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Fukui, Y.,Kawamura, A.,Wong, T.,Murai, M.,Iritani, H.,Mizuno, N.,Mizuno, Y.,Onishi, T.,Hughes, A.,Ott, J.,Muller, E.,Staveley-Smith, L.,Kim, S. IOP Publishing 2009 The Astrophysical journal Vol.705 No.1
<P>We compare the CO (J = 1-0) and HI emission in the Large Magellanic Cloud in three dimensions, i.e., including a velocity axis in addition to the two spatial axes, with the aim of elucidating the physical connection between giant molecular clouds (GMCs) and their surrounding Hi gas. The CO J = 1-0 data set is from the second NANTEN CO survey and the HI data set is from the merged Australia Telescope Compact Array ( ATCA) and Parkes Telescope surveys. The major findings of our analysis are as follows: (1) GMCs are associated with an envelope of HI emission, (2) in GMCs [average CO intensity] proportional to [ average Hi intensity](1.1 +/- 0.1), and (3) the HI intensity tends to increase with the star formation activity within GMCs, from Type I to Type III. An analysis of the HI envelopes associated with GMCs shows that their average line width is 14 km s(-1) and the mean density in the envelope is 10 cm(-3). We argue that the HI envelopes are gravitationally bound by GMCs. These findings are consistent with a continual increase in the mass of GMCs via HI accretion at an accretion rate of 0.05 M-circle dot yr(-1) over a timescale of 10 Myr. The growth of GMCs is terminated via dissipative ionization and/or stellar-wind disruption in the final stage of GMC evolution.</P>
Physical properties of giant molecular clouds in the Large Magellanic Cloud
Hughes, A.,Wong, T.,Ott, J.,Muller, E.,Pineda, J. L.,Mizuno, Y.,Bernard, J.-P.,Paradis, D.,Maddison, S.,Reach, W. T.,Staveley-Smith, L.,Kawamura, A.,Meixner, M.,Kim, S.,Onishi, T.,Mizuno, N.,Fukui, Y. Blackwell Publishing Ltd 2010 Monthly notices of the Royal Astronomical Society Vol.406 No.3
<P>ABSTRACT</P><P>The Magellanic Mopra Assessment (MAGMA) is a high angular resolution <SUP>12</SUP>CO (<I>J</I>= 1 → 0) mapping survey of giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud using the Mopra Telescope. Here we report on the basic physical properties of 125 GMCs in the LMC that have been surveyed to date. The observed clouds exhibit scaling relations that are similar to those determined for Galactic GMCs, although LMC clouds have narrower linewidths and lower CO luminosities than Galactic clouds of a similar size. The average mass surface density of the LMC clouds is 50 M<SUB>⊙</SUB> pc<SUP>−2</SUP>, approximately half that of GMCs in the inner Milky Way. We compare the properties of GMCs with and without signs of massive star formation, finding that non-star-forming GMCs have lower peak CO brightness than star-forming GMCs. We compare the properties of GMCs with estimates for local interstellar conditions: specifically, we investigate the H <SMALL>I</SMALL> column density, radiation field, stellar mass surface density and the external pressure. Very few cloud properties demonstrate a clear dependence on the environment; the exceptions are significant positive correlations between (i) the H <SMALL>I</SMALL> column density and the GMC velocity dispersion, (ii) the stellar mass surface density and the average peak CO brightness and (iii) the stellar mass surface density and the CO surface brightness. The molecular mass surface density of GMCs without signs of massive star formation shows no dependence on the local radiation field, which is inconsistent with the photoionization-regulated star formation theory proposed by McKee. We find some evidence that the mass surface density of the MAGMA clouds increases with the interstellar pressure, as proposed by Elmegreen, but the detailed predictions of this model are not fulfilled once estimates for the local radiation field, metallicity and GMC envelope mass are taken into account.</P>
