Rotational effect as the possible cause of the east-west asymmetric crater rims on Ryugu observed by LIDAR data

@article{Hirata2021RotationalEA,
  title={Rotational effect as the possible cause of the east-west asymmetric crater rims on Ryugu observed by LIDAR data},
  author={Naoyuki Hirata and Noriyuki Namiki and Fumi Yoshida and Koji Matsumoto and Hirotomo Noda and Hiroki Senshu and Takahide Mizuno and Fuyuto Terui and Yoshiaki Ishihara and Ryuhei Yamada and Keiko Yamamoto and Shinsuke Abe and Rina Noguchi and Naru Hirata and Yuichi Tsuda and Sei‐ichiro Watanabe},
  journal={Icarus},
  year={2021}
}

YORP Effect on Asteroid 162173 Ryugu: Implications for the Dynamical History

Asteroid 162173 Ryugu is a carbonaceous asteroid that was visited by Japan's Hayabusa2 spacecraft in 2018. The formation mechanism of the “spinning‐top” shape of Ryugu is a vital clue to the

Science operation plan of Phobos and Deimos from the MMX spacecraft

The Phobos observations during the first 1.5 years of the 76 spacecraft's stay around Mars, and the Deimos observations before leaving the Martian 77 system are described.

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The spatial distribution of impact craters on Ryugu

The Western Bulge of 162173 Ryugu Formed as a Result of a Rotationally Driven Deformation Process

162173 Ryugu, the target of Hayabusa2, has a round shape with an equatorial ridge, which is known as a spinning top shape. A strong centrifugal force is a likely contributor to Ryugu’s top-shaped

EROSION AND EJECTA REACCRETION ON 243 IDA AND ITS MOON

Abstract Galileo images of Asteroid 243 Ida and its satellite Dactyl show surfaces which are dominantly shaped by impact cratering. A number of observations suggest that ejecta from hypervelocity

Ejecta Emplacement on the Martian Satellites

Abstract Ejecta features on the martian satellites are compared to models of ballistic emplacement and downslope motion. The asymmetric distribution of ejecta around the large crater Stickney on

Shoemaker crater as the source of most ejecta blocks on the asteroid 433 Eros

It is suggested that most large ejecta blocks on Eros originate from a relatively young 7.6-km-diameter crater, and a large fraction of the ejecta from impacts pre-dating that crater has apparently been buried or eroded.

Geology of 243 Ida

Abstract The surface of 243 Ida is dominated by the effects of impacts. No complex crater morphologies are observed. A complete range of crater degradation states is present, which also reveals

The dynamical evolution and origin of the Martian moons

Rotational breakup as the origin of small binary asteroids

It is found that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation.