# The Mars system revealed by the Martian Moons eXploration mission

Kazunori Ogohara, Hiromu Nakagawa, Shohei Aoki, Toru Kouyama, Tomohiro Usui, Naoki Terada, Takeshi Imamura, Franck Montmessin, David Brain, Alain Doressoundiram, et al.

► To cite this version:

Kazunori Ogohara, Hiromu Nakagawa, Shohei Aoki, Toru Kouyama, Tomohiro Usui, et al. The Mars system revealed by the Martian Moons eXploration mission. Earth Planets and Space, 2022, 74, pp.10.1186/s40623-021-01417-0. insu-03510824

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# The Mars system revealed by the Martian Moons eXploration mission

Kazunori Ogohara<fnref n="1" />*, Hiromu Nakagawa², Shohei Aoki³,⁴, Toru Kouyama⁵, Tomohiro Usui⁶, Naoki Terada², Takeshi Imamura⁷, Franck Montmessin⁸, David Brain⁹, Alain Doressoundiram¹⁰, Thomas Gautier⁸, Takuya Hara¹¹, Yuki Harada¹², Hitoshi Ikeda¹³, Mizuho Koike¹⁴, François Leblanc¹⁵, Ramses Ramirez¹⁶,¹⁷,²⁵, Eric Sawyer¹⁸, Kanako Seki¹⁹, Aymeric Spiga²⁰,²¹, Ann Carine Vandaele²², Shoichiro Yokota²³, Antonella Barucci¹⁰ and Shingo Kameda²⁴

## Abstract

Japan Aerospace Exploration Agency (JAXA) plans a Phobos sample return mission (MMX: Martian Moons eXploration). In this study, we review the related works on the past climate of Mars, its evolution, and the present climate and weather to describe the scientific goals and strategies of the MMX mission regarding the evolution of the Martian surface environment. The MMX spacecraft will retrieve and return a sample of Phobos regolith back to Earth in 2029. Mars ejecta are expected to be accumulated on the surface of Phobos without being much shocked. Samples from Phobos probably contain all types of Martian rock from sedimentary to igneous covering all geological eras if ejecta from Mars could be accumulated on the Phobos surface. Therefore, the history of the surface environment of Mars can be restored by analyzing the returned samples. Remote sensing of the Martian atmosphere and monitoring ions escaping to space while the spacecraft is orbiting Mars in the equatorial orbit are also planned. The camera with multi-wavelength filters and the infrared spectrometer onboard the spacecraft can monitor rapid transport processes of water vapor, dust, ice clouds, and other species, which could not be traced by the previous satellites on the synchronous polar orbit. Such time-resolved pictures of the atmospheric phenomena should be an important clue to understand both the processes of water exchange between the surface/underground reservoirs and the atmosphere and the drivers of efficient material transport to the upper atmosphere. The mass spectrometer with unprecedented mass resolution can observe ions escaping to space and monitor the atmospheric escape which has made the past Mars to evolve towards the cold and dry surface environment we know today. Together with the above two instruments, it can potentially reveal what kinds of atmospheric events can transport tracers (e.g., H₂O) upward and enhance the atmospheric escape.

**Keywords:** Mars, Mars system, Paleoclimate, Atmospheric escape, Water cycle, Dust cycle, Transport process

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<footnote>*Correspondence: ogohara@cc.kyoto-su.ac.jp</footnote>

<footnote n="1">¹ Faculty of Science, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan</footnote>

<footnote>Full list of author information is available at the end of the article</footnote>
**Graphical Abstract**

<figure><img src="image_5.png" /></figure>

**Introduction**

Mars is the planet most similar to the Earth in the solar system in that it has a solid surface and an appreciable amount of atmosphere with moderate temperatures, and that there is evidence of liquid water activity, volcanic activity and a possible habitability. In recent decades many Mars missions have been conducted to reveal the planet's evolution and the current climate. Though the current Mars is a dry and cold world that includes a significant amount of frozen surface/subsurface water resources, geological evidence obtained by the spacecraft suggests that Mars may have sustained a wet and warm world in the past under the influence of a greenhouse effect (e.g., Ramirez and Craddock 2018). The transition to the current climate should have been driven by a combination of various physical/chemical processes, such as degassing, escape of volatiles to space, loss of the intrinsic magnetic field, exchange of water and other volatiles between the atmosphere and the crust, photochemistry, radiative transfer and atmospheric circulation. A possible example of strong coupling between different processes is the recent discovery of the apparent response of escaping ion fluxes to the upward transport of dust and water in the lower atmosphere (Heavens et al. 2018). The growing global interest in the history of the Martian surface

environment motivated us to develop a Mars observation plan in the MMX (Martian Moons eXploration) mission aiming to disentangle the coupling among different processes, thereby assessing the roles of short-term elementary processes in the atmosphere and in the circum-Mars space in the long-term evolution of the Martian environment.

MMX is the third sample return mission of JAXA (Japan Aerospace Exploration Agency) (Kuramoto et al. 2021). The spacecraft will conduct close-up observations of the Martian satellites Phobos and Deimos, collect samples from Phobos, and bring them back to the Earth to reveal the origin of the two moons. In addition, MMX will conduct remote observations of the Martian atmosphere and surface and in situ measurements of volatiles escaping to space during the 3-year Mars orbiting phase. We take advantage of MMX's unique orbit around Mars: the equatorial high-altitude orbit will enable continuous remote monitoring of short-timescale phenomena in the atmosphere and increase opportunities of the measurement of low-energy ion outflows in the shadows of Mars and Phobos. The samples brought back to the Earth are expected to contain particles ejected from the Martian surface by asteroid impacts, from which information on early Mars will be retrieved. Combining this broad range
of information will allow for an integrated understanding of Mars system that consists of Mars, its moons, and the circum-Mars space. For example, the transport of water across the atmosphere from the surface to space will be tracked with an infrared imaging spectrometer and an ion spectrometer, and this knowledge of water transport, combined with isotopic fractionation analysis of returned Mars samples, will allow us to develop a scenario of the environmental evolution of Mars. The spacecraft will be launched in 2024, put into a Martian orbit in 2025, stay in orbit around Mars until 2028, and return to the Earth in 2029. The detail of the mission sequence will be given by another paper in this issue.

Currently quite a few Mars missions are ongoing. They include Mars Odyssey, Mars Express (MEX), Mars Reconnaissance Orbiter (MRO), Curiosity rover, Mangalyaan orbiter, Chinese Tianwen 1 mission, Mars Atmosphere and Volatile Evolution (MAVEN), ExoMars Trace Gas Orbiter (EMTGO), and InSight lander. The Hope orbiter planned by United Arab Emirates will start remote observations of the Martian atmosphere from a high-altitude equatorial orbit in 2021. Mars sample return (MSR) mission is also currently under consideration to bring back samples from Mars (Beaty et al. 2019). The Mars observations in MMX are complementary to those missions in several aspects, such as the observation wavelength, the spatial resolution in global imaging, the sensitivity to low energies and the mass resolution in ion measurements, and the sample return to the Earth.

In this paper, we describe the science goals of the mission and the observation strategies. We describe the mission objectives related to the Mars science in the next section. The “Scientific background and key requirements for observation” section reviews the previous studies on the Martian paleoclimate, atmospheric escape and the transport processes in the atmosphere. What and how are understood from Martian samples accumulated on Phobos are summarized in the “Martian sample on the Phobos surface” section, the observation plan and the instruments in the “Mars observation by MMX” section, and the synergy with other Mars missions in the “Synergy with other missions” section. A summary is given in the last section.

## Mission definition regarding the Mars environmental history

We are motivated to plan MMX by the growing global interest in the evolution of the Martian environment as mentioned in the “Introduction” section. This is reflected in one of the scientific goals (SGs) of MMX. The first of SGs (SG-1) is related to studies on the Martian moons and the understanding of the planetary system formation and material transport in the solar system (Kuramoto

et al. 2021). The second scientific goal of the MMX (SG-2) is:

* From the viewpoint of the Martian moons, clarify the driving mechanism of the transition of the Mars-moon systems and add new knowledge to the evolution history of Mars.

What is crucial for studies on the evolution of the planetary surface environment is to directly observe the history as geologists have reconstructed the history of the terrestrial environment from rock or sediment samples. Another important approach is to understand the phenomena seen in the atmosphere and circum-Mars space today and infer the past from them. Thus, SG-2 is broken down into three medium objectives (MOs). Table 1 provides an overview of the relationship between the SG, MOs and related science themes. The first MO is associated with the surface processes of the airless small body (i.e., Phobos) and the other two MOs cover the Mars environmental evolution:

* MO-2.2: add new findings and constraints on the history of changes in the Martian surface,

* MO-2.3: constrain the mechanisms of material circulation in the Martian atmosphere affecting the transitions in the Martian climate.

One of methods to achieve MO-2.2 is to restore the paleoclimate changes from Martian samples that have been accumulated on the Phobos surface (Hyodo et al. 2017). The other is estimation of the past atmospheric escape based on the present observations. They are expected to be achieved by analyses of Martian samples on Phobos returned to Earth and observations of the atmospheric escape. MO-2.3 covers understanding of the efficient upward transport processes required for efficient H₂O escape from the top of the atmosphere. MO-2.3 is expected to be achieved by continuous full-disk monitoring of Mars with visible and infrared wavelengths. Observations of distributions of dust, ice clouds, and water vapor with higher temporal and spatial resolutions than the previous observations are necessary for MO-2.3.

Previous studies on the three science themes, paleoclimate of Mars restored from samples on Phobos, the Martian atmospheric escape, and transport mechanisms in the present Martian atmosphere, associated with the MOs are reviewed in the next section. Plans of the analyses of the samples and expected findings are described in detail in the “Martian sample on the Phobos surface” section. Although the orbit of the spacecraft and scientific payload are briefly introduced for the reviews in the next section, they are fully described in the “Mars observation
<table><caption>**Table 1** Relation between the science goal, medium objectives and related science themes</caption><thead><tr><td>Science goal</td><td>Medium objective</td><td>Science theme</td><td>Measurement</td></tr></thead><tbody><tr><td>SG-2: from the viewpoint of the Martian moons, clarify the driving mechanism of the transition of the Mars-moon systems and add new knowledge to the evolution history of Mars</td><td>MO-2.2: add new findings and constraints on the history of changes in the Martian surface</td><td>Paleoclimate restored from Martian samples on Phobos surface<br>History of changes in the H<sub>2</sub>O and CO<sub>2</sub> reservoirs of Mars</td><td>Martian samples accumulated on the Phobos surface<br>Ions escaping from the atmosphere including cold ions<br>Continuous monitoring of the behavior of dust, clouds and water vapor with high temporal and spatial resolutions</td></tr><tr><td></td><td>MO-2.3: constrain the mechanisms of material circulation in the Martian atmosphere affecting the transitions in the Martian climate</td><td>Material transport processes in the present<br>Martian atmosphere</td><td></td></tr></tbody></table>

See Kuramoto et al. (2021) for details of SG-1, MO-1, and MO-2.1
by MMX" section. While they have been designed to make sure of the other MOs regarding SG-1, it is emphasized in the following sections that they are also suitable for observations of the Martian atmosphere and circum-Mars space regarding the above MOs and distinguished from other missions.

## Scientific background and key requirements for observation

### Martian paleoclimate

Mars is a cold and dry planet that exhibits below-freezing mean surface temperatures that are akin to those in many portions of Antarctica (e.g., Spanovich et al. 2006). However, this frigid present Mars contrasts heavily with the much warmer and wetter world that observations (both orbital and rover) suggest existed ~3.5–4 Gyr ago (e.g., Masursky 1973; Craddock and Howard 2002; Ramirez and Craddock 2018). The ancient highlands, which represent the oldest terrains on Mars that cover ~2/3 of the planet, abound with fluvial features, including deltas, alluvial fans, possible ancient shorelines, and most famously, the valley networks (e.g., Masursky 1973; Craddock and Howard 2002; Fassett and Head 2008a, b; Howard et al. 2005; Irwin et al. 2011; Usui et al. 2020).

Although climate models simulate the current climate quite well (e.g., Fenton et al. 2007; Pottier et al. 2017; Haberle et al. 2019a), this warmer and wetter early Mars has been a challenge to explain. As a result of its larger orbital distance and the faint young sun, early Mars 4 Gyr ago receives only ~32% the incident flux that our planet does. Thus, a dense atmosphere with a very strong greenhouse effect would have been required to sustain stable bodies of liquid water on the Martian surface.

Mars may have initially accreted ~10 bars of CO₂ based on a simple mass-radius scaling from Earth's primordial inventory (e.g., Ramirez and Craddock 2018). This is enough CO₂ to solve the climate paradox even though other processes, including atmospheric escape and volcanic outgassing, would have led to a net decrease in atmospheric pressure over time (e.g., Tian et al. 2010; Kurokawa et al. 2018). Indeed, atmospheric CO₂ pressures exceeding ~5 bar 3.8 Gyr ago would have yielded mean surface temperatures above the freezing point of water (e.g., Pollack et al. 1987). However, these early calculations had neglected CO₂ condensation, which was shown to reduce tropospheric lapse rates and decrease mean surface temperatures to ~220–230 K (e.g., Kasting 1991; Tian et al. 2010; Ramirez et al. 2014). Thus, a different mechanism would be needed to resolve the climate conundrum.

