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Osaka, Japan

is a private university in Daitō, Osaka, Japan. The predecessor of the school was founded in 1928, and it was chartered as a junior college in 1950. It became a four-year college in 1965. Osaka Sangyo University operated a satellite campus in Studio City, based on the former campus of Corvallis High School from 1987-2011. It is now occupied by Bridges Academy, which leased the upper upper level from 2005-2011 until it was bought out in early 2011. Wikipedia.

Inoue A.K.,Osaka Sangyo University
Monthly Notices of the Royal Astronomical Society | Year: 2010

It is essential to know galactic emissivity and spectrum of Lyman continuum (LyC) in order to understand the cosmic re-ionization. Here we consider an escape of nebular LyC from galaxies and examine the consequent spectral energy distribution. It is usually assumed that hydrogen nebular LyC mostly produced by bound-free transitions is consumed within photoionized nebulae (so-called on-the-spot approximation). However, an escape of the continuum should be taken into account if stellar LyC escapes from galaxies through 'matter-bounded' nebulae. We show that the escaping hydrogen bound-free LyC makes a strong bump just below the Lyman limit. Such a galaxy would be observed as a Lyman 'bump' galaxy. This bump results from the radiation energy redistribution of stellar LyC by nebulae. The strength of the bump depends on electron temperature in nebulae, escape fraction of stellar and nebular LyC, hardness of stellar LyC (i.e. metallicity, initial mass function, age and star formation history) and intergalactic medium attenuation. We can use the bump to find very young (∼1 Myr), massive (∼100 M⊙) and extremely metal-poor (or metal-free) stellar populations at z < 4. Because of the bump, 900-to-1500 Å luminosity density ratio (per Hz) becomes maximum (two-three times larger than the stellar intrinsic ratio) when about 40 per cent of the stellar LyC is absorbed by nebulae. The total number of escaping LyC photons increases due to the escape of nebular LyC but does not exceed the stellar intrinsic one. The radiation energy redistribution by nebulae reduces the mean energy of escaping LyC only by ≈10 per cent relative to that of stellar LyC. Therefore, the effect of the escape of nebular LyC on the re-ionization process may be small. © 2009 RAS. Source

Horikoshi R.,Osaka Sangyo University
Journal of Chemical Education | Year: 2015

A unique method has been developed using an interlocking building-block model equipped with magnets to illustrate the catalytic asymmetric hydrogenation of Î′-keto esters by a BINAP-ruthenium complex to enhance students' understanding of this process. A BINAP-ruthenium block model, mimicking the coordination environment around the metal center in the real complex, can be used to convert the Î′-keto ester model into a Î′-hydroxy ester model. This model was used to provide a greater understanding of the essence of the catalytic reaction and to assist students in their understanding of its mechanism. © 2014 The American Chemical Society and Division of Chemical Education, Inc. Source

Asano R.S.,Nagoya University | Takeuchi T.T.,Nagoya University | Hirashita H.,Academia Sinica, Taiwan | Inoue A.K.,Osaka Sangyo University
Earth, Planets and Space | Year: 2013

This paper investigates the main driver of dust mass growth in the interstellar medium (ISM) by using a chemical evolution model of a galaxy with metals (elements heavier than helium) in the dust phase, in addition to the total amount of metals. We consider asymptotic giant branch (AGB) stars, type II supernovae (SNe II), and dust mass growth in the ISM, as the sources of dust, and SN shocks as the destruction mechanism of dust. Furthermore, to describe the dust evolution precisely, our model takes into account the age and metallicity (the ratio of metal mass to ISM mass) dependence of the sources of dust. We have particularly focused on the dust mass growth, and found that in the ISM this is regulated by the metallicity. To quantify this aspect, we introduce a "critical metallicity", which is the metallicity at which the contribution of stars (AGB stars and SNe II) equals that of the dust mass growth in the ISM. If the star-formation timescale is shorter, the value of the critical metallicity is higher, but the galactic age at which the metallicity reaches the critical metallicity is shorter. From observations, it was expected that the dust mass growth was the dominant source of dust in the Milky Way and dusty QSOs at high redshifts. By introducing a critical metallicity, it is clearly shown that the dust mass growth is the main source of dust in such galaxies with various star-formation timescales and ages. The dust mass growth in the ISM is regulated by metallicity, and we emphasize that the critical metallicity serves as an indicator to judge whether the grain growth in the ISM is the dominant source of dust in a galaxy, especially because of the strong, and nonlinear, dependence on the metallicity. © The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB. Source

Thermodynamic parameter Γ and thermodynamic scaling parameter γ for low-frequency relaxation time, which characterize flip-flop motion in a nematic phase, were verified by molecular dynamics simulation with a simple potential based on the Maier-Saupe theory. The parameter Γ, which is the slope of the logarithm for temperature and volume, was evaluated under various conditions at a wide range of temperatures, pressures, and volumes. To simulate thermodynamic scaling so that experimental data at isobaric, isothermal, and isochoric conditions can be rescaled onto a master curve with the parameters for some liquid crystal (LC) compounds, the relaxation time was evaluated from the first-rank orientational correlation function in the simulations, and thermodynamic scaling was verified with the simple potential representing small clusters. A possibility of an equivalence relationship between Γ and γ determined from the relaxation time in the simulation was assessed with available data from the experiments and simulations. In addition, an argument was proposed for the discrepancy between Γ and γ for some LCs in experiments: the discrepancy arises from disagreement of the value of the order parameter P2 rather than the constancy of relaxation time τ 1* on pressure. © 2013 American Institute of Physics. Source

Zackrisson E.,The Oskar Klein Center | Inoue A.K.,Osaka Sangyo University | Jensen H.,The Oskar Klein Center
Astrophysical Journal | Year: 2013

The fraction of ionizing photons that escape (f esc) from z ≳ 6 galaxies is an important parameter for assessing the role of these objects in the reionization of the universe, but the opacity of the intergalactic medium precludes a direct measurement of f esc for individual galaxies at these epochs. We argue that since f esc regulates the impact of nebular emission on the spectra of galaxies, it should nonetheless be possible to indirectly probe f esc well into the reionization epoch. As a first step, we demonstrate that by combining measurements of the rest-frame UV slope β with the equivalent width of the Hβ emission line, galaxies with very high Lyman continuum escape fractions (f esc ≥ 0.5) should be identifiable up to z = 9 through spectroscopy with the upcoming James Webb Space Telescope (JWST). By targeting strongly lensed galaxies behind low-redshift galaxy clusters, JWST spectra of sufficiently good quality can be obtained for M 1500 ≲ -16.0 galaxies at z = 7 and for M 1500 ≲ -17.5 galaxies at z = 9. Dust-obscured star formation may complicate the analysis, but supporting observations with ALMA or the planned SPICA mission may provide useful constraints on this effect. © 2013. The American Astronomical Society. All rights reserved. Source

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