# Sentence-Level Insights from the Martian Literature: A Natural Language Processing Approach
## 3 Results
### Unsupervised Clustering
\begin{table}
\begin{tabular}{c c c c} \hline
**No.** & **Sample Size** & **Topic** & **Summary** \\ \hline
11 & 643 & \
\begin{tabular}{c} Martian Meteorites as Proxies for \\ Mars’ Geochemistry \\ \end{tabular} &
\begin{tabular}{c} Martian meteorites reveal Mars’ mantle composition, volatile \\ content, and past aqueous processes, providing insights into its \\ magmatic evolution. \\ \end{tabular} \\ \hline
12 & 638 & \
\begin{tabular}{c} Geochemical Diversity \\ in Shergottites \\ \end{tabular} &
\begin{tabular}{c} Shergottites display geochemical diversity, indicating Mars’ \\ mantle heterogeneity and complex magmatic history. \\ \end{tabular} \\ \hline
13 & 612 & \
\begin{tabular}{c} Martian Crustal Magnetic Fields \\ and Solar \\ Wind Interaction \\ \end{tabular} &
\begin{tabular}{c} Mars’ crustal magnetic fields affect solar wind interaction, \\ influencing ion escape, atmospheric erosion, and \\ ionospheric structure. \\ \end{tabular} \\ \hline
14 & 587 & Stability of Liquid Water on Mars &
\begin{tabular}{c} Mars’ low pressure limits liquid water, but brines and transient \\ water exist, affecting its habitability and climate evolution. \\ \end{tabular} \\ \hline
15 & 548 & \
\begin{tabular}{c} Martian \\ Crust Composition \\ \end{tabular} &
\begin{tabular}{c} Mars’ crust is primarily basaltic with diverse igneous \\ compositions, shaped by magmatic and sedimentary processes. \\ \end{tabular} \\ \hline
16 & 511 & \
\begin{tabular}{c} Mapping Mars’ Topography with \\ Mars Orbiter Laser \\ Altimeter (MOLA) \\ \end{tabular} &
\begin{tabular}{c} MOLA provides precise topographic data, improving \\ understanding of Mars’ surface features, sedimentary \\ structures, and crater formations. \\ \end{tabular} \\ \hline
17 & 505 & \
\begin{tabular}{c} Sulfate minerals and Martian \\ Water History \\ \end{tabular} &
\begin{tabular}{c} Sulfates on Mars suggest past water activity, formed by \\ volcanic, acidic, or groundwater processes, \\ influencing habitability. \\ \end{tabular} \\ \hline
18 & 466 & \
\begin{tabular}{c} Martian Dust and \\ Climate Evolution \\ \end{tabular} &
\begin{tabular}{c} Dust controls Mars’ climate, affecting temperature, circulation, \\ and solar radiation interactions, influencing global weather. \\ \end{tabular} \\ \hline
19 & 463 & \
\begin{tabular}{c} Solar Wind and \\ Martian Atmosphere \\ \end{tabular} &
\begin{tabular}{c} Without a global magnetic field, Mars’ atmosphere interacts \\ directly with solar wind, affecting ion loss and \\ atmospheric evolution. \\ \end{tabular} \\ \hline
20 & 453 & \
\begin{tabular}{c} Impact Craters as Martian \\ Sediment Traps \\ \end{tabular} &
\begin{tabular}{c} Impact craters preserve Mars’ environmental history, trapping \\ sediments that reveal past climate and hydrological activity. \\ \end{tabular} \\ \hline
21 & 440 & \
\begin{tabular}{c} Water Ice Distribution \\ on Mars \\ \end{tabular} &
\begin{tabular}{c} Mars hosts widespread water ice, influenced by climate, \\ obliquity shifts, and atmospheric processes, key for \\ future exploration. \\ \end{tabular} \\ \hline
22 & 367 & \
\begin{tabular}{c} Fluvial Landforms and \\ Hydrological History of Mars \\ \end{tabular} &
\begin{tabular}{c} Mars’ valley networks and fluvial ridges indicate past surface \\ water, suggesting episodic precipitation and runoff. \\ Hydrological models support intermittent water flow. \\ \end{tabular} \\ \hline
23 & 362 & \
\begin{tabular}{c} Martian Crustal Structure and \\ Subsurface Properties \\ \end{tabular} &
\begin{tabular}{c} Mars’ crust varies in thickness and composition. Gravity and \\ seismic data show heterogeneous layering, affecting heat flow \\ and evolution. \\ \end{tabular} \\ \hline
24 & 361 & Climate History of Early Mars &
\begin{tabular}{c} Early Mars may have been warm and wet or cold and icy. \\ Geological evidence suggests episodic warming from \\ volcanism or impacts. \\ \end{tabular} \\ \hline
25 & 360 & \
\begin{tabular}{c} The Martian Water Cycle and \\ Atmospheric Loss \\ \end{tabular} &
\begin{tabular}{c} Mars’ water cycle involves surface-atmosphere exchanges. \\ Hydrogen and oxygen escape contribute to long-term \\ water loss. \\ \end{tabular} \\ \hline \end{tabular}
\end{table}