Subsequent calculations employing CO₂ clouds' scattering greenhouse effect showed that warm surface temperatures were achievable for CO₂ cloud coverage

approaching 100% (Forget and Pierrehumbert 1997). However, this warming is drastically reduced at more realistic cloud fractions (~50%) (Forget et al. 2013). Plus, models that employ more accurate multi-stream radiative transfer schemes predict a much weaker CO₂ cloud greenhouse effect than that estimated with traditional two-stream approaches (Kitzmann 2016).

Similar complications were found for upper tropospheric cirrus clouds composed of water vapor. One study predicts that impact-induced cirrus clouds that consist of 10 micron or larger sized particles could generate transiently warm conditions (e.g., Urata and Toon 2013). Again, significant warming was possible only for cirrus cloud fractions exceeding ~75%, which is unrealistically cloudy for a potentially habitable planet with both rising and subsiding air (Ramirez and Kasting 2017). A recent study argues that significant warming is possible at lower cloud fractions if cirrus clouds can form in the stratosphere (Turbet et al. 2020a). However, this scenario is extremely unlikely because the stratosphere is dry and cirrus cloud formation is disfavored (Ramirez and Kasting 2017).

Thus, the difficulty of warming early Mars with just CO₂ and H₂O has led various investigators to consider whether the surface geology could have formed in a cold climate instead. This has spawned various cold and icy early Mars scenarios that invoke transient warming episodes caused by external events, including volcanic eruptions, meteoritic impacts, obliquity changes, methane bursts, or climate limit cycles (e.g., Segura et al. 2002, 2008; Ehlmann et al. 2011; Urata and Toon 2013; Forget et al. 2013; Kite et al. 2013, 2020; Wordsworth et al. 2013, 2015; Batalha et al. 2016; Haberle et al. 2019b; Steakley et al. 2019; Hayworth et al. 2020). It is worth noting that the notion of a permanently cold and icy early Mars has been questioned in recent years (e.g., Craddock and Howard 2002; Ramirez and Craddock 2018). For example, such mechanisms (to date) cannot produce the water amounts necessary to explain the widespread fluvial erosion, including the valley networks (e.g., Davis et al. 2016; Ramirez and Craddock 2018). Also, both rover and orbital evidence have shown no unambiguous evidence of extensive glaciation, whether wet- or dry-based, anywhere in valley network terrains (e.g., Burr et al. 2010; Grotzinger et al. 2015; Davis et al. 2016, 2019). Such observations have led to an increase in our understanding and contributed to the recent increase in solutions that favor various transiently and continuously warm scenarios over those that advocate a permanently cold and icy early Mars (e.g., Ramirez and Craddock 2018).

Nevertheless, it is now understood that the combined greenhouse effect of CO₂ and H₂O, even with clouds, does not provide enough warming to solve the
early Martian climate problem. Some investigators have argued that secondary greenhouse gases could have provided that additional warming. Sulfur dioxide ($SO_2$), for instance, is an effective warming agent in a $CO_2$-dominated early Martian atmosphere (e.g., Postawko and Kuhn 1986; Mischna et al. 2013; Halevy and Head 2014; Kerber et al. 2015). However, not only does sulfur form long chains that reflect away incoming radiation, but $SO_2$ rains out of the atmosphere as temperatures warm, severely limiting its effectiveness (e.g., Tian et al. 2010).

Other gases have been considered as well. Using data suggesting potentially oxidizing conditions at Gale crater, Ito et al. (2020) posit that hydrogen peroxide ($H_2O_2$) could have been this potent secondary greenhouse gas. That said, an extremely high (and likely implausible) degree of supersaturation would have been required to warm the planet and offset photochemical destruction (Ito et al. 2020).

Another important greenhouse gas combination is $CO_2-CH_4$, which has a relatively strong greenhouse effect at high enough pressures (e.g., Ramirez et al. 2014; Wordsworth et al. 2017). However, absorption at solar wavelengths forms upper atmospheric temperature inversions that negate some of this warming (Ramirez et al. 2014; Wordsworth et al. 2017). Although initial estimates of $CO_2-CH_4$ collision-induced absorption (CIA) had suggested that ~10% $CH_4$ in a 2-bar $CO_2$ atmosphere could have nearly produced the required climates (Wordsworth et al. 2017), subsequent experimental estimates found that $CO_2-CH_4$ CIA is much weaker than previously estimated, further weakening the plausibility of this solution (Turbet et al. 2019, 2020b).

Ramirez et al. (2014) had originally proposed that a $CO_2-H_2$ greenhouse could have warmed early Mars. This was based on analyses of Martian meteorites suggesting a highly reducing early mantle (e.g., Shearer et al. 2006; Nakada et al. 2020; Wadhwa et al. 2001), permitting percent levels of volcanically outgassed hydrogen to accumulate in the atmosphere in spite of high atmospheric escape rates (Ramirez et al. 2014). Revised calculations suggest that atmospheres consisting of ~3–10% $H_2$ and 1–2 bars of $CO_2$ may have been sufficient to warm early Mars (Wordsworth et al. 2017; Ramirez 2017). Other calculations indicate that such $CO_2-H_2$ atmospheres are photochemically stable (Batalha et al. 2015). However, as with methane, $CO_2-H_2$ CIA had been significantly overestimated (Turbet et al. 2019, 2020b). That said, even with the revised absorption cross sections, this greenhouse solution remains very promising. For instance, warm climates can be achieved with just 5% $H_2$ in a 2-bar $CO_2$ atmosphere (Turbet et al. 2020b; Godin et al. 2020).

However, these previous $CO_2-H_2$ computations were performed using simple radiative-convective climate models. Recent studies utilizing advanced climate models have incorporated oceans and calculated estimated precipitation (rain, snow) rates (Ramirez et al. 2020; Kamada et al. 2020). The warm simulations in both studies yield hydrogen and carbon dioxide partial pressures that are consistent with those predicted by radiative-convective models. They also find that a warm early Mars with a large northern ocean would have likely had an arid to semi-arid climate (Ramirez et al. 2020; Kamada et al. 2020). Valley network formation would have been brief, nearly global, and finished within $10^4-10^7$ years (Ramirez et al. 2020; Kamada et al. 2020), which is consistent with geologic inferences (e.g., Hoke et al. 2011; Orofino et al. 2018). In addition, Ramirez et al. (2020) find that precipitation rates are negligible for warm climates with small oceans. Thus, they conclude that a large ocean may have been necessary to produce a hydrologic cycle that was robust enough to form the observed surface geology. It is possible that Mars samples retrieved from Phobos could elucidate the earliest period of Mars (the “Martian sample on the Phobos surface” section), including the amount of water that may have existed during these ancient times.

## Atmospheric escape

The cumulative effect of the atmospheric erosion due to the external forcing, such as solar radiation and solar wind, is regarded as one of the plausible candidates of the drastic climate change from warm and wet to cold and dry environment. Especially, the lack of a global magnetic field on Mars must have a significant impact on the atmospheric escape. The weak magnetosphere would have allowed solar wind to strip away much of its atmosphere to space. There have been proposed a variety of processes of the atmospheric escape from Mars (e.g., Shizgal and Arkos 1996; Chassefiere and Leblanc 2004).

The lack of a global magnetic field means that the upper atmosphere of Mars is directly exposed to the solar wind, leading to erosion of ionized gasses from the top of the atmosphere through various processes driven by the solar wind interaction. The Soviet Mars 2, 3, and 5 spacecraft first measured the ion escape from Mars and also identified characteristic plasma boundaries such as bow shock (e.g., Vaisberg and Smirnov 1986, and references therein). Later Phobos 2 spacecraft also measured a significant loss of ionospheric ions through the magnetotail (e.g., Lundin et al. 1989; Lundin et al. 1990; Lundin and Dubinin 1992). These spacecrafts estimated ion escape rates to be of the order of $1024-1025 s^{-1}$, which correspond to evacuation of the total oxygen content in the present-day atmosphere of Mars in less than
108–109 years. Recently the Ion Mass Analyser (IMA) instrument, one of the Analyser of Space Plasma and Energetic Atoms (ASPERA-3) package aboard ESA's Mars Express (Barabash et al. 2006), has successfully measured heavy ions such as $O^+$, $O_2^+$, and $CO_2^+$ escaping through the induced magnetotail (e.g., Carlsson et al. 2006; Lundin et al. 2009). IMA has measured ion distribution functions since 2004 to date, and the > 16 years of observations have provided many opportunities to study the ion escape for characteristic solar events and seasonal changes (e.g., Futaana et al. 2008; Dubinin et al. 2009; Edberg et al. 2010; Hara et al. 2011; Yamauchi et al. 2015). The long-term dataset of IMA has also provided comprehensive views in the heavy ion escape rates from Mars, varying within $1024 \text{ s}^{-1}$ order of magnitude under a variety of external conditions in terms of the solar wind and solar EUV flux (e.g., Lundin et al. 2008; Nilsson et al. 2010, 2011; Ramstad et al. 2015, 2017, 2018).

Recent observations of the Suprathermal and Thermal Ion Composition (STATIC) instrument (McFadden et al. 2015) aboard NASA's MAVEN spacecraft resolved two distinctive ion escape channels, the plume channel along the convective electric field of the solar wind and the tail channel along the magnetotail (Dong et al. 2015; Brain et al. 2015), which agrees with theoretical studies (e.g., Fang et al. 2008). Dong et al. (2015, 2017) also estimated the $O^+$ ion escape rates of the orders of $1023 \text{ s}^{-1}$ and $1024 \text{ s}^{-1}$ through the plume and tail channels, respectively. The simultaneous ion and magnetic field measurements of MAVEN also provided characteristic features linked to the ion acceleration and escape such as classical pickup ions in the solar wind (Rahmati et al. 2017, 2018; Masunaga et al. 2017), their reflections in the magnetosheath and resulting ion beams above the bow shock (Masunaga et al. 2016, 2017), magnetic reconnections in the tail and dayside ionosphere (Harada et al. 2015, 2017, 2018, 2020), vortex structures likely caused by the Kelvin-Helmholtz instability (Ruhunusiri et al. 2016), and flux ropes containing heavy ions near the crustal magnetic field (Hara et al. 2015, 2016).

Modeling efforts have been also made to understand the observational results for decades (e.g., Brain et al. 2010, and references therein). The modeling works today can reproduce characteristic plasma environments around Mars in a good agreement with observations (e.g., Ma et al. 2004, 2017; Fang et al. 2008, 2017) and calculate global ion escape rates for the major ion species at present-day Mars (e.g., Ma et al. 2004, 2015; Modolo et al. 2016; Dong et al. 2018). Such modeling works have been also applied to ancient Mars (e.g., Terada et al. 2009; Sakai et al. 2018, 2020).

As reviewed above, comprehensive observations of the Martian upper atmosphere by previous Mars

missions and modelling works have provided the oxygen ion escape rate from present-day Mars and estimate of its integrated loss through time, and similar efforts have been also made for other escape processes such as Jeans' escape of hydrogen, photochemical and sputtering losses of oxygen (e.g., Jakosky et al. 2018, and references therein). However, it is not yet understood whether these oxygen escapes originate from $H_2O$ or $CO_2$ of the Martian atmosphere. Although theoretical estimate of carbon escape rate from present-day Mars is 1–2 orders of magnitude smaller than those of H and O (Gröller et al. 2014; Cui et al. 2019), it could have been comparable to or even greater than the O escape rate in the past (Amerstorfer et al. 2017). In order to understand the integrated losses of $H_2O$ and $CO_2$ through time, determining not only oxygen and hydrogen escape rates, but also carbon escape rate at Mars today and their extrapolation backward in time are equally important. To date a few studies established mass separation methods for IMA and STATIC measurements and identified escaping $O^+$, $O_2^+$ and $CO_2^+$ ions (Carlsson et al. 2006; Inui et al. 2018, 2019) and many multispecies simulation results provided global escape rates of these ion species (e.g., Ma et al. 2004). However, these species could be resolved further into minor species at their neighboring masses such as $C^+$, $N^+$, $Ar^+$, and so on. In addition, recent MAVEN observations in the Mars shadow have revealed cold ion outflow rates that would significantly contribute to the total outflow rate (Inui et al. 2018, 2019). However, the understanding of the cold ion outflow is still shrouded in mystery owing to lack of measurements and difficulty in validation by theoretical studies (e.g., Dubinin et al. 2011; Lundin 2011; Harnett and Winglee 2006; Ma et al. 2004). Precise estimates of the atmospheric and water amounts that have escaped to space in the past remain elusive.