( K. Mizuno ),( T. Okada ),( M. Tsuboi ),( T. Hongou ),( M. Fukuda ),( S. Imaizumi ) 한국폐기물자원순환학회 2002 APLAS Vol.2002 No.2
지오멤브레인은 매립지 차수재로 사용되어 왔다. 일본에서는 평지의 부족으로 인해 종종 계곡매립이 이루어져왔다. 따라서 매립지는 많은 경사면을 갖고 있다. 복토층은 경사각이 H:L=1:1.5 이상인 경사면에서는 안정적이지 않으므로, 지오멤브레인은 복토층을 따로 두지 않으므로 포설 후 노출되게 된다. 이로 인해 지오멤브레인은 외적 환경에 직접적인 영향을 받는다. 외적 환경이 변화하면 stress(길이변형)와 strain(응력)이 일어나게 된다. 결과적으로 지오멤브레인의 장기적인 안정성을 위해서는 노출된 지오멤브레인의 stress와 strain 을 평가하는 것이 중요하다. 매우 추운 지역의 경우 낮은 온도(thermal stress)가 지오멤브레인의 주요한 영향인자로서 고려되어야 한다. 그리고 나서 slow load가 두 번째 인자로서 생각될 수 있다. 본 논문의 목적은 눈이 많이 내리는 지역에서의 지오멤브레인의 stress와 strain을 평가하는 것이다. 그림1과 그림2에 나타낸 것처럼, 일본 다설지역에서의 실규모 션장조사를 행하여 온도와 두꺼운 snow layer 아래에서의 slow load를 측정하였다. 본 논문은 현장 조사결과를 나타내고 매우 추운 지역에 적합한 최상의 지오멤브레인을 제안하고자 하였다.
Effeets of Local Damage on Asymptotic Stress Field of a Growing Creep Crack
Murakami, S .,Liu, Y .,Hirano, T .,Mizuno, M . 대한금속재료학회(대한금속학회) 1998 METALS AND MATERIALS International Vol.4 No.3
A parametric study on the effects of local damage field on the crack-tip stress field of a growing Mode I creep crack is performed in the framework of Continuum Damage Mechanics (CDM). According to the results of creep crack growth analysis based on CDM and Finite Element Method, the damage distribution 1-(D/D_(cr))=h(θ)r^m represented by a power law function of the radius r from the crack tip is postulated for the damage variable D. The damage effects are incorporated into the Norton creep law by means of the hypothesis of strain equivalence of CDM. The resulting two-point boundary value problems of differential equations for the growing creep cracks in the states of plane strain and plane stress are solved by means of a shooting method. For a given creep exponent n of the Norton law, the exponent p of the asymptotic stress field σ_(ij) ∝ r^n is found to be governed by the exponent m of the power law damage distribution r^m.
OPTICAL-INFRARED AND HIGH-ENERGY ASTRONOMY COLLABORATION AT HIROSHIMA ASTROPHYSICAL SCIENCE CENTER
UEMURA, MAKOTO,YOSHIDA, MICHITOSHI,KAWABATA, KOJI S.,MIZUNO, TSUNEFUMI,TANAKA, YASUYUKI T.,AKITAYA, HIROSHI,UTSUMI, YOUSUKE,MORITANI, YUKI,ITOH, RYOSUKE,FUKAZAWA, YASUSHI,TAKAHASHI, HIROMITSU,OHNO, MA The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
The Hiroshima Astrophysical Science Center (HASC) was founded in 2004 at Hiroshima University, Japan. The main mission of this institute is the observational study of various transient objects including gamma-ray bursts, supernovae, novae, cataclysmic variables, and active galactic nuclei by means of multi-wavelength observations. HASC consists of three divisions; the optical-infrared astronomy division, high-energy astronomy division, and theoretical astronomy division. HASC is operating the 1.5m optical-infrared telescope Kanata, which is dedicated to follow-up and monitoring observations of transient objects. The high-energy division is the key operation center for the Fermi gamma-ray space telescope. HASC and the high-energy astronomy group in the department of physical science at Hiroshima University are closely collaborating with each other to promote multi-wavelength time-domain astronomy. We report the recent activities of HASC and some science topics pursued by this multi-wavelength collaboration.