arXiv subjects

Kei Kurita

Publications and source records attributed to Kei Kurita.

3 recordsLinked to original sources

arXiv2017

New classification method of volcanic ash samples using statistically determined grain types

We developed a method to classify volcanic ash samples by introducing statistically determined grain types. Using more than 10,000 numbers of automatically measured grain data (parameters of grain shape and transparency) and the cluster analysis, we made grain types without human eyes. By components of the grain type in each samples, we classified samples from types of basaltic monogenetic volcanoes: 1) Funabara scoria cone, Izu Peninsula, Japan (magmatic eruption origin); 2) Nippana tuff ring, Miyakejima, Japan (phreatomagmatic eruption origin); and 3) rootless cones in Myvatn, Iceland (rootless eruption origin). We tested two cases; using grain shape parameters only, and both of grain shape parameters and transparency values. It is found that the sample classification is more consistent with their eruption style in the case of using both parameters of grain shape and transparency. By sampling several layers of an outcrop, this procedure can be used to interpret changes in eruption/fragmentation style during a volcanic event. Furthermore, this procedure might be applicable to other aims such as sedimentology and planetary science.

physics.geo-ph↗

arXiv2015

Avalanche-like fluidization of a non-Brownian particle gel

We report on the fluidization dynamics of an attractive gel composed of non-Brownian particles made of fused silica colloids. Extensive rheology coupled to ultrasonic velocimetry allows us to characterize the global stress response together with the local dynamics of the gel during shear startup experiments. In practice, after being rejuvenated by a preshear, the gel is left to age during a time $t_w$ before being submitted to a constant shear rate $\dot γ$. We investigate in detail the effects of both $t_w$ and $\dot γ$ on the fluidization dynamics and build a detailed state diagram of the gel response to shear startup flows. The gel may either display transient shear banding towards complete fluidization, or steady-state shear banding. In the former case, we unravel that the progressive fluidization occurs by successive steps that appear as peaks on the global stress relaxation signal. Flow imaging reveals that the shear band grows up to complete fluidization of the material by sudden avalanche-like events which are distributed heterogeneously along the vorticity direction and correlated to large peaks in the slip velocity at the moving wall. These features are robust over a wide range of values of $t_w$ and $\dot γ$, although the very details of the fluidization scenario vary with $\dot γ$. Finally, the critical shear rate $\dot γ^*$ that separates steady-state shear-banding from steady-state homogeneous flow depends on the width on the shear cell and exhibits a nonlinear dependence with $t_w$. Our work brings about valuable experimental data on transient flows of attractive dispersions, highlighting the subtle interplay between shear, wall slip and aging which modeling constitutes a major challenge that has not been met yet.

cond-mat.soft↗

arXiv2014

Thermal-orbital coupled tidal heating and habitability of Martian-sized extrasolar planets around M stars

M type stars are good targets in the search for habitable extrasolar planets. Because of their low effective temperatures, the habitable zone of M stars is very close to the star itself. For planets close to their stars, tidal heating plays an important role in thermal and orbital evolutions, especially when the planet orbit has a relatively large eccentricity. Although tidal heating interacts with the thermal state and orbit of the planet, such coupled calculations for extrasolar planets around M star have not been conducted. We perform coupled calculations using simple structural and orbital models, and analyze the thermal state and habitability of a terrestrial planet. Considering this planet to be Martian sized, the tide heats up and partially melts the mantle, maintaining an equilibrium state if the mass of the star is less than 0.2 times the mass of the Sun and the initial eccentricity of the orbit is more than 0.2. The reduction of heat dissipation due to the melted mantle allows the planet to stay in the habitable zone for more than 10 Gyr even though the orbital distance is small. The surface heat flux at the equilibrium state is between that of Mars and Io. The thermal state of the planet mainly depends on the initial value of the eccentricity and the mass of the star.

astro-ph.EP↗