Extracting carbon from the dominant ion populations, such as oxygen ions at present day requires accurate mass separation of these species and has been a challenging subject. The mass spectrum analyzer (MSA) aboard MMX has advantages over its preceding measurements of ion outflows from Mars in terms of (1) high mass resolution measurements of escaping ions at high altitudes and (2) cold ion measurements in the shadows of Mars and Phobos. MSA will achieve unprecedented high mass resolution observations with $M/dM > 100$ at high altitudes (Phobos orbit) to measure ion outflows including tenuous ions such as $C^+$, $N^+$, and $Ar^+$. MSA will also attempt to measure isotope ratios of $O^+$ and $C^+$ and deduce their fractionation factors to understand the long-term evolution of the Martian atmosphere.

The new comprehensive measurements of carbon-, oxygen-, and hydrogen-bearing ion species with high mass resolution of MSA will provide crucial constraints
on H₂O and CO₂ escape rates and its extrapolation backward in time. The extrapolation can be done using a simple approach in Jakosky et al. (2018), i.e., adopt already published models for the time history of escapes, and apply a scaling factor so that the models match the escape rates measured today by the spacecraft. Or, it may be directly derived from measurements of the dependence of the escape rates on solar conditions (e.g., Ramstad et al. 2018). Furthermore, as will be discussed in “Martian sample on the Phobos surface” section, the long-term evolution of oxygen and carbon isotopic ratios in the Martian surface environment may be constrained by the samples brought back by MMX. Combined with the isotopic fractionation factors of outflow ions deduced by MSA, the evolutionary history of the amount of H₂O and CO₂ reservoirs in the Martian surface environment is expected to be further constrained (e.g., Jakosky and Jones 1997).

As for cold ion measurements, MMX will frequently enter the shadows of Mars and Phobos, which will provide a unique opportunity to measure cold ions escaping from Mars. In the shadows, spacecraft is negatively charged, allowing it to measure low-energy ions that cannot be detected in sunlit regions. Observations in the shadow of Phobos will enable the first measurements of cold ions outside the Martian shadow. Previous observations showed that the acceleration mechanisms of the cold planetary ions depend both on tailward distance from Mars and solar wind conditions (e.g., Nilsson et al. 2012; Inui et al. 2019). MSA observations at the fixed tailward distance will provide unique data to assess the effects of solar conditions on the cold ion escape process through the induced magnetotail. Simultaneous observations with other Mars orbiters such as MAVEN and ESCAPADE (ESCape and Plasma Acceleration and Dynamics Explorers) will add extra value to the MSA observations in this context. The knowledge of the solar variation dependence of the cold ion escape process is essential to derive an accurate extrapolation into the past. High mass resolution measurements by MSA also provide valuable opportunity to compare characteristics of different ion species such as O⁺, C⁺, N⁺, and Ar⁺, which will give us critical information to identify major acceleration mechanisms to cause cold planetary ion outflows from Mars.

Moreover, as shown by MAVEN, it is also possible to derive the neutral exosphere density from in situ pickup ion measurements (Rahmati et al. 2018) at distance where no direct measurement of the neutral exosphere is possible and where the neutral exosphere is essentially escaping. In another way, MSA will also have an indirect capability to reconstruct Mars' exospheric neutral escape thanks to its large energy range and mass resolution and

to track the dependency of this escape channel with respect to the solar conditions.

The atmospheric Martian He can be produced by radioactive decay of U and Th in the interiors of the planet followed by surface outgassing (Krasnopolsky and Gladstone 1996), by solar wind implantation (Stenberg et al. 2011) and lost by photo-ionization and acceleration by the solar wind convective electric field (Barabash and Norberg 1994) or by non-thermal escape (Gu et al. 2020). To reconstruct accurately the global balance of the atmospheric He sources can therefore provide key information on the origins of the atmospheric He and a constraint of the intensity of the surface outgassing. MSA by measuring the He⁺ will quantify two key channels of the atmospheric He balance: Solar wind implantation (including the open question of solar wind reflexion at the bow shock (Chanteur et al. 2009)) and solar wind sweeping.

The multi-instrumental sciences of MMX will provide an ideal opportunity to reveal the fate of water of Mars. As will be described in “Fine structure and rapid transport processes of water and dust” section, MMX will measure dust activity and upward transport of water in the Martian atmosphere. At almost the same time, MMX will observe the outflow of ions into space. So, we can clarify the connection between the outflow of ions and the atmospheric events in the lower atmosphere such as dust storms and water ice clouds. Recent observations by Mars orbiters and space telescopes have revealed the importance of high-altitude water for hydrogen escape to space (e.g., Clarke et al. 2014; Chaffin et al. 2017; Heavens et al. 2018; Aoki et al. 2019; Stone et al. 2020; Masunaga et al. 2020). It has also been suggested that the oxygen loss rate may decrease during a dust storm (Lee et al. 2020). Coordinated observations of MSA and the other instruments (see “Instruments” section) aboard MMX will clarify a possible connection between the Martian atmosphere and atmospheric escapes.

Some portion of the escaping ions from the Martian atmosphere will impinge on the surface of Phobos and cause space weathering of the surface layer. We plan to identify the contributions to space weathering of escaping ions through tail and of plume ions, including C⁺, N⁺, etc., to understand the co-evolution of Mars and its moons (Yokota et al. 2021).

## Fine structure and rapid transport processes of water and dust

The previous observations of the lower atmosphere have been mostly done by polar-orbiting spacecrafts (such as Mars Global Surveyor (MGS), MEX, MRO) (e.g., Smith 2002; Kleinböhl et al. 2009). These observations have provided global pictures of the atmospheric species and
aerosols distributions at the Martian atmosphere; however, their diurnal variations have only been investigated using observations at (mostly) fixed local times in the interval 2–3 AM and PM. MEX is not sun-synchronous. So, it can cover all local times in principle, but it takes long time to do it. Thus, hourly development and decay of mesoscale to synoptic scale atmospheric events (such as horizontal water transport including surface–atmosphere interaction, clouds formation, and dust storms, etc.) have remained unclear. The more recent TGO mission already improved this coverage with its inclined orbit (74°) allowing different local times to be probed. The equatorial orbit of MMX, which is driven by the Phobos sample return goals, will be unique in this context. One of the main advantages of the MMX orbit is that we can monitor same regions for a few hours almost every day during a particular period (described in “Baseline operation” section), which allows us to reveal the rapid transport processes of the atmospheric species and aerosols with relatively high spatial resolution (typically 2–5 km/pixel); whereas, it is neither possible for the MMX orbit to observe the polar regions nor to cover all local times in the regions of interest in a single sol. Towards the MMX era, here we briefly review what the previous measurements revealed in terms of water vapor and dust fine structures and their rapid transport processes.

Previous observations have shown that a high variability governs the global-scale water vapor distribution. The seasonal variation of water vapor appears mainly controlled by atmospheric dynamics and sublimation–condensation process between the atmosphere and the polar regions (e.g., Smith 2002; Fouchet et al. 2007; Montmessin et al. 2017). Also, Mars’ water cycle evolves in a steady-state with some interannual variability mostly visible during southern summer (Smith 2004). However, the water cycle remains overall more stable than dust since water sources or sinks are not directly stimulated by the occurrence of dust storms.

Progress in our understanding of the water cycle has been rapid over the last two decades, thanks to the continuous survey performed by several orbiters and also by the maturation of 3D Mars climate models (Navarro et al. 2014; Haberle et al. 2019a; Neary et al. 2020). However, some old questions have resisted interpretation so far. One of them concerns the exchange of water between the regolith and the atmosphere. The puzzling local maxima observed in the low-to-middle latitudes reported by Fouchet et al. (2007) can potentially be explained by dynamics, yet water locally trapped by the subsurface cannot be ruled out. In short, despite a large corpus of dedicated studies, the regolith’s role in the water cycle remains largely elusive. Even if modelers have produced consistent simulations of Mars’ water cycle without a regolith,

suggesting the latter could be neglected at first, observations have left a large gap in bringing the constraints needed to elucidate this role.

One key that could help filling this gap resides in monitoring the local time variation while producing global views of the water vapor column-abundance. That way a closure between the horizontal and the vertical fluxes of water could be tentatively undertaken and some source or sink at/in the surface could then be spotted.

However, the retrieval of water vapor during the nighttime is difficult, if not impossible, for most remote-sensing observations conducted so far (no Sun implies no signal in the near-infrared while the weak thermal contrast between the surface and the atmosphere at night and the colder temperature leave thermal infrared sensors “blind”). Some previous measurements implied that the water vapor abundances could vary daily by a factor of 2–3 (Titov 2002 and reference therein). In contrast, other studies show no significant local time variation (Maltagliati et al. 2011; Trokhimovskiy et al. 2015).

These previous observations were conducted in the context of polar orbits and had to compare data taken at different Mars years or locations to study local time variation. Thus, it has been difficult to directly explore the diurnal cycle except in the polar regions where it is possible to cover different local time in a single orbit (Melchiorri et al. 2009). The MMX Mars observations will investigate the local-time variation of column density of water vapor at low-to-middle latitudes by continuous monitoring from its equatorial orbit. Recent in situ measurements have suggested a strong diurnal variation of local water vapor abundances on the surface at low-to-middle latitudes (e.g., Savijärvi et al. 2019), and the MMX measurements will provide a comprehensive view on the surface–atmosphere interaction of water by remote-sensing observations.

Another piece of the water cycle puzzle still missing concerns its local distribution. Only two instruments—OMEGA onboard MEX and Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) onboard MRO—have had capability to investigate mid-resolution maps of water vapor (<5 km), but were limited in their total swath to a few hundred km, making it impossible to contextualize the observed fine structures (see e.g., Melchiorri et al. 2009). The latter authors identified a fine structure of water vapor enhancement correlated with surface albedo map, arguably caused by surface–atmosphere interactions. Maltagliati et al. (2008) investigated high-resolution maps of water vapor over the Tharsis volcanoes. They found a peculiar water vapor enrichment on the top of volcanoes that could be caused by local circulation around the volcanoes (e.g., Rafkin et al. 2002). Such a local upward topographically
forced transport may contribute to the formation of water detached layers, as suggested in Heavens et al. (2019). The MMX observations of Mars will monitor water vapor at high spatial resolution and provide a global view that shall help better characterizing the existence of fine structures and of potential exchanges between the atmosphere and the regolith. The detailed capability of MMX Mars observations is described in the next section and summarized in Table 2.

Recent observational and modeling work about dust transport processes on Mars highlighted both the fine-scale structure of dust storms and the rapid vertical transport they imply. The key role played by the radiative warming by dust particles in dust storms has been recognized at all scales, from local to global (Heavens et al. 2019). This makes the dynamics of dust storm and dust transport processes very likely to be developing over a couple of hours, as shown both by modeling (e.g., “rocket dust storms”, Spiga et al. 2013) and observations (e.g., “textured dust storms”, Guzewich et al. 2017). One of the most striking recent results is the enhanced transport of water vapor to the upper atmosphere of Mars, and surge in atmospheric escape of hydrogen, especially during global dust storms (Fedorova et al. 2018, 2020; Vandaele et al. 2019; Aoki et al. 2019; Stone et al. 2020) in which dusty deep convection occurs (Heavens et al. 2018; Shaposhnikov et al. 2019; Neary et al. 2020). The MY34 (Mars Year 34) dust storm illustrated how strong and rapid vertical transport of dust particles can be (Bertrand et al. 2020) and how the diurnal variability of dust optical depth is stronger than initially thought, as a result of vertical and horizontal transport processes (Kleinböhl et al. 2020; Montabone et al. 2020; Liuzzi et al. 2020). Many of the aforementioned results and interpretations were, however, obtained from a combination of sun-synchronous orbital observations and atmospheric modeling. The complete life cycle of a dust storm, the rapid development of convective units within the storm cluster, and the vertical extent and magnitude of dust transport have never been observed on Mars. This is where the peculiar orbit and multi-instrumental payload of MMX

may play a role in permitting to broaden the knowledge of dust transport processes on Mars.

## Martian sample on the Phobos surface

MMX plans to collect a sample of at least 10 g from the regolith of Phobos (Usui et al. 2020). The surface of Phobos is likely to exhibit evidence of meteoritic ejecta from Mars (Ramsley and Head 2013; Nayak et al. 2016; Hyodo et al. 2019). The Martian ejecta on Phobos represent Martian topsoil accumulated over geologic time, which may include various materials different from Martian meteorites. Recent work by Hyodo et al. (2019) estimate that several hundreds of ppm of Martian ejecta is mixed within the Phobos regolith. Within a decade, MMX may collect rare Martian materials along with the Phobos regolith, providing new insights into the environment and possible habitability of early Mars. In this subsection, we briefly review what we currently know about the Martian surface evolution from the geological and mineralogical records on Mars and the geochemical records in Martian meteorites. Usui et al. (2020) summarizes the scientific importance of the Phobos sample. More specific strategies for the initial analysis and the curation process are proposed by Fujiya et al. (in prep.) in this same volume.

