Shibuya-ku, Japan
Shibuya-ku, Japan

Kokugakuin University is a private university, whose main office is located in Tokyo's Shibuya district. It was established in 1920. Wikipedia.

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Sato M.,Honda Electronics Co. | Sato H.,Kokugakuin University
Physics Essays | Year: 2017

Entanglement that is represented by the conservation law is instantaneous and permanent. Entanglement is not uniquely quantum mechanical, although it looks conspicuous in quantum mechanics. Newtonian mechanics are in the lines of entanglement. Einstein-Podolsky-Rosen (EPR)-type sequential experiments can be performed using an entangled photon beam and two pairs of linear polarization analyzers setting at cross-Nicol condition (i.e., setting at orthogonal to each other). In this experiment, we predict that the "continuity of quantum entanglement" under a pure Hamiltonian evolution is detected. © 2017 Physics Essays Publication.

Panwar N.,National Central University | Panwar N.,University of Delhi | Chen W.P.,National Central University | Pandey A.K.,Aryabhatta Research Institute of Observational science ARIES | And 5 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2014

Bright-rimmed clouds (BRCs), illuminated and shaped by nearby OB stars, are potential sites of recent/ongoing star formation. Here we present an optical and infrared photometric study of three BRCs: BRC 5, BRC 7 and BRC 39 to obtain a census of the young stellar population, thereby inferring the star formation scenario, in these regions. In each BRC, the Class I sources are found to be located mostly near the bright rim or inside the cloud, whereas the Class II sources are preferentially outside, with younger sources closer to the rim. This provides strong support to sequential star formation triggered by radiation-driven implosion due to the ultraviolet radiation. Moreover, each BRC contains a small group of young stars being revealed at its head, as the next-generation stars. In particular, the young stars at the heads of BRC 5 and BRC 7 are found to be intermediate-/high-mass stars, which, under proper conditions, may themselves trigger further star birth, thereby propagating star formation out to long distances. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

Jose J.,Aryabhatta Research Institute of observational science ARIES | Pandey A.K.,Aryabhatta Research Institute of observational science ARIES | Ogura K.,Kokugakuin University | Ojha D.K.,Tata Institute of Fundamental Research | And 5 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2011

We present a comprehensive multiwavelength analysis of the young cluster NGC 1624 associated with the Hii region Sh2-212 using optical UBVRI photometry, optical spectroscopy and GMRT radio continuum mapping along with the near-infrared (NIR) JHK archival data. From optical observations of the massive stars, reddening E(B-V) and distance to the cluster are estimated to be 0.76-1.00mag and 6.0 ± 0.8kpc, respectively. The present analysis yields a spectral class of O6.5V for the main ionizing source of the region, and the maximum post-main-sequence age of the cluster is estimated as ~4Myr. Detailed physical properties of the young stellar objects (YSOs) in the region are analysed using a combination of optical/NIR colour-colour and colour-magnitude diagrams. The distribution of YSOs in the (J-H)/(H-K) NIR colour-colour diagram shows that a majority of them have AV≤ 4mag. However, a few YSOs show AV values higher than 4mag. Based on the NIR excess characteristics, we identified 120 probable candidate YSOs in this region, which yield a disc frequency of ~20 per cent. However, this should be considered as a lower limit. These YSOs are found to have an age spread of ~5Myr with a median age of ~2-3Myr and a mass range of ~0.1-3.0 M⊙. A significant number of YSOs are located close to the cluster centre and we detect an enhanced density of reddened YSOs located/projected close to the molecular clumps detected by Deharveng et al. at the periphery of NGC 1624. This indicates that the YSOs located within the cluster core are relatively older in comparison to those located/projected near the clumps. From the radio continuum flux, the spectral class of the ionizing source of the ultracompact Hii (UCHii) region at the periphery of Sh2-212 is estimated to be ~B0.5V. From the optical data, the slope of the mass function (MF) Γ, in the mass range 1.2 ≤M/M⊙ < 27, can be represented by a single power law with a slope -1.18 ± 0.10, whereas the NIR data in the mass range 0.65 ≤M/M⊙ < 27 yield Γ=-1.31 ± 0.15. Thus the MF agrees fairly with the Salpeter value. The slope of the K-band luminosity function (KLF) for the cluster is found to be 0.30 ± 0.06, which is in agreement with the values obtained for other young clusters. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

