Interaction of Space Weather Phenomena with Mars Plasma Environment During Solar Minimum 23/24

Kajdič, Primož; Sánchez–Cano, Beatriz; Neves‐Ribeiro, L.; Witasse, Olivier; Bernal, G. C.; Rojas‐Castillo, Diana; Nilsson, Hans; Fedorov, A.

doi:10.1029/2020ja028442

Cited by 10 publications

(5 citation statements)

References 80 publications

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“…While all energy fluxes are calculated during times when the spacecraft encounters the solar wind, per the Trotignon et al. (2006) empirical formula for the bow shock location, the bow shock is not a static boundary and can diverge from this formula, particularly during space weather events (Gruesbeck et al., 2018; Kajdić et al., 2021). When the bow shock is located further from Mars than the empirical formula suggests, we sample the sheath in addition to the solar wind.…”

Section: Datamentioning

confidence: 99%

Energy Input of EUV, Solar Wind, and SEPs at Mars: MAVEN Observations During Solar Minimum

et al. 2023

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Solar energy inputs drive atmospheric, ionospheric, and induced magnetospheric processes at unmagnetized planets like Mars. Solar extreme ultraviolet (EUV) radiation is the dominant energy source, heating the Martian thermosphere and producing the majority of the Martian ionosphere. Energetic particles in the space environment may additionally ionize and heat the upper atmosphere, provided they can enter and "precipitate" into the atmosphere. Since Mars lacks an intrinsic magnetic field, the interplanetary magnetic field (IMF) carried with the incident solar wind flow induces currents in the ionosphere to form an induced magnetosphere. The resulting interaction shocks, decelerates, and deflects the solar wind (see Nagy et al., 2004 and references therein). However, the solar wind can still directly impart energy to the atmosphere: as ions that have been converted into energetic neutral atoms (ENAs) and as electrons precipitating into magnetically connected regions of the upper atmosphere. In addition, solar transients such as coronal mass ejections (CMEs) and stream-interaction regions (SIRs) can accelerate ions and electrons to very high energies, supplying solar energetic particles (SEPs) that may episodically deposit significant energy into the atmosphere.Many prior studies have characterized the energy input of EUV, solar wind, and SEPs separately. This study aims to directly intercompare these solar drivers over time and quantify their relative magnitudes in the near Mars environment. We assess if sporadic SEP energy fluxes can temporarily exceed the comparatively steady EUV or solar wind energy fluxes, and if this influence remains when integrated over a fraction of a solar cycle. We also approximate how much energy flux is absorbed by the Martian atmosphere for each solar driver to determine whether a solar driver can displace another as a meaningful source of energization. Since each solar driver varies on timescales that range from hours to years, we analyze the energy fluxes in the context of event-to-event variation, changing seasons, and a declining solar cycle. Finally, we compare modern energy fluxes to prior published energy fluxes derived for the young sun. This provides useful context for studies of current and historical

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Section: Datamentioning

confidence: 99%

Energy Input of EUV, Solar Wind, and SEPs at Mars: MAVEN Observations During Solar Minimum

et al. 2023

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“…During this Venus flyby, the orbit skimmed the bow shock. Kivelson et al (1991) used the magnetometer data to investigate the cross section of the bow shock. They found that it seemed to be smaller when its direction was aligned with the IMF when compared to when its direction was perpendicular to the IMF.…”

Section: Mariner 10 Galileo and Pioneer Venusmentioning

confidence: 99%

Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby

et al. 2021

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Abstract. Out of the two Venus flybys that BepiColombo uses as a gravity assist manoeuvre to finally arrive at Mercury, the first took place on 15 October 2020. After passing the bow shock, the spacecraft travelled along the induced magnetotail, crossing it mainly in the YVSO direction. In this paper, the BepiColombo Mercury Planetary Orbiter Magnetometer (MPO-MAG) data are discussed, with support from three other plasma instruments: the Planetary Ion Camera (SERENA-PICAM) of the SERENA suite, the Mercury Electron Analyser (MEA), and the BepiColombo Radiation Monitor (BERM). Behind the bow shock crossing, the magnetic field showed a draping pattern consistent with field lines connected to the interplanetary magnetic field wrapping around the planet. This flyby showed a highly active magnetotail, with e.g. strong flapping motions at a period of ∼7 min. This activity was driven by solar wind conditions. Just before this flyby, Venus's induced magnetosphere was impacted by a stealth coronal mass ejection, of which the trailing side was still interacting with it during the flyby. This flyby is a unique opportunity to study the full length and structure of the induced magnetotail of Venus, indicating that the tail was most likely still present at about 48 Venus radii.

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“…It is now well-accepted that ICMEs are the solar transients that have the greatest effect on the space environment and cause the most adverse space weather effect (Zhang et al 2021b). ICME events significantly affect the structure of the upper atmosphere and ionosphere of Mars, and influence the loss of ions to space (Jakosky et al 2015;Sánchez-Cano et al 2017;Kajdič et al 2021). Therefore, ICMEs play an important role in driving plasma escape and the evolution of the Martian atmosphere.…”

Section: Introductionmentioning

confidence: 99%

Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection

Yu¹,

Chi²,

Owens

et al. 2023

ApJ

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Interplanetary coronal mass ejections (ICMEs) are solar transients that have significant effects on the upper atmosphere and ionosphere of Mars. The simultaneous spacecraft observations from Tianwen-1/MOMAG in solar wind and multiple instruments on board the Mars Atmosphere and Volatile Evolution (MAVEN) in the Martian upper atmosphere are used to study the response of Mars to an ICME. The ICME was observed at Mars by Tianwen-1 and MAVEN at 00:00 UT on 2021 December 10, which was earlier observed by BepiColombo upstream of Mars at 22:32 UT on 2021 December 6. During 2021 December 6–15, MAVEN measured the nightside ionosphere and Tianwen-1 measured the dayside ionosphere while both were inside the Martian bow shock. The rapid drop in densities of ionospheric ions and electrons, which is typically identified as the end of the ionosphere at altitudes between 300–800 km, is known as the ionopause. The altitude of the Martian ionopause location was lowered by the high dynamic pressure of the solar wind during the ICME passage. The depletion of the plasma density in the topside Martian ionosphere on the nightside reveals the presence of substantial ion and electron escape to space through the interaction between the ICME and Mars. The column abundance of plasma dramatically decreased, with 34% e−, 61% O 2 + , and 73% O+ reduced. This study highlights the significant impact of the space weather associated with the intense magnetic field and high dynamic pressure of the ICME on Mars’s atmosphere, which is particularly important for future human exploration missions to Mars.

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Interaction of Space Weather Phenomena with Mars Plasma Environment During Solar Minimum 23/24

Cited by 10 publications

References 80 publications

Energy Input of EUV, Solar Wind, and SEPs at Mars: MAVEN Observations During Solar Minimum

Energy Input of EUV, Solar Wind, and SEPs at Mars: MAVEN Observations During Solar Minimum

Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby

Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection

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