Sota Arakawa
YOU?
Author Swipe
View article: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories Open
Mechanical properties of small bodies such as dust, pebbles, and planetesimals are key to better understanding the formation of planetary systems against their collisional destruction. We present a simple mathematical formulation to determ…
View article: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks Open
The tensile strength of solid particles is the key parameter that controls not only the formation of planetesimals in protoplanetary disks but also outburst and splitting of comets and rotational bursting of asteroids in planetary systems.…
View article: Thermal Diffusivity, Thermal Conductivity and Thermal Inertia of Individual Lunar Regolith Grains: Case Study of Sample 70161 from Apollo 17
Thermal Diffusivity, Thermal Conductivity and Thermal Inertia of Individual Lunar Regolith Grains: Case Study of Sample 70161 from Apollo 17 Open
The regolith on the shallow lunar surface was formed through micrometeorite impacts over time. Investigating the thermophysical properties of the regolith provides valuable insights into the thermal history of the Moon as recorded by these…
View article: Solar System’s earliest solids as tracers of the accretion region of Ryugu and Ivuna-type carbonaceous chondrites
Solar System’s earliest solids as tracers of the accretion region of Ryugu and Ivuna-type carbonaceous chondrites Open
Samples from the carbonaceous asteroid Ryugu and CI (Ivuna-type) chondrites are dominated by low-temperature, aqueously formed secondary minerals, with rare occurrences of anhydrous primary minerals that formed in the high-temperature regi…
View article: Numerical investigation on the compressive behavior of hierarchical granular piles
Numerical investigation on the compressive behavior of hierarchical granular piles Open
Hierarchical granular piles composed of aggregates are key structural features in both geoscience and planetary science, from fault gouge in seismic zones to the internal structures of comets. Although experimental studies have suggested a…
View article: Energy budget analysis of fault motion in a granular rock box simulation
Energy budget analysis of fault motion in a granular rock box simulation Open
View article: Low Rock Mass Fraction Within Trans‐Neptunian Objects Inferred From the Spin–Orbit Evolution of Orcus–Vanth and Salacia–Actaea
Low Rock Mass Fraction Within Trans‐Neptunian Objects Inferred From the Spin–Orbit Evolution of Orcus–Vanth and Salacia–Actaea Open
Satellites play a crucial role in understanding the formation and evolution of trans‐Neptunian objects (TNOs). The spin–orbit evolution of satellite systems depends on their thermal histories, allowing us to constrain the rock mass fractio…
View article: Oxygen Isotope Exchange between Dust Aggregates and Ambient Nebular Gas
Oxygen Isotope Exchange between Dust Aggregates and Ambient Nebular Gas Open
Meteorites and their components exhibit a diverse range of oxygen isotope compositions, and the isotopic exchange timescale between dust grains and ambient gas is a key parameter for understanding the spatiotemporal evolution of the solar …
View article: A closer look at individual collisions of dust aggregates: material mixing and exchange on microscopic scales
A closer look at individual collisions of dust aggregates: material mixing and exchange on microscopic scales Open
Collisions between aggregates with different histories and compositions are expected to be commonplace in dynamically active protoplanetary discs. None the less, relatively little is known about how collisions themselves may contribute to …
View article: A closer look at individual collisions of dust aggregates: Material mixing and exchange on microscopic scales
A closer look at individual collisions of dust aggregates: Material mixing and exchange on microscopic scales Open
Collisions between aggregates with different histories and compositions are expected to be commonplace in dynamically active protoplanetary discs. Nonetheless, relatively little is known about how collisions themselves may contribute to th…
View article: On the elastoplastic behavior in collisional compression of spherical dust aggregates
On the elastoplastic behavior in collisional compression of spherical dust aggregates Open
View article: Oxygen Isotope Exchange Between Dust Aggregates and Ambient Nebular Gas
Oxygen Isotope Exchange Between Dust Aggregates and Ambient Nebular Gas Open
Meteorites and their components exhibit a diverse range of oxygen isotope compositions, and the isotopic exchange timescale between dust grains and ambient gas is a key parameter for understanding the spatiotemporal evolution of the solar …
View article: On the elastoplastic behavior in collisional compression of spherical dust aggregates
On the elastoplastic behavior in collisional compression of spherical dust aggregates Open
Aggregates consisting of submicron-sized cohesive dust grains are ubiquitous, and understanding the collisional behavior of dust aggregates is essential. It is known that low-speed collisions of dust aggregates result in either sticking or…
View article: Isotopic variation of non-carbonaceous meteorites caused by dust leakage across the Jovian gap in the solar nebula
Isotopic variation of non-carbonaceous meteorites caused by dust leakage across the Jovian gap in the solar nebula Open
High-precision isotopic measurements of meteorites revealed that they are classified into non-carbonaceous (NC) and carbonaceous (CC) meteorites. One plausible scenario for achieving this grouping is the early formation of Jupiter because …
View article: Chondrule Destruction via Dust Collisions in Shock Waves
Chondrule Destruction via Dust Collisions in Shock Waves Open
A leading candidate for the heating source of chondrules and igneous rims is shock waves. This mechanism generates high relative velocities between chondrules and dust particles. We have investigated the possibility of the chondrule destru…
View article: Chondrule Destruction via Dust Collisions in Shock Waves