Geological and mineralogical records on the Martian surface indicate that the red planet was not red early in its history. Recent Mars exploration missions have reported conclusive evidence for the past existence of liquid water and a thicker atmosphere and the global-scale transition to the currently cold desert-like surface condition (e.g., Bibring et al. 2006; Carr and Head 2010; Ehlmann and Edwards 2014; Usui 2019a). The Noachian Martian (> ~3.7 Ga) terrains are characterized by significant fluvial erosions, dense valley networks, lakes and rivers, as well as active volcanism and massive impact cratering (e.g., Craddock and Howard 2002; Fasset and Head 2008). Secondary phyllosilicates, such as Fe/Mg smectite and chlorites were identified throughout Noachian regions (Bibring et al. 2006; Ehlmann et al. 2011; Ehlmann and Edwards 2014). The widespread occurrence of the fluvial landforms and the hydrous minerals suggest, episodically, if not continuously, warmer and water-rich conditions

<table><caption>**Table 2** Summary of the MMX capability for Mars observations</caption><thead><tr><td>Instrument</td><td>Spatial resolution<sup>a</sup></td><td>Temporal resolution</td><td>Mass resolution</td><td>Targets</td></tr></thead><tbody><tr><td>MIRS</td><td>~ 2.5 km</td><td>1 h</td><td></td><td>Dust, H<sub>2</sub>O, CO<sub>2</sub>, Water ice clouds, CO<sub>2</sub> ice clouds, surface pressure, O<sub>2</sub> dayglow</td></tr><tr><td>TENGOO</td><td>~ 35 m</td><td>1 min</td><td></td><td>Dust events, water ice clouds</td></tr><tr><td>OROCHI</td><td>~ 2.5 km</td><td>15 min</td><td></td><td>Dust events, water ice clouds</td></tr><tr><td>MSA</td><td></td><td>> 4 s</td><td>M/ΔM ~ 100</td><td>ion outflows including C<sup>+</sup>, N<sup>+</sup>, O<sup>+</sup>, and Ar<sup>+</sup></td></tr></tbody></table>

<footnote><sup>a</sup> Spatial resolution at the sub-spacecraft point when observing from QSO</footnote>
during the late Noachian/early Hesperian (e.g., Ramirez and Craddock 2018), although the nature of the ancient climate remains a matter of debate (see “Martian paleoclimate” section). During the late Noachian to early Hesperian, the surface mineralogy also gradually shifted from phyllosilicates to carbonate and sulfate-rich assemblages, suggesting monotonic acidification of the fluid chemistry (Ehlmann et al. 2011; Ehlmann and Edwards 2014; Usui 2019a). The overall geomorphologic and mineralogical findings indicate a global transition from an early Earth-like Mars to the currently cold desert-like surface. In contrast to the earlier periods, most Amazonian terrains (< ~ 3.0 Ga) are characterized by anhydrous oxide-rich mineralogy suggestive of scant fluvial activity, although massive amounts of water ice and/or icy sediment might be hidden beneath the surface (Usui 2019a).

Geochemical information obtained from Martian meteorites is another important clue. Most known Martian meteorites are basaltic or ultramafic in composition and subdivided into three mineralogical groups: shergottites, nakhlites and ch assignites (McSween and McLennan 2014; McSween 2015 and references therein). Their Martian origin was originally determined via measuring the isotopic compositions of the trapped gases within impact-melted glasses from some meteorites (Bogard and Johnson 1983). The others are linked by oxygen three isotopic compositions (Clayton and Mayeda 1996) as well as other geochemical characteristics (e.g., Agee et al. 2013). Magmatic crystallization ages are relatively recent (~1.3 Ga to 0.2 Ga; Nyquist et al. 2001) and represent mostly anhydrous Amazonian conditions, although some rocks contain the trace aqueous weathering products that formed at the near-surface system (Bridges et al. 2019). On the other hand, a few old rocks have been classified as irregular Martian members, such as a 4.1 Ga orthopyroxenite, ALH 84001 (Mittlefehldt 1994; Lapen et al. 2010) and an ancient basaltic breccia, NWA 7034 and its paired meteorites (Agee et al. 2013). The various igneous lithologies found in the NWA 7034 series are likely to have formed by intensive magmatic and/or impact events during at Noachian age of 4.43 Ga to ~4.3 Ga (Humayun et al. 2013; Bellucci et al. 2015; Nyquist et al. 2016; Cassata et al. 2018), although their whole rocks experienced the prolonged thermal metamorphism during early to middle Amazonian period. Hence, only ALH 84001 is known to have preserved Noachian near-surface materials in its alteration deposits to date (e.g., Borg et al. 1999; Halevy et al. 2011; Bridges et al. 2019). Nevertheless, sporadic, but large variations of the formation and/or metamorphic ages of the Martian meteorites enable us to estimate the fate of the ancient Martian water cycle over time.

The atmospheric D/H ratio is one of the most informative tracers for the Martian surface evolution (Usui 2019b), as its isotopic fractionation likely reflects temporal variations in the near-surface hydrologic cycle and atmospheric escape. The current Martian atmosphere and the surface regolith are known to have a D/H ratio that is ~6–8 times higher than that of terrestrial ocean water (e.g., Owen et al. 1988; Webster et al. 2013; Leshin et al. 2013). Such extremely high D/H ratio resulted from a preferential escape of the lighter isotope (¹H), suggesting that the Martian atmosphere was irreversibly lost over geologic history (Lammer et al. 2013; Kurokawa et al. 2014). Igneous and/or secondary hydrous phases in the Martian meteorites record the past D/H ratio of the various water reservoirs. The igneous water (OH)-bearing minerals and hydrous glasses in the young (<1 Ga) meteorites have comparable D/H ratio to the current Martian atmosphere (Greenwood et al. 2008; Hu et al. 2014), suggesting that their water reservoir was in equilibrium with the near-surface atmosphere. The D/H ratio of the Noachian crustal water recorded in the ALH 84001 was reported to ~4 times as high as the terrestrial value (Greenwood et al. 2008). This implies that the Martian atmosphere and surface water had been extensively lost prior to 4 Ga (Kurokawa et al. 2014), although modest D/H ratios were also proposed for ALH 84001 (Sugiura and Hoshino 2000; Doctor et al. 2003).

Along with the surface water records, the D/H ratio of the Martian primordial water is another essential piece of information for understanding the global evolution. Previous studies estimate that the Martian mantle has retained its primordial water, whose D/H ratio is similar to or slightly higher than the terrestrial water (Leshin 2000; Usui et al. 2012). However, the mantle water abundance may be quite low (<100 ppm; Usui et al. 2012; McCubbin et al. 2016), at least in Martian meteorite source regions. In addition to the surface and interior (primordial) water, the existence of another water reservoir on current Mars is predicted (Usui et al. 2015; Mahaffy et al. 2015) based on D/H studies of Martian meteorites and hydrous minerals from 3 Ga Gale Crater mudstones. Subterranean water ice, icy sediments, and/or hydrated minerals are plausible candidates for this potential hidden Martian water, which has been kept isotopically isolated from the near-surface environment over geologic history. Indeed, massive ground ice layers have been geologically identified by recent observations (Mouginot et al. 2012; Dundas et al. 2018). If the hydrous subsurface has been retained under the dry, cold and oxidizing surface of Mars, ancient Martian life, if any, might have survived within the subsurface until today (Usui 2019a, b and references therein).
In addition to the D/H ratios, other atmophile com-
ponents are important tracer of the Martian surface
evolution. Compared to the terrestrial atmosphere,
the present-day Martian atmosphere is character-
ized with isotopically heavy carbon dioxide (CO₂) with
δ¹³C = 46 ± 4 ‰ (Webster et al. 2013), dinitrogen (N₂)
with δ¹⁵N = 572 ± 82 ‰ (Wong et al. 2013) and noble
gases such as ²⁰Ne/²²Ne = 10.1 ± 0.7 (Pepin 1991) and
³⁶Ar/³⁸Ar = 4.2 ± 0.1 (Atreya et al. 2013). Those are
results of the complicated atmospheric evolutions via
thermal and non-thermal escapes (e.g., ion pic up, sput-
tering, impact erosion) and replenishment by impacts
and/or magmatism (Lammer et al. 2020). Lifetimes of N₂
and light noble gases are estimated as shorter than the
age of Mars, indicating that their present-day isotopic
compositions reflect the recent (< 4 Ga) atmospheric loss
and input balance (Lammer et al. 2020). On the other
hand, Xe in the Martian atmosphere is an important clue
for the ancient environmental shift. Xenon, the heavi-
est noble gas with nine stable isotopes (124, 126, 128,
129, 130, 131, 132, 134, 136), is more difficult to escape
compared to the lighter noble gases via mass-dependent
thermal processes. Nevertheless, its isotopic composi-
tions (¹Xe/¹³²Xe) show significant fractionations both
in the terrestrial and Martian atmosphere (Conrad et al.
2016; reviewed by Avice and Marty 2020). Such Xe frac-
tionation can be attributed to the ancient hydrodynamic
escape triggered by the EUV radiation from young Sun.
Moreover, the Xe fractionation can also be caused by the
ionic coupling with escaping hydrogen (H) originated
from the surface water. Cassata (2017) reported that the
4 Ga atmospheric Xe trapped in ALH 84001 (and prob-
ably, NWA 7034, as well) seems to be already isotopically
fractionated to the present level, suggesting that the Mar-
tian Xe had intensively escaped during early Noachian
era, which had ceased prior to 4 Ga. This is opposite to
the Earth case, where the atmospheric Xe continued to
fractionate for ≥ 2 billion years, coupled with the surface
water escape (Avice and Marty 2020). The early cessation
of the Martian Xe fractionation indicates disappearance
of the permanent liquid water on Mars prior to 4 Ga,
which is consistent with the other geochemical and geo-
logical implications.

The case of Martian atmospheric nitrogen (N₂) appears
to be somewhat different from the Xe evolution. Its pre-
sent ¹⁵N/¹⁴N ratio is known ~ 1.6 times as heavy as the
terrestrial value (i.e., δ¹⁵N = 572 ± 82‰; Wong et al.
2013), although the Noachian atmosphere trapped in
ALH 84,001 showed very little ¹⁵N enrichments (Mathew
and Marti 2001). It is suggested that the Martian ¹⁵N/¹⁴N
ratio was elevated by later atmospheric evolution (< 4 Ga
to present). Because of the lack of Martian surface sam-
ples aged between 4 and ~ 0.5 Ga, this evolution history

remains unsolved. Meanwhile, some Martian meteorites
and the Martian soils analyzed by MSL recently sug-
gested the presence of “fixed nitrogen” such as nitrate
and N-bearing organic matter (e.g., Kounaves et al. 2014;
Stern et al. 2015; Koike et al. 2020), whose isotopic com-
positions would provide further constraint on the Mar-
tian surface evolution.

Isotopic composition of carbon (¹³C/¹²C) is somewhat more complicated. Carbon dioxide (CO₂) dominates the current Martian atmosphere and is involved in various planetary processes, including volcanic degassing, atmospheric escape, formation of carbonate minerals and organic matter and their possible preservation at the Martian subsurface system (Hu et al. 2015; Bridges et al. 2019; Kounaves and Oberlin 2019). Present-day Martian atmospheric CO₂ has heavy ¹³C/¹²C ratio of δ¹³C = 46 ± 4 ‰ referenced to the Vienna Pee Dee belemnite (VPDB) analyzed by Curiosity rover (Webster et al. 2013). The heavy ¹³C/¹²C was also reported for young Amazonian-aged meteorite (δ¹³C up to ~ 40‰; Carr et al. 1985), while Martian mantle-derived ¹³C/¹²C is estimated to be much lighter. The 4 Ga carbonates in ALH 84001 also has high δ¹³C value of ~ 27 to 64 ‰ (Niles et al. 2005), probably reflecting the isotopically heavy Noachian atmosphere. If the ALH 84001 carbonates represent the 4 Ga atmospheric δ¹³C value, the Martian atmosphere is inferred to have extensively escaped by that time and have been kept without severe change over the next ~ 4 billion years. On the other hand, Hu et al. (2015) consider that the Martian atmospheric ¹³C/¹²C records more recent (from 3.8 Ga to present) evolution, from which they estimate the atmospheric pressure of ≤ 1 bar for the Noachian Mars. In contrast to the carbon isotopes, the oxygen isotopic ratios (¹⁸O/¹⁶O) in the Martian atmosphere and water vapor are considered to be buffered by large O-reservoirs on Mars, such as the crustal rocks and the near-surface ice (Webster et al. 2013).

