Zobrazeno 1 - 10
of 124
pro vyhledávání: '"Wakita, Shigeru"'
Autor:
Taki, Tetsuo, Wakita, Shigeru
The lifetime of mm size dust grains, such as chondrules, in the nominal solar nebula model is limited to $\sim 10^{5}$ yr due to an inward drift driven by gas drag. However, isotopic and petrological studies on primitive meteorites indicate a discrep
Externí odkaz:
http://arxiv.org/abs/2401.02574
Autor:
Arakawa, Sota, Wakita, Shigeru
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 whether the cryst
Externí odkaz:
http://arxiv.org/abs/2401.00231
Autor:
Wakita, Shigeru, Johnson, Brandon C., Soderblom, Jason M., Shah, Jahnavi, Neish, Catherine D., Steckloff, Jordan K.
Selk crater is an $\sim$ 80 km diameter impact crater on the Saturnian icy satellite, Titan. Melt pools associated with impact craters like Selk provide environments where liquid water and organics can mix and produce biomolecules like amino acids. I
Externí odkaz:
http://arxiv.org/abs/2302.11330
The record of impact induced shock-heating in meteorites is an important key for understanding the collisional history of the solar system. Material strength is important for impact heating, but the effect of impact angle and impact velocity on shear
Externí odkaz:
http://arxiv.org/abs/2208.07630
Autor:
Wakita, Shigeru, Johnson, Brandon C., Soderblom, Jason M., Shah, Jahnavi, Neish, Catherine D.
As the only icy satellite with a thick atmosphere and liquids on its surface, Titan represents a unique end-member to study the impact cratering process. Unlike craters on other Saturnian satellites, Titan's craters are preferentially located in high
Externí odkaz:
http://arxiv.org/abs/2201.09587
During the early stages of an impact a small amount material may be jetted and ejected at speeds exceeding the impact velocity. Jetting is an important process for producing melt during relatively low velocity impacts. How impact angle affects the je
Externí odkaz:
http://arxiv.org/abs/2102.02303
Shock-induced metamorphism in meteorites informs us about the collisional environment and history of our solar system. Recently the importance of material strength in impact heating was reported from head-on impact simulations. Here, we perform three
Externí odkaz:
http://arxiv.org/abs/1912.00371
Major components of chondrites are chondrules and matrix. Measurements of the volatile abundance in Semarkona chondrules suggest that chondrules formed in a dense clump that had a higher solid density than the gas density in the solar nebula. We inve
Externí odkaz:
http://arxiv.org/abs/1911.10467
Understanding chondrule formation provides invaluable clues about the origin of the solar system. Recent studies suggest that planetesimal collisions and the resulting impact melts are promising for forming chondrules. Given that the dynamics of plan
Externí odkaz:
http://arxiv.org/abs/1909.03655
Autor:
Wakita, Shigeru, Genda, Hidenori
Hydrous minerals are found on the surfaces of asteroids, but their origin is not clear. If their origin is endogenic, the hydrous minerals that were formed in the inner part of a planetesimal (or parent body) should come out on to the surface without
Externí odkaz:
http://arxiv.org/abs/1903.04675