Chauhan N.,Aryabhatta Research Institute of observational science ARIES | Pandey A.K.,Aryabhatta Research Institute of observational science ARIES | Ogura K.,Kokugakuin University | Jose J.,Aryabhatta Research Institute of observational science ARIES | And 3 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2011

The aim of this paper is to present the results of photometric investigations of the central cluster of the W5 E Hii region as well as a follow-up study of the triggered star formation in and around bright-rimmed clouds (BRCs). We have carried out wide-field UBVIC and deep VIC photometry of the W5 E Hii region. A distance of ~2.1 kpc and a mean age of ~1.3 Myr have been obtained for the central cluster. The young stellar objects (YSOs) associated with the region are identified on the basis of near-infrared and mid-infrared observations. We confirmed our earlier results that the average age of the YSOs lying on/inside the rim is younger than those lying outside the rim. The global distribution of the YSOs shows an aligned distribution from the ionizing source to the BRCs. These facts indicate that a series of radiation-driven implosion processes proceeded from near the central ionizing source towards the periphery of the W5 E Hii region. We found that, in general, the age distributions of the Class II and Class III sources are the same. This result is apparently in contradiction to the conclusion by Bertout, Siess & Cabrit and Chauhan et al. that classical T Tauri stars evolve to weak-line T Tauri stars. The initial mass function of the central cluster region in the mass range 0.4 ≤M/M⊙≤ 30 can be represented by Γ=-1.29 ± 0.04. The cumulative mass functions indicate that in the mass range 0.2 ≤M/M⊙≤ 0.8, the cluster region and BRC NW have more low-mass YSOs compared to BRCs 13 and 14. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

Deguchi T.,Tokyo Institute of Technology | Takahashi K.,Tokyo Institute of Technology | Takahashi K.,Kokugakuin University | Takayasu H.,Sony | And 2 more authors.
PLoS ONE | Year: 2014

We investigate the economic hubs and authorities of the world trade network (WTN) from 1992 to 2012, an era of rapid economic globalization. Using a well-defined weighted hyperlink-induced topic search (HITS) algorithm, we can calculate the values of the weighted HITS hub and authority for each country in a conjugate way. In the context of the WTN, authority values are large for countries with significant imports from large hub countries, and hub values are large for countries with significant exports to high-authority countries. The United States was the largest economic authority in the WTN from 1992 to 2012. The authority value of the United States has declined since 2001, and China has now become the largest hub in the WTN. At the same time, China's authority value has grown as China is transforming itself from the "factory of the world" to the "market of the world." European countries show a tendency to trade mostly within the European Union, which has decreased Europe's hub and authority values. Japan's authority value has increased slowly, while its hub value has declined. These changes are consistent with Japan's transition from being an export-driven economy in its high economic growth era in the latter half of the twentieth century to being a more mature, economically balanced nation. © 2014 Deguchi et al.

Sugawara J.,Japan National Institute of Advanced Industrial Science and Technology | Hayashi K.,Japan National Institute of Advanced Industrial Science and Technology | Hayashi K.,Kokugakuin University | Tanaka H.,University of Texas at Austin
Journal of Hypertension | Year: 2014

OBJECTIVES:: Brachial-ankle pulse wave velocity (baPWV) is one of few indices of arterial stiffness that has been incorporated into a routine clinical setting. baPWV is associated with markers of central arterial stiffness, but the absolute values are substantially higher than other PWV measures. We tested the hypothesis that the height-based formulas underestimate actual arterial path lengths overestimating PWV values. METHODS:: Arterial path lengths were measured in 220 adults by the three-dimensional MRI arterial tracing. RESULTS:: Actual path lengths from the heart to the ankle (Lha) and from the heart to the brachium (Lhb) were significantly longer than those estimated by the height-based formula (1464±85 vs. 1439±71 mm and 476±41 vs. 335±19 mm, both P < 0.0001). Consequently, the MRI-based effective path length for baPWV (Lha - Lhb) was shorter than the height-based path length (988±66 vs. 1105±52 mm, P < 0.0001). baPWV re-calculated by using the MRI-based path length was 11% lower than that derived from the height-based path length but was still 45% greater than carotid-femoral PWV (cfPWV). Both height-based and MRI-based baPWV measures were significantly associated with cfPWV (r=0.84 and 0.87, both P < 0.0001). CONCLUSION:: We concluded that the height-based formulas to estimate arterial path length grossly overestimate the actual path length resulting in the overestimation of PWV values and that baPWV was still significantly higher than other PWV measures even when the actual path length is used to calculate. These results suggest that other methodological considerations apart from the arterial path length estimation contribute to higher absolute baPWV values. Copyright © Lippincott Williams & Wilkins.

