Unveiling the Dynamics of Interaction Between Mars' Magnetic Field and the Solar Wind

The interplay between solar winds and planetary magnetic fields is pivotal for the evolution of planetary atmospheres and their habitability. Here we focus on how solar wind interacts with Mars.
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It's widely understood that the interplay between stellar winds and planetary magnetic fields is pivotal for the evolution of planetary atmospheres and their habitability. Within our solar system, Mars stands out: it lacks a global magnetic field but possesses small-scale crustal magnetic fields, which provide a unique natural laboratory for studying the impacts of small-scale crustal fields on atmospheric escape. Small-scale crustal fields are often referred to as “mini-magnetospheres” because they bear a resemblance in morphology to Earth's intrinsic magnetosphere, albeit on a reduced scale. Yet, the dynamics of charged particles, both ions and electrons, might differ between these crustal fields and the intrinsic magnetospheres. Earth's intrinsic magnetosphere traps these charged particles, which then accumulate around the planet, forming a dense ring current and radiation belt (see Figure 1). These phenomena pose risks by potentially damaging spacecraft electronics and presenting health hazards to astronauts. Three pertinent questions emerge:

  1. How do the crustal fields influence particle dynamics?
  2. Can these small-scale crustal fields also trap particles in a manner akin to the intrinsic magnetospheres?
  3. In what ways do the crustal fields impact the interaction between solar wind and a planet, and how might they influence atmospheric evolution?

Driven by these inquiries - and, to be honest, mainly due to curiosity, I set out to explore the ions behaviors within the small-scale Martian crustal fields based on the high-resolution measurements provided by the NASA’s Mars Atmosphere and Volatile EvolutioN (MAVEN) mission.

Figure 1. Comparison between the Martian small-scale crustal fields (a) and the Earth’s intrinsic magnetosphere (b), adapted from https://svs.gsfc.nasa.gov/. The yellow, blue spiral curves are the particle’s trajectory. These particles are trapped by the magnetic fields, forming ring current and radiation belt around the planet.

For decades, there has been no observational evidence of trapped ions at Mars. This absence has fostered the notion that, owing to Mars's weak magnetic field environment, ions are predominantly unmagnetized and will escape to space. However, in October, 2022, we found a distinctive and unique case where ions appeared to be magnetized and trapped by the crustal fields, a phenomenon highlighted by the spatial dispersion structures of the ions (refer to Figure 2). Intriguingly, this kind of signature has, until now, only been detected within intrinsic magnetospheres.

 

Initially, I was both surprised and elated, recognizing that this unique event could deepen our insight into Martian crustal fields. My supervisor and colleagues suggested that this finding is novel and could be published in a high-quality journal. However, to be honest, I was uncertain about how to delve deeper into the analysis and truly grasp its significance. In reality, I have shared and discussed this event with numerous researchers, spanning not just the Mars research domain but also those specializing in Earth’s magnetosphere. Our primary challenge was discerning how these signatures emerged from drift motion. Given the intricate nature of the crustal fields and our lack of data on electric fields, this was no simple task. As a workaround, we embarked on test particle simulations based solely on crustal field models, aiming to reveal the formation mechanism of these dispersion structures.

Figure 2. The magnetospheric ion drift patterns and the relative path of MAVEN on the magnetic equator plane of crustal fields. (a) The spatial distribution of the magnetic strength in the magnetic equator plane of crustal fields. The white arrows are the magnetic drift velocity of 100 eV protons. The blue curve with arrow represents the MAVEN path relative to the crustal fields. The azimuthal and radial distance are the relative distance between each point to the origin point (marked by the white star in the top left corner). (b) Time series of the magnetic field strength of magnetic equator points of the traced magnetic field lines crossed by MAVEN. (c) The ion energy-versus-time spectrum.

Nonetheless, with the guidance of several researchers well-versed in studying ion motions within intrinsic magnetospheres, we realized we couldn’t accurately reproduce the structures based on the model without accounting for electric fields. This left me somewhat disheartened, and I voiced concerns to my colleagues about the lack of a solid explanation. My colleagues were supportive and believed that our findings were valuable. We note that this unsuccessful experiment emphasizes the existence of electric fields within the crustal fields, an aspect that had been previously neglected. The infrequent appearance of this signature further suggests its formation is intrinsically tied to specific configurations of electric fields. This has greatly improved our understanding of Martian crustal fields.

Figure 3. Sketch of the drift dispersion of ions within the Martian crustal fields. The ions (white dots) with different energies are spatially separated due to their energy-dependent drift velocity (blue arrows). The shades of color represent the ion’s energy. The dark (light) color represents the ion’s energy is high (low). The red crescent-shaped area denotes the possible injection location. The blue dashed line with arrow shows the MAVEN’s path. The low-energy (high-energy) ions were located in the outer (inner) region of the crustal fields, leading to MAVEN recorded the increase (decrease) in ion’s energy when moving towards the inner (outer) part of the crustal fields.

We then set out to examine the spatial distribution of ions with varying energies, comparing it to patterns observed in Earth’s magnetosphere. We observed that as MAVEN approached the inner sections of the crustal fields, ion energy increased, while it decreased as the spacecraft moved towards the outer regions. This suggests that ions with higher energies are found in the inner parts, while those with lower energies are in the outer regions (refer to Figures 2 and 3). This spatial ion distribution mirrors patterns seen on Earth, implying the underlying mechanisms are likely the same.

The significance of this discovery is multi-fold. Firstly, it offers profound insights into the operation of Martian crustal fields. While we have had a more complete understanding of how the global intrinsic magnetospheres affect the solar wind interaction with planet, Mars’s case provides insights into a scenario where small-scale crustal magnetic fields play a dominant role. Second, going forward, by understanding the of Martian magnetic fields, we edge closer to unraveling the geologic history and atmospheric evolution of the red planet.

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Planetary Science
Physical Sciences > Physics and Astronomy > Astronomy, Cosmology and Space Sciences > Planetary Science
Space Physics
Physical Sciences > Physics and Astronomy > Astronomy, Cosmology and Space Sciences > Space Physics

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