Although we have learned much from the study of
Martian meteorites, retrieving the whole Mars his-
tory from current meteorite collections is highly chal-
lenging, especially regarding the evolution of the early
environment (Noachian to Hesperian), mainly because
of the following difficulties. The first concern is pos-
sible contamination of the Martian rocks by terres-
trial water, air and/or organic matter. Most Martian
meteorites land resided on terrestrial hot deserts or
Antarctic ice and weather for a long time before they
are finally collected. Even ‘fall meteorites’ (those col-
lected shortly after their arrival to Earth) may have
been affected by the terrestrial surroundings within a
short time (Stephant et al. 2018). Contamination would
also occur during laboratory processing (although this
can be reduced by recent technical improvements).
Second, and possibly fatal, is the sampling bias of Mar-
tian meteorites. As noted above, most Martian mete-
orites are middle-to-late Amazonian igneous rocks
(Nyquist et al. 2001; McSween and McLennan 2014).
The only one Noachian igneous rock (i.e., ALH 84001;
Mittlefehldt 1994; Lapen et al. 2010) and one Noachian
clast-bearing breccia (i.e., the NWA 7034 series; Agee
et al. 2013; Humayun et al. 2013) were found. The lat-
ter suffered severe metamorphism during Amazonian
age. No meteorite contains Hesperian-aged materials.
The cause of such sampling bias has been unsolved,
although severe shock effects during meteoritic ejec-
tion (with the peak shock pressures up to ~ 15–45 GPa;
Nyquist et al. 2001) may be a dominant reason. In order
to escape from the Martian gravity and reach Earth,
the rock had to be accelerated to > ~ 5 km/s probably
by a heavy impact. In such ejecta, fragile sedimen-
tary materials including the aqueous alteration phases
(e.g., clays, carbonates, sulfates, and chlorites) and the
organic compounds should have been broken and lost
before arriving to Earth as “meteorite”. On the other
hand, ejecta with much lower velocity (i.e., lower shock
pressure) can reach to the surface of Phobos (Ramsley
and Head 2013; Nayak et al. 2016; Hyodo et al. 2019).
This suggests that the Martian sedimentary materials,
which are quite important for the Mars surface history,
but rarely found in the Martian meteorites, have been
accumulated and preserved on the surface of Phobos
(Usui et al. 2020).

The recent calculation estimates that at
least > 340 ppm of Martian ejecta is mixed in with Pho-
bos regolith (Hyodo et al. 2019), suggesting that more
than ~ 30 grains out of the 10-g Phobos sample col-
lected by the MMX sampling system will have a ‘Mar-
tian’ origin. As the Martian ejecta can be delivered to
Phobos by numerous random impacts, the obtained
Martian grains may represent various geological eras
on Mars and cover the whole evolution history. These
Martian grains in the regolith on Phobos with a typical
grain diameter of 300 µm is expected to contain more
than one “chronometer” mineral (e.g., zircon, baddeley-
ite, or Ca-phosphate for U–Pb dating) in the case that
the typical size (< 30 µm) and abundance (~ 0.1–1%)
of chronometer minerals are comparable to those of
Martian meteorites (McSween 2015). The chronometer
minerals record the timing of formation and/or meta-
morphism of the individual grains. Thus, ~ 30 Martian
grains returned by MMX would provide a wealth of
“time-resolved” information on the evolution of Mar-
tian surface environments because these grains would
have been transported randomly from any of the seven
geologic units. More importantly, this will enable us to
obtain precise isotopic compositions of key volatiles

reviewed above (i.e., D/H, δ¹³C, δ¹⁵N and noble iso-
topes) via in situ analyses of the individual grains.

The surface mineralogy and chemistry of Phobos
depends on its origin (summarized by Usui et al. 2020).
In the captured (D- or T-type) asteroid origin hypothesis
(Murchie and Erard 1996), the endogenous regolith on
Phobos may present chondritic chemistry and mineral-
ogy, probably like those of carbonaceous chondrites. On
the other hand, if Phobos had formed through a giant
impact on early Mars instead (Rosenblatt et al. 2016;
Hyodo et al. 2017), its regolith may originate in Martian
interior rocks with high temperature-pressure phases
and the bulk Martian chemistry. Whatever the origin
of the endogenous materials on Phobos, however, the
exogenous grains (i.e., the Martian ejecta on Phobos)
can be clearly distinguished based on their mineralogy
and chemistry and will be confirmed by analyses of sta-
ble isotopes, including O, Cr and Ti. Once the grain is
recognized as ‘Martian’, a series of organic and inorganic
analyses will be investigated on the individual grains,
including the volatile isotopic compositions, the U–Pb
and other radiometric chronology, remnant magnetiza-
tion, as well as possible Martian biosignature. Further
analytical strategies and expectations are provided by
Fujiya et al. (this volume).

Mars observation by MMX

Orbit and observation window

MMX will travel in a cruising orbit to Mars for 1 year,
observe Mars and its moons for 3 years from 2025 to
2028, and eventually bring back collected samples to the
Earth after a 1-year journey. During most of its 3-year
mission, MMX trajectory will be in Quasi-Satellite Orbit
(QSO) around Phobos, which is very similar to Phobos
orbit around Mars: nearly equatorial and circular, with

<figure><img src="image_6.png" /><figcaption>**Fig. 1** A schematic view of QSO. The spacecraft is orbiting Mars near Phobos, but from Phobos it appears as if the spacecraft is orbiting Phobos</figcaption></figure>
a period of 7h40' and distance of about 9,376 km from the Mars center (about 6000 km from the Mars surface) (Fig. 1). The detailed descriptions of QSO orbits and definition of the mission phases can be found in the companion paper in this special issue. In operation on Mars Moon proximity, remote sensing for atmospheric phenomena and in situ measurement for atmosphere escaping are continuously conducted on QSOs as a home position throughout the mission from Mars Orbit Insertion (MOI) in Phase 0. After arrival on Phobos QSO on October 2025, the landing site selection and the touchdowns to Phobos surface have the first priority over all considerations during the first one-half years from October 2025 to July 2027 as defined in Phases 1, 2, and 3. Mars observation will be made during the first one-half of year without interfering with Phobos observations or its data transfer (e.g., while on the nightside of Phobos). In the latter half of the mission from August 2027 to September 2028 as defined in Phases 4 and 5, we will have much more time to focus on Mars observations. Especially, the transfer orbits during Deimos flyby in Phase 5 will allow to explore Mars' surface and atmosphere with a different perspective thanks to elliptic orbits that enable the time-resolution observation of larger area than in QSO thanks to the increase on distance and decrease on ground speed around apoapsis.

Mars observation by MMX from the Martian equatorial plane (inclination of ~1°) has several assets. This circular orbit is relatively close to Mars when comparing to the areostationary orbit. MMX orbital motion (0.013°/s with the period of 7h40') will be faster than the rotational period of Mars (0.004°/s). As a consequence, the difference of rotation rate drifts the subsatellite point around 0.009°/s. In 7h40', subsatellite point shifts ~248° eastward. After three orbits of 7h40' (~23 h), subsatellite point has shifted of ~744° = $2 \times 360° + 24°$, so MMX is located above a longitude 24° east of that three orbits ago. Quasi-areostationary orbiters are innovative platforms for space-born Mars science, as has been geostationary satellite imagery which revolutionized Earth weather forecasting from 1970s. The first equatorial orbiters will blaze a trail for the continuous remote sensing of the Martian atmosphere. Remote sensing from high orbit will enable to work in conjunction with satellites in polar or eccentric low-altitude orbits, which provide truly global coverage and synergistic perspective. From the equatorial plane, it is however noted that the apparent visible disk of Mars takes up a field of view of about ~43°. The coverage reaches up to approximately 68° latitude. In addition, the equatorial orbit of MMX will essentially increase opportunities to directly measure the low-energy outflow of ionospheric ions from Mars in the inner magnetosheath, which has been poorly understood so far.

## Instruments

The mass spectrum analyzer (MSA) is a scientific instrument onboard the MMX spacecraft, which consists of an ion energy mass spectrometer and two magnetometers (Yokota et al. 2021). The ion spectrometer measures distribution functions of low-energy (<10 s keV) ions and their mass/charge distributions using a top-hat electrostatic energy analysis and a linear-electric-field time-of-flight mass analysis. The fluxgate magnetometers measure the vector magnetic field of the solar wind, which is occasionally perturbed by Mars and possibly Phobos in their neighborhood. The MSA experiment is designed to perform in situ observations of secondary ions emitted from Phobos, water ions generated from the Phobos torus if exists, and escaping ions from the Martian atmosphere with monitoring the solar wind. The MSA is developed based on the techniques used for previous space plasma missions such as KAGUYA (Yokota et al. 2005; Saito et al. 2010; Tsunakawa et al. 2010), ARASE (Yokota et al. 2017; Asamura et al. 2018; Matsuoka et al. 2018), Bepi-Colombo/MIO (Delcourt et al. 2016; Saito et al. 2020). Thus, the performance is similar to that of typical space plasma instruments except the mass resolution of $M/\Delta M \sim 100$, because the MSA will measure heavy ions and their isotopes coming from the Martian atmosphere to estimate the amount of the atmospheric escape. MMX will be located in the Mars shadow (eclipse) at approximately half of the year. In these periods, MMX will measure escaping ions in the magnetotail. In other periods, MMX will observe the solar wind. Seasonal variation of the MMX orbit with respect to the magnetotail can allow us to observe the longitudinal-latitudinal structure of escaping ions at 6000 km distance from Mars.

Since the MSA ion analyzer has a hemispherical field-of-view, solar wind ions can be continuously caught at the same time in many cases of the MMX nominal observation. Escaping ions from the Martian atmosphere will be measured when the spacecraft is in the Martian tail region together with Phobos. Only to observe secondary ions emitted from Phobos, the surrounding electric field must direct from Phobos to the spacecraft, because the ions with initial energies of ~0 eV travel along the electric field to the spacecraft.

Optical radiometer composed of chromatic imagers (OROCHI) is designed for capturing spectral features of Phobos from ultraviolet to near-infrared wavelengths with 7 wide-angle bandpass imagers and 1 panchromatic imager. Detailed information of design and performance of OROCHI is introduced in Kameda et al. (2021).

The field of view (FOV) of each imager is >1 rad and the instantaneous FOV (iFOV) is 0.4 milli-radian. Figure 2 shows how Mars will be observed in the OROCHI's FOV. Because of the wide FOV, OROCHI can capture
<figure><img src="image_7.png" /></figure>

whole disk of Mars in its FOV from the Phobos altitude with the pixel resolution of 2.4 km.

Since the orbit of MMX is similar to the Phobos orbit (see "Orbit and observation window" section), which is almost a circular orbit around Mars, OROCHI will observe Mars from almost same altitude (~6000 km), and thus it will provide images with a stable spatial resolution. Besides, OROCHI can monitor a specific region for more than 3 h with 2.4 km/pixel resolution and an interval of 15 min. This will give critical information for understanding how local/regional dust storms develop. The dataset from OROCHI is similar to those from a geostationary weather satellite whose spatial and temporal resolution are the order of 1 km and 10 min, respectively. Also, thanks to its wide FOV, OROCHI can observe a wide range of local time from morning to evening in one observation. It will also give a lot of information about local time dependence or morning-evening symmetry/asymmetry.

The center wavelengths of the OROCHI bandpass filters are 390 nm, 480 nm, 550 nm, 650 nm, 730 nm, 860 nm, and 950 nm, and designed signal-to-noise (S/N) ratio for spectral analysis (i.e., band ratios) is 100 (Kameda et al. 2021). For Mars observation, the blue and red bands will be mainly used for monitoring atmospheric dynamics. Dust and water ice clouds can be roughly distinguished based on a difference in brightness between the two bands. The high SN ratio is enough to resolve the difference in the photometrical properties between dust and water ice (c.f. Bell et al. 2009). The near-infrared band (950 nm) will be also important to connect the OROCHI images and MIRS data since the wavelength is commonly used by both instruments, then more detailed spectral analysis will be possible.

Telescopic Nadir imager for GeOmOrphology (TEN-GOO) is a panchromatic (370–850 nm) imager with a quite high spatial resolution, <6 µ-radian/pixel, which is 60 times higher than that for OROCHI. The high spatial

resolution allows to observe the Martian surface with a resolution of 35 m/pixel from the altitude of Phobos, thus we can analyze sub-km scale atmospheric phenomena from TENGOO images. TENGOO's FOV is 0.82 × 1.1°, which corresponds to 86.5 × 115.5 km region in one TENGOO FOV when observing Mars from the QSO.

Figure 3 shows examples of images that we expect TENGOO will take. The images were made from Context Camera (CTX) onboard Mars Reconnaissance Orbiter whose spatial resolution is 6 m/pixel (Malin et al. 2007). To simulate TENGOO observation from a CTX image, every 6 × 6 pixels of the CTX image are merged into one pixel and Gaussian smoothing is performed with full width at half-maximum (FWHM) = 1.8 pixel based on a high-resolution camera onboard Hayabusa-2 (Kameda et al. 2017). Even after the pixel merging, fine-scale dust streams can be clearly seen in the image (the event was introduced by Malin et al. 2009). Therefore, TENGOO is expected to resolve finer structures in dust storms and ice clouds with spatial scales of about 10 km. We may understand a short timescale variation of a local dust storm by sequential observations with TENGOO.