Imanaka T.,Kyoto University | Endo S.,Hiroshima University | Sugai M.,Kokugakuin University | Ozawa S.,Nihon University | And 2 more authors.
Health Physics | Year: 2012

Following the news that the radiation level in Iitate Village, located 25-45 km from the Fukushima Daiichi Nuclear Power Plant, was seriously increased, an urgent field survey was carried out on 28 and 29 March 2011. Radiation levels at 130 locations were measured inside a van that traveled throughout the village using a CsI pocket survey meter and an ionization chamber. Soil samples were also taken at five locations and submitted to gamma ray analysis using a Ge detector. A radiation exposure rate of more than 20 μSv h-1 was observed in the southern part of Iitate Village. Volatile radionuclides such as iodine and cesium were found to be the main components of radioactive contamination. A trace amount of plutonium isotopes originating from the accident was also confirmed in several soil samples, the level of which was less than the global fallout. Based on the measured density of radionuclides at the highest contamination location during the present survey, an exposure rate of about 200 μGy h-1 at 1 m above the ground was estimated at the time of the radioactive deposition on March 15. At this location, the cumulative exposure would reach 50 mGy in the middle of May 2011. Copyright © 2012 Health Physics Society.

Chauhan N.,Aryabhatta Research Institute of Observational science ARIES | Ogura K.,Kokugakuin University | Pandey A.K.,Aryabhatta Research Institute of Observational science ARIES | Samal M.R.,Aryabhatta Research Institute of Observational science ARIES | Bhatt B.C.,Indian Institute of Astrophysics
Publications of the Astronomical Society of Japan | Year: 2011

The HII region IC 1848 harbors a lot of intricate elephant trunk-like structures that look morphologically different from usual bright-rimmed clouds (BRCs). Of particular interest is a concentration of thin and long elephant trunk-like structures in the southeastern part of IC 1848E. Some of them have an apparently associated star or two stars at their very tip. We conducted VI c photometry of several of these stars. Their positions on the V/(V-Ic) color-magnitude diagram as well as the physical parameters obtained by SED fittings indicate that they are lowmass pre-main-sequence stars having ages of mostly one Myr, or less. This strongly suggests that they formed from elongated, elephant trunk-like clouds. We presume that such elephant trunk-like structures are genetically different from BRCs, on the basis of the differences in morphology, size distributions, and the ages of the associated young stars. We suspect that those clouds have been caused by hydrodynamical instability of the ionization/shock front of the expanding HII region. Similar structures often show up in recent numerical simulations of the evolution of HII regions. We further hypothesize that this mechanism makes a third mode of triggered star formation associated with HII regions, in addition to the two known mechanisms, i.e., collect-and-collapse of the shell accumulated around an expanding HII region and radiation-driven implosion of BRCs originated from pre-existing cloud clumps. © 2011. Astronomical Society of Japan.

Sato M.,Honda Electronics Co. | Sato H.,Kokugakuin University
Physics Essays | Year: 2015

The speed of light is observed differently depending on the observer's velocity. Therefore, the Lorentz contraction cannot be derived; the length contraction is unnecessary in physics. Time dilation has been experimentally confirmed. Using Einstein and Feynman light clock, we show that the Lorentz time dilation is derived in Fresnel's ether. The Galilean transformation with Lorentz time dilation is introduced. © 2015 Physics Essays Publication.

Sato M.,Honda Electronics Co. | Sato H.,Kokugakuin University
Physics Essays | Year: 2015

The equivalence of inertial and gravitational masses is discussed. The resistance (i.e., the impedance) from accelerated motion in the ether is considered to be inertia. Mass is an eddy-making resistance generated by the accelerated motion of a massive particle in the ether, in which the eddy is de Broglie wave, that is, adhered photon. The resistance in the ether is isotropic; thus, the inertial mass is equivalent to the gravitational mass. Copyright © 2015 Physics Essays Publication.

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