Zobrazeno 1 - 9
of 9
pro vyhledávání: '"Ohkubo T"'
Autor:
Oida, Y., Sakuragi, S., Igari, T., Nakajima, Y., Ro, E., Shimizu, F., Futami, M., Hakozaki, Y., Ohkubo, T., Ishikawa, H., Takada, S., Sawada, S., Murakami, K., Suzuki, K., Maruyama, I.
Finite element method (FEM) modeling of the volumetric expansion phenomenon associated with the accumulation of irradiation was performed on rocks in a concrete for nuclear power plant. The FEM mesh of sandstone, tuff, and granite was created based o
Externí odkaz:
http://arxiv.org/abs/2206.07140
Autor:
Kozuka, Y., Isogami, S., Masuda, K., Miura, Y., Das, Saikat, Fujioka, J., Ohkubo, T., Kasai, S.
Publikováno v:
Phys. Rev. Lett. 126, 236801 (2021)
Spin-charge conversion via spin-orbit interaction is one of the core concepts in the current spintronics research. The efficiency of the interconversion between charge and spin current is estimated based on Berry curvature of Bloch wavefunction in th
Externí odkaz:
http://arxiv.org/abs/2105.03574
Autor:
Fischbacher, J., Kovacs, A., Kühnel, L. Exl J., Mehofer, E., Sepehri-Amin, H., Ohkubo, T., Hono, K., Schrefl, T.
Magnetization reversal in permanent magnets occurs by the nucleation and expansion of reversed domains. Micromagnetic theory offers the possibility to localize the spots within the complex structure of the magnet where magnetization reversal starts.
Externí odkaz:
http://arxiv.org/abs/1805.09798
Autor:
Motohara, K., Maeda, K., Gerardy, C. L., Nomoto, K., Tanaka, M., Tominaga, N., Ohkubo, T., Mazzali, P. A., Fesen, R. A., Hoeflich, P., Wheeler, J. C.
Publikováno v:
Astrophys.J.652:L101-L104,2006
We present near-infrared spectra of late phase (>200 d) Type Ia supernovae (SNe Ia) taken at the Subaru telescope. The [Fe II] line of SN 2003hv shows a clear flat-topped feature, while that of SN 2005W show less prominent flatness. In addition, a la
Externí odkaz:
http://arxiv.org/abs/astro-ph/0610303
Publikováno v:
Astrophys.J.653:1145-1171,2006
We calculate the evolution of heavy element abundances from C to Zn in the solar neighborhood adopting our new nucleosynthesis yields. Our yields are calculated for wide ranges of metallicity (Z=0-Z_\odot) and the explosion energy (normal supernovae
Externí odkaz:
http://arxiv.org/abs/astro-ph/0608688
Publikováno v:
Astrophys.J.645:1352-1372,2006
We calculate evolution, collapse, explosion, and nucleosynthesis of Population III very-massive stars with 500$M_{\odot}$ and 1000$M_{\odot}$. Presupernova evolution is calculated in spherical symmetry. Collapse and explosion are calculated by a two-
Externí odkaz:
http://arxiv.org/abs/astro-ph/0507593
Recent studies of core-collapse supernovae have revealed the existence of two distinct classes of massive supernovae (SNe): 1) very energetic SNe (Hypernovae), whose kinetic energy (KE) exceeds $10^{52}$ erg, about 10 times the KE of normal core-coll
Externí odkaz:
http://arxiv.org/abs/astro-ph/0506597
A key question for supernova cosmology is whether the peak luminosities of Type Ia supernovae (SNe Ia) are sufficiently free from the effects of cosmic and galactic evolution. To answer this question, we review the currently popular scenario of SN Ia
Externí odkaz:
http://arxiv.org/abs/astro-ph/0308138
Publikováno v:
Prog.Theor.Phys.Suppl.151:44-53,2003
Stars more massive than $\sim$ 20 - 25 \ms form a black hole at the end of their evolution. Stars with non-rotating black holes are likely to collapse "quietly" ejecting a small amount of heavy elements (Faint supernovae). In contrast, stars with rot
Externí odkaz:
http://arxiv.org/abs/astro-ph/0306412