Same as OROCHI, the most significant advantage of TENGOO observation is that TENGOO can conduct a sequential observation for several hours which is critical for understanding short timescale atmospheric phenomena on Mars. Thanks to the high spatial resolution of TENGOO, we may track sub-km scale dust flows, and then we will be able to retrieve a local wind distribution in the FOV of TENGOO. TENGOO was originally designed to observe Phobos, not Mars. However, it allows us to make some significant observations described above. We plan to propose observations of Mars using TENGOO ("Observation campaign" section).

MMX InfraRed Spectrometer (MIRS) is a push-broom imaging spectrometer in the near-infrared spectral range (0.9 to 3.6 µm). MIRS detector is a 2D array providing image of a strip in one spatial direction with the spectrum
<figure><img src="image_8.png" /></figure>

of each point in the spectral direction. A second spatial direction is provided by the instrument line of sight in the along-track direction of MMX. MIRS FOV is $\pm 1.65^\circ$ and while targeting a spatial resolution of 10 km on Mars, MIRS expected geometric resolution on Mars from Phobos orbit is $\sim 2$ km so spatial binning can be implemented to increase signal-to-noise ratio and decrease data volume. MIRS has a spectral resolution of about 20 nm and a targeted signal-to-noise ratio above 100 for features of interest. Further detailed information on the instrument can be found in Barucci et al. (2021).

MMX quasi-circular orbit with a period of $\sim 7$ h, will provide more than 3-h windows to MIRS. Different observation strategies will be possible to maximize either temporal or spatial coverage of MIRS monitoring of Martian atmosphere, from 30' time resolution observation of a limited zone to a complete coverage in a few orbits (see Barucci et al. 2021). MIRS will also perform limb observations to obtain information on Martian atmosphere at high vertical resolution.

MIRS observations will be used to constrain transport processes for dust and water in the Martian atmosphere, observations of the equatorial to mid-latitude distributions of dust storms, water ice clouds and water vapor. $CO_2$ (and thus pressure) will be monitored through $CO_2$ 2.0 µm band. Water vapor will be monitored on a daily basis using its 2.6 µm band (Maltagliati et al. 2008) and water ice clouds through their spectral features between 0.9 and 3.6 µm (Vincendon et al. 2011). MIRS will be able to detect CO and $O_2$ with their 2.35-µm and 1.27-µm bands, respectively. MIRS will also provide monitoring of the atmospheric dust content and of water adsorbed in the surface regolith. Finally, in collaboration with the OROCHI and TENGOO instruments, it will also be

possible to investigate $CO_2$ clouds following the procedure proposed by Vincendon et al. (2011).

By providing long-term monitoring of multiple Martian atmosphere constituents, MIRS observations, together with the ones from MSA, OROCHI and TENGOO, will help better understand the interdependencies of these species and their roles in the Martian water, $CO_2$ and dust cycles.

## Baseline operation

Once inserted into QSO, the spacecraft will spend most of its time in this QSO. Therefore, the basic operation for Mars observation should be planned for the period that the spacecraft stays in the QSO before and after touchdowns on Phobos. Basically, when the spacecraft stays on the dayside of Mars and the nightside of Phobos, we can allocate observation time to Mars. This is because most of the time on the dayside of Phobos will be spent on remote-sensing observation of Phobos, and our instruments are not sensitive enough to observe the night-side of Mars. The orbital period of Phobos is approximately 7 h and 40 min (0.31 sols, mean solar day on Mars). Thus, while the spacecraft is in the QSO, it enters the day and nightsides of Mars every 3 h and 50 min. On the other hand, the pseudo-orbital period of the spacecraft around Phobos depends on the mean distance between the spacecraft and the surface of Phobos. It is about a month when the spacecraft is in orbit at a distance of 100 to 200 km from the Phobos surface, called QSO-H. It is roughly four (Earth) days in orbit at a distance of 50–90 km, called QSO-M. Finally, it is roughly 12 h in orbit at a distance of 30 to 50 km from the Phobos surface, QSO-L. Figure 4 shows the case of QSO-H. The period of the Phobos dayside where Mars is not observable lasts for half a month, followed by the period
<figure><img src="image_9.png" /></figure>

of Phobos nightside where Mars is observable for half a month as shown in Fig. 4a. Thus, only during the latter half of the month, observation time for Mars, the dayside of Mars, lasts 3.84 h every 7.67 h. The observable longitude range is shifted by about 120° to the west in each orbit around Mars. If we focus on a certain longitude, the next opportunity for continuous observation of that longitude will be one day later, and slightly earlier in local time (Fig. 4b, c). For example, if the sub-spacecraft point on Mars passes through 0°E at about 14:30LT, we can observe 0°E at about 11:30LT the next day. Figure 5 shows the case of QSO-M. The dayside of Mars is observable for 3.84 h every 7.67 h, the same as QSO-H, but the nightside of Phobos where Mars is observable lasts for 51 h every 102 h, overlapping with series of the day and nightsides of Mars. The observable longitude range will be shifted by about 120° to the west in each orbit around Mars, as in the case of QSO-H (Fig. 5c). Tendencies of the longitude and local time of the sub-spacecraft point are the same as in the case of QSO-H. The difference from the case of QSO-H is that the spacecraft enters the dayside of Phobos after about 2 days (Fig. 5c). It means that we will not be able to observe Mars. On QSO-L, the nightside of Phobos where Mars is observable lasts for 12 h every day. The total time to observe Mars within a given period

does not change for the three types of QSOs. For example, the total time that we can observe Mars in a month is about 180 h, quarter of a month.

Regardless of the type of QSO that the spacecraft stays in, the continuous observation time of 3 h 50 min remains the same. During this time, OROCHI continues to acquire a multi-colored full-disk image every 15 min. High temporal resolution observations of terrestrial dust events in the Middle East by the Spinning Enhanced Visible and Infrared Imager (SEVIRI) onboard Meteosat Second Generation (MSG) show that the number of dust events detected at 30-min intervals is clearly lower than that at 15-min intervals, especially during the summer months (Hennen et al. 2019). This is expected to enable us to monitor in detail the development of small-scale dust events over a wide area in low and mid-latitudes. The MIRS also continues to acquire several stripes with all the wavelengths during the observation time of 3 h 50 min.

The MMX is a three-axis stabilized spacecraft with a high gain antenna (HGA) fixed on the side (+X plane), and a medium gain antenna (MGA). As the HGA has a radiation pattern with a narrow beam width, the HGA boresight direction is precisely controlled toward the Earth for communications, while MGA takes advantage
<figure><img src="image_10.png" /></figure>

of the flexibility of the spacecraft's attitude and orientation control. In the nadir observation mode for atmospheric remote sensing, the -Z-axis boresighted along the viewing axes of the optical instruments is maintained towards the center of Mars (Fig. 1). Orientation is a spacecraft resource that has to be shared with Phobos observations. The slew maneuver from one orientation to another is required in order to switch between Mars observation and Phobos observation during QSOs. The spacecraft's slewing capabilities will also be used during observations of Mars in order to maximize the coverage of the MIRS on Mars disk, in combination with its scan mirror. The MIRS scans the area of interest from low to mid-latitudes within an hour. Along-track and cross-track scans are done by the MIRS's scan mirror and the maneuver of the spacecraft, respectively. We are also considering extending the observable latitudinal range by increasing the scan speed of the mirror while maintaining the temporal resolution, although the spatial resolution will be reduced. In any case, MIRS provides hourly horizontal distributions of quantities important to Martian meteorology around the area of interest, such as the amount of water vapor and dust.

## Observation campaign

The basic operations described in the previous subsection alone can produce significant results. During the baseline operation, however, the optical instruments

are basically either pointing at the center of Mars or scanning in the cross-track/along-track directions. This means that the east and west Martian limbs are not in the field of view of the instruments other than OROCHI. We plan to conduct several limb observation campaigns, using MIRS, which will allow us to observe the limb over a wide latitudinal range within an hour, and to obtain vertical profiles of dust, water vapor, ice clouds, and dayglow/nightglow, etc. (e.g., Vasilyev et al. 2009). Sánchez-Lavega et al. (2018) reported the temporal variation of detached clouds and dust seen in limb observations by Visual Monitoring Camera (VMC) onboard MEX. The vertical resolution of VMC depends on the altitude of MEX above the Mars surface and ranged from 350 m to 8.5 km in their cases. If TENGOO is pointed at the limb at a high frequency (e.g., 1 image/min) by the maneuver of the spacecraft, it may be possible to track the temporal changes in the vertical distribution of dust and clouds with much higher vertical resolution than that of VMC. And if this coincides with the MIRS limb observations, it will be easier to distinguish between dust and clouds. In this limb mode, the -Z-axis of the spacecraft is pointed in a precalculated orientation so that the instruments scan across the limb. The slit and scan mirror of MIRS, and CCD imagery of the TENGOO may be positioned parallel to the limb. In any cases of the limb observations, the FOV of OROCHI is so wide that OROCHI can
observe most parts of the Mars disk even if the other two instruments are pointing at the limb.

Another target for campaign observations is atmospheric phenomena that are already known to occur in a particular region. For example, ice clouds are frequently observed around the high mountains (Wang and Ingersoll 2002), and numerical simulations show that they are formed by upslope winds (Spiga and Forget 2009). The spatial scale of these ice clouds is on the order of 10 to 100 km, and their formation should be closely linked to diurnal phenomena (Wilson et al. 2007). Dust haze inside the Valles Marineris has been observed by MEX (Inada et al. 2008). The Valles Marineris is also the site of “puffy” dust storms defined by Kulowski et al. (2017). These dust events are mesoscale phenomena and so their development should be controlled to some extent by the diurnal variation. Ogohara and Satomura (2011) listed several other areas (the Acidalia Planitia, the Arabia Terra, the east of the Elysium Mons, and the Sirenum-Aonia region) where dust haze tends to spread in addition to the mountainous areas and the Valles Mariners suggested. The formation, transport and dissipation of clouds and dust events can be observed in detail with high temporal resolution if MIRS and TENGOO are pointed at these regions. However, whether we can really

point the spacecraft freely to those areas depends largely on the thermal conditions and communication rates of the spacecraft at the time. Frequent observation of high-resolution images means an increase in the amount of data. Therefore, considering such external conditions, the feasibility of campaign observations, including when they are feasible, will be examined. We are currently investigating whether there are any other important observations other than the two campaign observations mentioned above. Compromises and a use case of various observation modes for atmospheric remote sensing will be also investigated.

## Synergy with other missions

The recent years have seen a renewed interest whole throughout the Martian atmosphere, thanks to the aggressive explorations by the MRO, MEX, Curiosity rover, MAVEN and TGO missions, etc.; we now appreciate that it is considerably mutually coupled system of the surface, lower and upper atmospheres, and the surrounding space environment than previous expected (e.g., Nakagawa 2019). However, their spatial coverage and temporal resolution are often strongly limited by the FOV of the instrument and the orbit of the spacecraft. Figure 6 is a schematic view showing the orbits of the

<figure><img src="image_11.png" /><figcaption>**Fig. 6** A schematic view of the orbits of the ongoing and future missions. The orbit of MEX appears in this figure to be similar to that of MMX, but in fact an elliptical polar orbit with an apoapsis in the southern hemisphere is intended</figcaption></figure>
ongoing and future spacecrafts. Orbit is closely linked to the spatial coverage of a single observation and the temporal resolution. MMX's trajectory, which is quite different from other missions, means that it will produce a completely different type of dataset in terms of temporal resolution and observational coverage.

In order to complete our understanding of atmospheric mutual coupling system, the monitoring capability throughout the atmosphere from near-surface to the space is of importance. Figure 7 shows target altitudes of several missions including MMX and atmospheric phenomena at those altitudes. MMX covers the lowest and highest altitudes, while the other polar-orbiting satellites observe the altitudes in between, including the near-surface atmosphere. MAVEN can observe the widest range of observational altitudes from the surface to space. The limited target altitude of MMX is due to the fact that it is designed to monitor atmospheric phenomena in the lower atmosphere, which has small spatial scales and large temporal variations. Therefore, MMX and these missions are highly complementary, both in terms of the time resolution and spatial coverage derived from the orbit, and in terms of observation altitude.

