclination angle indicate that the strong crustal field regions in the southern hemisphere are mainly occupied by magnetic field lines with high absolute magnetic inclination angle, while horizontal field lines are dominant in the northern hemisphere, which leads to a higher O+ escape rate in the Martian southern hemisphere than in the northern, from altitudes of 275 to 1000 km. This is a significant advance in understanding the impact and mechanism of the Martian magnetic field directions on ion escape.

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Effects of a dipole-like crustal field on solar wind interaction with Mars

Cited by 11 publications

References 46 publications

The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

Effects of Force in the Martian Plasma Environment With Solar Wind Dynamic Pressure Enhancement

The Impact and Mechanism of the Magnetic Inclination Angle on O⁺ Escape from Mars

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Effects of a dipole-like crustal field on solar wind interaction with Mars

Cited by 11 publications

References 46 publications

The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

The Influence of Crustal Magnetic Fields on the Martian Bow Shock Location: A Statistical Analysis of MAVEN and Mars Express Observations

Effects of Force in the Martian Plasma Environment With Solar Wind Dynamic Pressure Enhancement

The Impact and Mechanism of the Magnetic Inclination Angle on O+ Escape from Mars

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The Impact and Mechanism of the Magnetic Inclination Angle on O⁺ Escape from Mars