Chondrule Destruction via Dust Collisions in Shock Waves Open
A leading candidate for the heating source of chondrules and igneous rims is shock waves. This mechanism generates high relative velocities between chondrules and dust particles. We have investigated the possibility of the chondrule destru…
View article: Interparticle normal force in highly porous granular matter during compression
Interparticle normal force in highly porous granular matter during compression Open
We perform a numerical simulation of compression of a highly porous dust aggregate of monodisperse spheres. We find that the average interparticle normal force within the aggregate is inversely proportional to both the filling factor and t…
View article: Energy Balance Analysis of Fault Motion in a Granular Rock Box Simulation
Energy Balance Analysis of Fault Motion in a Granular Rock Box Simulation Open
View article: Survivability of Amorphous Ice in Comets Depends on the Latent Heat of Crystallization of Impure Water Ice
Survivability of Amorphous Ice in Comets Depends on the Latent Heat of Crystallization of Impure Water Ice Open
Comets would have amorphous ice rather than crystalline one at the epoch of their accretion. Cometary ice contains some impurities that govern the latent heat of ice crystallization, $L_{\rm cry}$. However, it is still controversial whethe…
View article: Root mean squares of distance and geodesic between two constituent particles within fractal aggregates prepared by BCCA, DLA, and GSAW procedures
Root mean squares of distance and geodesic between two constituent particles within fractal aggregates prepared by BCCA, DLA, and GSAW procedures Open
Understanding the geodesic properties of fractal aggregates is essential, as their thermal and mechanical properties are characterized by their geodesics. In this study, we investigate the root mean square (RMS) of the geodesic between two…
View article: Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth
Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth Open
Understanding the collisional behavior of dust aggregates is essential in the context of planet formation. It is known that low-velocity collisions of dust aggregates result in bouncing rather than sticking when the filling factor of colli…
View article: Oxygen Isotope Exchange Between Molten Silicate Spherules and Ambient Water Vapor with Nonzero Relative Velocity: Implication for Chondrule Formation Environment
Oxygen Isotope Exchange Between Molten Silicate Spherules and Ambient Water Vapor with Nonzero Relative Velocity: Implication for Chondrule Formation Environment Open
Oxygen isotope compositions of chondrules reflect the environment of chondrule formation and its spatial and temporal variations. Here, we present a theoretical model of oxygen isotope exchange reaction between molten silicate spherules an…
View article: Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth
Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth Open
Understanding the collisional behavior of dust aggregates is essential in the context of planet formation. It is known that low-velocity collisions of dust aggregates result in bouncing rather than sticking when the filling factor of colli…
View article: Igneous Rim Accretion on Chondrules in Low-velocity Shock Waves
Igneous Rim Accretion on Chondrules in Low-velocity Shock Waves Open
Shock-wave heating is a leading candidate for the mechanisms of chondrule formation. This mechanism forms chondrules when the shock velocity is in a certain range. If the shock velocity is lower than this range, dust particles smaller than…
View article: Insights on the Sun Birth Environment in the Context of Star Cluster Formation in Hub–Filament Systems
Insights on the Sun Birth Environment in the Context of Star Cluster Formation in Hub–Filament Systems Open
Cylindrical molecular filaments are observed to be the main sites of Sunlike star formation, while massive stars form in dense hubs at the junction of multiple filaments. The role of hub–filament configurations has not been discussed yet i…
View article: Insights on the Sun birth environment in the context of star-cluster formation in hub-filament systems
Insights on the Sun birth environment in the context of star-cluster formation in hub-filament systems Open
Cylindrical molecular filaments are observed to be the main sites of Sun-like star formation, while massive stars form in dense hubs, at the junction of multiple filaments. The role of hub-filament configurations has not been discussed yet…
View article: Interpebble contact radius in a comet nucleus
Interpebble contact radius in a comet nucleus Open
In recent years, the gravitational collapse of pebble clumps in the early Solar system has been regarded as a plausible scenario for the origin of comets. In this context, ‘pebbles’ represent mm- to cm-sized dust aggregates composed of (su…
View article: Interpebble contact radius in a comet nucleus
Interpebble contact radius in a comet nucleus Open
In recent years, the gravitational collapse of pebble clumps in the early Solar System has been regarded as a plausible scenario for the origin of comets. In this context, ``pebbles'' represent mm- to cm-sized dust aggregates composed of (…
View article: Igneous Rim Accretion on Chondrules in Low-Velocity Shock Waves
Igneous Rim Accretion on Chondrules in Low-Velocity Shock Waves Open
Shock wave heating is a leading candidate for the mechanisms of chondrule formation. This mechanism forms chondrules when the shock velocity is in a certain range. If the shock velocity is lower than this range, dust particles smaller than…
View article: Threshold velocity for the collisional growth of porous dust aggregates consisting of cohesive frictionless spheres
Threshold velocity for the collisional growth of porous dust aggregates consisting of cohesive frictionless spheres Open
Understanding the collisional outcomes of dust aggregates and their dependence on the material properties of the constituting particles is of great importance for understanding planet formation. Recent numerical simulations have revealed t…