## Overview of each mission

Mars Express represents the first attempt of Europe to visit another planet in the Solar System (Chicarro et al. 2004). Mars Express (MEX) has remained in orbit around

Mars since the end of 2003, delivering a continuous and diverse survey of Mars, monitoring all the components of the Martian system from the subsurface to the exosphere, including the surface, the neutral atmosphere, as well as the magnetosphere. When the MMX mission will be reaching its destination, MEX will have spent more than 20 years in orbit and should still be in good health to join MMX in its observing campaign. MEX has set the path for helping MMX prepare its future exploration, with its recurrent observations of the Martian moons, leading to a better characterization of Phobos properties in particular (Witasse et al. 2014). With the Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA, a hyperspectral imager, Bibring et al. 2004) and the High-Resolution Stereo Camera (HRSC, Neukum et al. 2004), Mars Express will be able to assist and complement MMX MIRS, TENGOO and OROCHI in their imaging quest of Mars, Phobos and Deimos surfaces. All these instruments feature comparable characteristics, delivering images at a variety of wavelengths, from UV (>390 nm) to infrared (<5 µm), where surface and atmospheric components possess distinct imprints. However, the ~1-h temporal sampling of MMX will allow a systematic characterization of the diurnal cycle of the Martian atmosphere at any given place of the planet throughout the MMX mission lifetime, such thing that MEX could only tentatively address after years of observations with the Planetary Fourier Spectrometer (PFS, Giuranna et al.

<figure><img src="image_12.png" /><figcaption>**Fig. 7** Target altitudes of the atmospheric observations by the several missions and typical atmospheric phenomena at those altitudes.</figcaption></figure>
2021) or with the Spectroscopy for Investigation of Char-
acteristics of the Atmosphere of Mars (SPICAM, Mont-
messin et al. 2017). Combining MMX capability with,
e.g., recurrent solar occultations by SPICAM, it should be
possible to establish a better understanding of the parti-
tioning of water vapor between the near-surface accessed
by MMX quasi-ubiquitously and the atmosphere above
where solar occultations provide a high vertical resolu-
tion. While MMX has no capability to directly extract
temperature profiles, PFS and the Mars Radio Science
experiment (MaRS, Hinson et al. 2019) will be able to fill
partially this gap up to > 40 km of altitude, but only for a
small fraction of the maps produced by MMX. Between
MMX/MSA, MEX/MaRS and The Analyser of Space
Plasma and Energetic Atoms (ASPERA), and MAVEN
(Jakosky et al. 2015), three spacecrafts will sample simul-
taneously the Martian magnetosphere at three different
locations for the first time, enhancing the coverage in the
characterization of the ionized atmosphere, providing
unique insights in the escaping mechanisms prevailing
on the planet. In particular, the permanent position of
MMX at a distance of Mars where it will essentially sam-
ple the solar winds will make MMX extremely comple-
mentary to MEX whose elliptical orbit as MEX is capable
to penetrate the Martian atmosphere down to ~ 300 km
far from the surface at periapsis, with an apoapsis located
at ~ 10,000 km.

The ExoMars Trace Gas Orbiter is an European Space
Agency (ESA)/ROSCOSMOS mission dedicated to the
investigation of the Martian atmospheric trace gases and
their sources, and how the water and the geochemical
environment varies, i.e., by characterizing their distribu-
tion in the atmosphere, on and near the surface or as a
function of depth in the shallow subsurface (Vago et al.
2015). TGO was launched in March 2016, and started
its science phase in April 2018. With its near-circular
orbit (eccentricity of 0.0069), varying between 380 and
430 km above the planet's surface, with an inclination
of 74°, the ground track repeats after 30 sols with one
orbital period being approximately 2 h long (12 orbits
in one sol). This orbit provides optimum coverage of the
surface and solar occultation possibilities for the science
instruments, while still allowing the spacecraft to relay
data from the different assets now on the planet, as well
as from future landers and rovers. EMTGO comprises
four instruments: CASSIS, Colour and Stereo Surface
Imaging System (Thomas et al. 2017), FREND, Fine Reso-
lution Epithermal Neutron Detector (Mitrofanov et al.
2018), and two spectrometers' suites, ACS (Atmospheric
Chemistry Suite, Korablev et al. 2018) and NOMAD
(Nadir and Occultation for MArs Discovery, Vandaele
et al. 2018). The two missions will be complimentary in
that MMX will provide the global context to TGO, which

has a smaller field of view but can still observe vertical
distribution of dust, water vapor, and other trace gases
with high accuracy by solar occultation technique. The
high temporal resolution observations by OROCHI and
MIRS can fill in the gaps of observations by TGO. This
will be of particular importance to understand the impact
of dust storms, global or regional, on the transport of
trace gases within the atmosphere. On the other hand,
NOMAD and ACS can also derive the vertical distribu-
tions of the atmospheric temperature, while MIRS will
not be able to measure them accurately. So, TGO can
contribute to understanding the dynamics controlling the
transport of the tracers that will be discovered by MMX,
perhaps through numerical simulations and data assimi-
lation of the temperature distributions. Also direct com-
parison and mutual validation will be possible between
instruments on both missions, as for example between
the NOMAD and MIRS nadir observations, or between
the cameras.

Al Amal ('Hope' in Arabic), also known as the Emirates
Mars Mission (EMM), was successfully launched to Mars
from the Tanegashima Space Center in Japan on 20 July,
2020, the 51st anniversary of the Apollo 11 Moon land-
ing. EMM will make measurements relevant for under-
standing energy transport in the Martian atmosphere,
both within the lower atmosphere (as a function of local
time, geographic location, and season) and between the
lower and upper atmosphere (Sharaf et al. 2020). EMM
carries three science instruments: the Emirates Mars
Infrared Spectrometer (EMIRS, 6–40 microns), a multi-
wavelength 12-megapixel visible and near-UV imager
(Emirates eXploration Imager, EXI), and an ultravio-
let spectrometer (100–170 nm). The orbital inclination
of the spacecraft is low (~25°) and the orbital period is
large (~55 h), so that EMM's measurements will typi-
cally be global (e.g., EXI's images will contain the full
disk of Mars). This orbit will enable EMM to measure all
longitudes on Mars at all times of day every ~ 10 days—
something that has not been possible with previous
Mars spacecraft. The nominal mission for EMM is one
Mars year (spring 2021-spring 2023), with a possibility
for mission extension for an additional Mars year. Thus,
it is unlikely that EMM and MMX will overlap as active
missions at Mars. However, the datasets from the two
missions will be complementary, and therefore the EMM
observations may help to inform the MMX observa-
tions. Both missions will investigate transport processes
for water and dust in the lower atmosphere. The EMIRS
can observe spatial distributions of the major trac-
ers and temperature in the lower atmosphere although
its spatial resolution on Mars is much lower than the
MIRS onboard MMX. MIRS can monitor temporal vari-
ations of the much finer structures of the tracers than
the EMIRS's spatial resolution while it will not be able to measure temperature accurately near the Mars surface. Both missions will also investigate escape of the Martian atmosphere to space. EMM can observe neutral molecules escaping from Mars, while MSA onboard MMX can detect escaping ions.

MRO, which was launched on August 2005, has observed the Martian atmosphere for about 15 years (Zurek and Smrekar 2007). Its orbit is the sun-synchronous polar orbit and therefore it can observe 12–13 longitudes for each latitudinal band for one sol. The local time of observations will correspond to slightly after midnight and noon. This type of orbit is suitable for monitoring diurnal to seasonal variations of weather systems in all latitudes. Observations of the day and nightsides of Mars at several longitudes every sol enable us to derive the meridional distributions of zonal mean of observed variables (e.g., the atmospheric temperature). Mars Climate Sounder (MCS) has quantified the vertical and horizontal variations of water vapor, dust, and the atmospheric temperature (Kleinböhl et al. 2009) on the dayside and nightside of Mars and the database that has been accumulated since the MOI reveals their seasonal and annual changes. Mars Color Imager (MARCI, Bell et al. 2009) is a push-bloom camera with a wide longitudinal FOV and can scan Mars in the latitudinal direction following the satellite's orbital motion. Accordingly, MARCI can cover the whole of Mars surface in one sol. However, if we focus on a particular region, the time resolution of observations of the region is worse than half a sol except the polar regions. MARCI that uses visible wavelengths filters can take only one image of the regions every sol. MCS can observed the nightside of Mars, but the longitudinal resolution of the observations is low due to its narrow FOV and limb-viewing operation. Therefore, the instruments onboard MRO cannot monitor rapid variations of fine structures in the spatial distributions of the tracers with shorter time-scales than one sol and smaller horizontal scales than the synoptic scale. Although MMX cannot observe the nightside of Mars, it fills in the gaps between MRO observations and reveals the continuous variations in the fine distribution of water vapor and dust.

MAVEN is a NASA Mars-orbiting spacecraft mission dedicated to investigating the upper atmosphere and plasma environment around Mars in order to determine the role of the atmospheric escape to space has played in altering the Martian climate over the planet's history (Jakosky et al. 2015). MAVEN was launched in November 2013 and entered into orbit around Mars in September 2014. MAVEN carries 9 science instruments to measure the solar and solar wind drivers of escape, the upper atmospheric reservoirs for escape, and the

escape processes and rates. These measurements have also enabled to determine that the atmospheric escape has played an important role in Martian climate evolution, such that the atmospheric escape removed half a bar or more of CO₂ from the atmosphere over Martian history (Jakosky et al. 2017). The MAVEN instruments consist of both in situ particle and field detectors and a remote sensing package. Having a mission dedicated to a single science goal making coordinated observations has enabled a number of new or unexpected discoveries, including diffuse aurorae over the entire Martian disk (Schneider et al. 2015), the response of the Martian upper atmosphere to both dust storms and solar storms (e.g., Lee et al. 2020, and the complex magnetic configuration near Mars driven by crustal magnetic fields (e.g., Xu et al. 2017, DiBraccio et al. 2017). MAVEN's instruments are currently all working well, and the mission is expected to last until 2030. Therefore, the MMX MSA instrument and MAVEN could potentially make simultaneous observations of the Martian magnetosphere and the solar wind. If the MEX mission is also extended, three multi-point measurements of MEX, MAVEN and MMX will strongly help distinguish between temporal and spatial variabilities of the solar wind-driven magnetospheric and ion escape processes at Mars.

ESCAPADE (ESCAPE and Plasma Acceleration and Dynamics Explorers) is a planned twin-spacecraft mission (in the preliminary design phase under the NASA's SIMPLEX-II program as of this writing) that will measure charged particles and magnetic fields around Mars. Ion and magnetic field data provided by MSA on MMX will be highly complementary to ESCAPADE (and the currently operating MAVEN and MEX missions, if extended) in multiple ways. First, the high mass resolution (M/dM ~ 100) of MSA complements other suprathermal ion instruments generally with lower mass resolutions by providing detailed information on ion composition and even on isotopes. Second, the MMX's nominal quasi-satellite orbit provides an equatorial, nearly circular orbit around Mars, enabling regular in situ sampling of the solar wind and magnetotail plasma every orbit, provided that the MSA's 2π sr field of view is oriented properly. Around the Phobos distance, MMX is expected to be located in the upstream solar wind for roughly half of the orbit around Mars under nominal solar wind conditions (e.g., Trotignon et al. 2006). The regular solar wind coverage is particularly valuable for other spacecraft in highly inclined, elliptical orbits with gradual precession of periapsis because they typically lose the solar wind coverage for a long duration once they are in an orbital configuration unfavorable for solar wind measurements. Finally, the addition of MSA data will augment the multi-spacecraft science originally envisioned by ESCAPADE.
If simultaneous observations by MMX and ESCAPE are realized along with extended operation of MAVEN and MEX, there may possibly be 5 spacecraft with plasma instrumentation orbiting Mars. This will be an unprecedented opportunity for a rich variety of multi-point analyses on the highly dynamic and complex magnetosphere of Mars and planetary ions escaping through it. These analyses include, but are not limited to: (i) distinguishing spatial from temporal variations; (ii) simultaneous observations of drivers and responses, thereby monitoring time evolution of the system during solar transients, and (iii) timing analysis between multiple locations, thereby determining direction and speed of perturbations propagating through the system.

## Synergy for each science theme

The study on the paleo-environment of Mars using the Martian samples that MMX will bring back to Earth is expected to have synergy with MSR first and foremost. The NASA-ESA-led Mars Sample Return (MSR) and MMX missions are both planned for the 2020s. MSR will return samples back to the Earth in 2031 from the Perseverance rover landing site Jezero crater (Beaty et al. 2019), whereas MMX will return the Phobos regolith in 2029 (Kawakatsu et al. 2017; Kawakatsu 2018). MSR will provide a comprehensive dataset regarding the single location with the geologic context. At the same time, MMX will return Martian surface materials ejected from multiple unknown locations by numerous impact processes (Hyodo et al. 2019). Together MSR and MMX are the first-ever missions designed to collect material samples from the Mars system for analysis. Eventually, their complementary nature will address questions on the origin (e.g., source of building blocks of Mars), interior evolution (e.g., crust-mantle differentiation), geologic history (e.g., hydrologic cycles), and the potential biological activity (e.g., nature and extent of habitability and preservation of biosignatures/biomarkers).

In order to understand the drastic climate change on early Mars and the evolutionary history of the total amount of CO₂ and H₂O reservoirs in the Martian surface environment, we need to understand the escape rates of H, O, and C as a function of external drivers, such as solar radiation and solar wind, from the observations of atmospheric processes and near-space environment of present-day Mars. As reviewed in the "Atmospheric escape" section, acceleration mechanisms of cold planetary ions depend both on tailward distance from Mars and solar wind conditions (e.g., Nilsson et al. 2012; Inui et al. 2019). While MSA measurements at a fixed tailward distance will provide data to assess the effects of solar wind conditions, a synergy with other missions with multi-point measurements by MEX/ASPERA,

MAVEN/STATIC, and ESCAPE at different distances from Mars will give an unprecedented opportunity to clarify the acceleration mechanisms and escape channels of cold ions from Mars. Especially, simultaneous multi-point measurements of atmospheric response to an extreme transient event, such as CME and CIR, could provide a deep insight of the global structure of vigorous escape processes in the ancient days. Another synergy with other missions regarding this science theme is simultaneous observations from the ground to space in order to understand a possible connection between the Martian atmosphere and atmospheric escape. Although OROCHI and MIRS onboard MMX provide the detailed global monitoring of water vapor and dust in the lower atmosphere, the vertical evolution of water vapor and dust into the upper atmosphere should be complemented by sensitive occultation observations by MEX, TGO, and MAVEN. Mutual system of the Martian atmosphere and high-speed transport of water from lower to upper atmosphere could be clarified only by such synergy.

One of our objectives is continuous monitoring of rapid transport processes controlled by atmospheric phenomena with fine structures as described in the above sections. Spatial and temporal data coverage of this type of observations is completely different from that of typical polar-orbiting spacecrafts. MMX can monitor the rapid development of dust storms and ice clouds and the deformation of distributions of water vapor with a temporal resolution less than one hour. However, it cannot observe variables included in the basic equations of the atmosphere (e.g., temperature or velocity). Accordingly, the behavior of dust storms and water vapor revealed by MMX cannot be interpreted from MMX observations alone. On the other hand, typical polar-orbiting satellites, such as MRO and TGO, cannot monitor the rapid development of dust storms and other phenomena sequentially, but MCS onboard MRO and the two instruments onboard TGO can observe the synoptic structure of the atmospheric temperature on a daily basis. Especially, MCS can measure the atmospheric temperature even at the nightside of Mars. Zonal mean temperature and anomalies from the zonal mean derived from such polar-orbiting satellites are crucial to understand mechanisms of the behavior of tracers observed by MMX because they enable us to infer distributions of horizontal winds that actually transport the tracers. Another synergy with other missions regarding these science themes is simultaneous observations of dust, ice clouds, and water vapor by spectrometers. MIRS has comparable characteristics with MEX/OMEGA and is a powerful instrument for observation of fine structures of water vapor. Although MIRS will continue to hourly scan several areas of Mars, observation time cannot be always
assigned to Mars (e.g., during the dayside of Phobos). Therefore, coordinated observations between MMX and MEX may be able to fill in the missing observation period of water vapor distribution. In addition, EMIRS onboard HOPE can always obtain the global tracer distribution. Although its spatial resolution is much lower than that of MIRS and OMEGA, it can monitor the global structure of the atmosphere, in which the water vapor distribution obtained by MIRS and OMEGA is embedded. Of course, the complementarity between MMX and MEX in being able to fill in missing observation periods is also the case with other instruments on other spacecraft; using MRO/MARCI and HOPE/EXI allows for more continuous observations than OROCHI alone.

## Summary

The aims of MMX with respect to Mars system sciences are:

* Obtain new information on the history of the Martian surface environment,

* Advance our understanding of material transport processes in the Martian atmosphere affecting the transitions in the Martian climate.

There is a possibility that Martian ejecta are deposited on the surface of Phobos. Moreover, those ejecta do not need to be launched as fast as the Martian meteorites. Therefore, it is possible that they have not been much thermally metamorphosed and may retain information from various eras. It is expected that the Martian ejecta deposited on the Phobos surface can be brought back to Earth for analysis to understand the environment on the Martian surface at various eras.

The Martian surface environmental changes in the past are closely related to changes in the amount of the atmosphere (i.e., the surface pressure). There is a large uncertainty in estimation of the total amount of H₂O and CO₂ that have been lost from the Martian atmosphere to space in the past. Comprehensive measurements of oxygen-, carbon-, hydrogen-bearing ion species with high mass resolution of MSA at the Phobos orbit will provide crucial constraints on H₂O and CO₂ escape rates at present-day Mars and its extrapolation backward in time. MMX will frequently enter the shadows of Mars and Phobos as it will stay in the Phobos orbit. MSA observations at the fixed distance from Mars will provide a unique opportunity to assess the effects of solar wind conditions on the cold ion escape process through the Martian-induced magnetotail. Another strength of the planned atmospheric escape observations is coordination with observations of the lower atmosphere of Mars by MMX as well as synergy with MEX, TGO, EMM, MRO, MAVEN, and

ESCAPADE observations. We can verify whether the ion outflows are correlated with initiations and developments of dust events and ice clouds.

The major difference between MMX observations of the Mars lower atmosphere and previous missions is that MMX continuously observes a wide area from the equatorial orbit with high temporal resolution. This will help to elucidate the fine structures of water vapor near the Martian surface which have been observed recently, the distribution of water vapor associated with dust events, and their temporal variations. The rapid development and dissipation of sub-mesoscale to mesoscale atmospheric phenomena cannot, in principle, be observed by conventional polar-orbiting satellites. However, considering that the fluctuation component with the largest amplitude near the Martian surface is the diurnal variation, weather satellite-like observations such as MMX are essential to understand the mechanism of such small-scale dust events and ice clouds and the efficient vertical transport of water vapor and dust to the upper atmosphere by them, which may have contributed to efficient escape of H₂O. MMX will monitor the fine structure of dust and water vapor in the lower atmosphere with high temporal resolution, and will also observe atmospheric escape. On the other hand, the other spacecrafts are mainly observing the Martian atmosphere between the two altitudes from polar orbits. MMX is highly complementary to them in that it fills a spatio-temporal gap that has not been observed so far.

## Abbreviations

ACS: Atmospheric chemistry suite; ASPERA: The analyser of space plasma and energetic atoms; CASSIS: Colour and stereo surface imaging system; CIA: Collision-induced absorption; CIR: Corotating interaction region; CME: Coronal mass ejection; CRISM: Compact Reconnaissance Imaging Spectrometer for Mars; CTX: Context camera; EMIRS: Emirates Mars Infrared Spectrometer; EMTGO: ExoMars Trace Gas Orbiter; ESCAPADE: ESCape and Plasma Acceleration and Dynamics Explorers; EXI: Emirates eXploration Imager; FWHM: Full width at half-maximum; FOV: Field of view; FREND: Fine resolution epithermal neutron detector; IFOV: Instantaneous field of view; IMA: Ion mass analyser; HGA: High gain antenna; HRSC: High-resolution stereo camera; MARCI: Mars color imager; MaRS: Mars Radio Science experiment; MAVEN: Mars Atmosphere and Volatile Evolution; MCS: Mars climate sounder; MGS: Mars Global Surveyor; MIRS: MMX InfraRed Spectrometer; MMX: Martian Moons eXploration; MO: Mission objective; MOI: Mars orbit insertion; NOMAD: Nadir and Occultation for MArS Discovery; MRO: Mars Reconnaissance Orbiter; MSA: Mass spectrum analyzer; MSR: Mars sample return; OMEGA: Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité; OROCHI: Optical Radiometer cComposed of CHromatic Imagers; PFS: Planetary Fourier spectrometer; QSO: Quasi-satellite orbit; SEVIRI: Spinning enhanced visible and infrared imager; SPICAM: Spectroscopy for investigation of characteristics of the atmosphere of Mars; STATIC: Suprathermal and thermal ion composition; TGO: Trace gas orbiter; VMC: Visual monitoring camera.

## Acknowledgements

The SPICE toolkit released from the Navigation and Ancillary Information Facility was used for simulations of the expected Mars views and the spatial and temporal distributions of the sub-spacecraft points on Mars. We thank to the MMX engineering team for creating some SPICE kernels. Also, we would like to thank the other members of the Mars System sub-science team, especially
O. Korablev and H. Kurokawa, for looking over this manuscript and for their many helpful comments. We also would like to thank K. Masunaga for his great contribution in replying to the reviewers' comments. RMR acknowledges support by the Earth-Life Science Institute (ELSI) and the National Institutes of Natural Sciences: Astrobiology Center (Grant Number JY310064). This work was supported by ISAS/JAXA as a part of Phase-A/B activities of MMX and by JSPS KAKENHI to TU (JP 17H06459), TK (JP20H01958, JP19K14789), HN (JP20H04605, JP19K03943), SY (JP20K04039), and NT (JP18KK0093, JP19H00707, JP20H00192).

**Authors' contributions**

KO, HN, SA, TK, TU, NT, TI, FM, DB, AD, TG, TH, YH, MK, FL, RR, ES, KS, AS, ACV, and SY prepared the initial manuscript. KO, HN, SA, TK, TU, NT, TI, and FM contributed to the development of mission objectives, consideration of integrated operation plans, and analysis of temporal variations in instrument field of view and footprint. HI and ES brought important technical information on the spacecraft and instruments and helped plan the baseline observations. SY, AB, SK, TK, HN, TG, AD and ES contributed to the design and development of the instruments. All authors provided us with feedback. All authors read and approved the final manuscript.

**Funding**

RMR receives funding from the Earth-Life Science Institute (ELSI) and the National Institutes of Natural Sciences: Astrobiology Center (grant number JY310064). Our work was supported by ISAS/JAXA as a part of Phase-A/B activities of MMX and by JSPS KAKENHI to TU (JP 17H06459), TK (JP20H01958, JP19K14789), HN (JP20H04605, JP19K03943), SY (JP20K04039), and NT (JP18KK0093, JP19H00707, JP20H00192).

**Availability of data and materials**

The actual SPICE kernel for the probe will be released when the spacecraft is launched and the mission is executed.

**Declarations**

**Ethics approval and consent to participate**

Not applicable.

**Consent for publication**

Not applicable.

**Competing interests**

The authors declare that they have no competing interests.

**Author details**

¹Faculty of Science, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan. ²Graduate School of Science, Tohoku University, 6-3, Aram-aki-Aza-Aoba, Aoba-ku, Sendai, Miyagi, Japan. ³LPAP, STAR Institute, Université de Liège, Allée du 6 août 19C, 4000 Liège, Belgium. ⁴Royal Belgian Institute for Space Aeronomy, 3 Avenue Circulaire, 1180 Brussels, Belgium. ⁵Artificial Intelligence Research Center, National Institute of Advanced Industrial Science and Technology, 2-3-6, Aomi, Koto-ku, Tokyo, Japan. ⁶Department of Solar Sys-tem Sciences, Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshi-nodai, Sagamihara, Kanagawa 252-5210, Japan. ⁷Graduate School of Frontier Sciences, The University of Tokyo, 5-1-5, Kashiwanohai, Kashiwa, Chiba 277-8561, Japan. ⁸LATMOS/IPSL, CNRS, Sorbonne Université, UVSQ-UPSaclay, Guyancourt, France. ⁹LASP/University of Colorado, Boulder, CO, USA. ¹⁰LESA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France. ¹¹Space Sciences Labora-tory, University of California, Berkeley, 7 Gauss Way, Berkeley, CA 94720, USA. ¹²Graduate School of Science, Kyoto University, Kitashirakawaiowake-cho, Sakyo-ku, Kyoto 606-8502, Japan. ¹³Research and Development Directo-rate, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 252-5210, Japan. ¹⁴Graduate School of Advanced Science and Engi-neering, Hiroshima University, 1-3-1 Kagamiyama, Higashihiroshima, Hiro-shima 739-8526, Japan. ¹⁵LATMOS/CNRS, Sorbonne Université, UVSQ, Paris, France. ¹⁶Earth-Life Science Institute, Tokyo Institute of Technology, 2-12-1, Tokyo 152-8550, Japan. ¹⁷Space Science Institute, Boulder, CO, USA. ¹⁸CNES, 18 avenue Edouard Belin, 31400 Toulouse, France. ¹⁹Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, Hongo

7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan. ²⁰Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Campus Pierre et Marie Curie BC99, 4 place Jussieu, 75005 Paris, France. ²¹Institut Universitaire de France, 1 rue Descartes, 75005 Paris, France. ²²Royal Belgian Institute for Space Aeronomy, avenue Circulaire 3, 1180 Brussels, Belgium. ²³Graduate School of Science, Osaka University, Machikaneyama-cho, Toyonaka, Japan. ²⁴Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo 171-8501, Japan. ²⁵Department of Physics, College of Sciences, University of Central Florida, 4111 Libra Drive, Physical Sciences Bldg. 430, Orlando, FL, USA.

Received: 27 November 2020 Accepted: 9 April 2021

Published online: 03 January 2022

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