1,128 research outputs found
Explanation of Plates: Image of Buddha-at-Birth from Kuze Temple Site (Kept by the Board of Education, Joyo City, Nara)
No full textThe image of Buddha-at-Birth, introduced here, was excavated at the Kuze Temple Site at Kuze, Jōyō City, near Kyoto. Jōyō City, abundant in ancient temple and in dwelling sites. is now under development as a satellite town of Kyoto and Osaka. Since February 1975, the Board of Education has excavated many of these archaeological sites, among which was the Kuze Temple Site which contained earth podiums of the Golden Hall and the Pagoda. This temple seems to have had a Hokkeji type layout of buildings. On the north side of the South Great Gate site of the temple, this image was unearthed on March 31, 1975. It is almost perfect except that its right arm which points to heaven is about to break near the elbow. A long tenon behind the head suggests that it originally had a halo, though it is now missing.
Most of the images of Buddha-at-Birth from the seventh and eighth centuries are in bad condition having suffered from fire. This one, however, has no trace of having been burned and has the bright colour of gilding. This image measures 11.5 cm from the tip of the right hand pointing to heaven to the bottom of the stem of the lotus pedestal, and 7 cm from the top of the head to the bottom of the feet. As is usual with such small images, the entire image is cast in one mould, perhaps in the lost-wax technique. Thick gilding is done not only over the Buddha himself, but also over the lotus pedestal and its stem.
In this paper, the author discusses the art his torical significance of the image in relation to the other Buddha-at-Birth images from the seventh and eighth centuries. Generally speaking, those of the Asuka, Hakuhō and Nara Periods gradually changed from slender proportions to more rounded proportions. The skirts of earlier ones are generally short and expose both legs; the skirts of later figures gradually became longer until they reached the ankles. At the same time, drapery-folds changed from symmetrical to more irregular and complicated forms. The image of Buddha-at-Birth excavated at the Kuze Temple Site has a comparatively long, fully modelled head with a healthy countenance and a well-built body. The skirt it wears is long and reaches the ankles. These characteristics indicate that perhaps this image is not of the Hakuhō Period but of the next Nara Period. This presumption meets with the date of the roof tiles from this temple site.journal articl
Clinical significance of total and separated renal clearance in urological practice Part I : Preoperative and postoperative renal clearances, total and separated, in various urological diseases
No full textPre- and postoperative total renal clearance was estim a ted in 160 cases and separated renal clearance in 50 cases in which pyelo- or ureterolithotomy, nephrectomy, prostatectomy and partial cystectomy were performed. A few nonsurgical conditions were included. 1) The average level of pre- and postoperative clearances was found to b e significantly lower than normal. 2) Tota l renal clearance does not indicate exact renal function in urological diseases. 3) As to the effect of aging, both CPAH and CSTS were markedly lowered af t e r fourty years of age. 4) In t ravenous pyelography occasionally reflects better renal function than real one. 5) After pyelo- or ureterolithotomy CPAH rose on the affected side, however, re m ained unchanged or slightly decreased on the healthy side. CSTS elevated on both sides. 6) After nephrectomy compensatory function of solitary kidney was we l l demonstrated with CPAH and CSTS. Functionally compensation of the solitary kidney acquired after 41 of age was much less than those younger than 40 years old. 7) CPAH and CSTS were markedly elevated im m ediately after nephrectomy but they became gradually reduced as being 80-90% of normal value, after 6, -8 weeks. 8) No compensatory change of the solitary kidney after nephrecto m y was noted when its function had been originally reduced to below 50%
Comparison of flow patterns around stenotic area in elastic PVA-H model and in rigid-like silicone model
No full textW, Z and photon production at the LHC
No full textRecent results on W, Z and photon production at the LHC are presented
A search for the HOCO radical in the massive star-forming region Sgr B2(M)
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Previous issue date: 6Made available in DSpace on 2018-01-29T23:04:21Z (GMT). No. of bitstreams: 3
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Previous issue date: 6Despite importance of the origin of life, long lasting challenges to detect the simplest amino acid glycine (chem{H_2NCH_2COOH}) in interstellar medium has not been successful. As a preliminary step toward search for glycine, detection of its precursor has received attention. It is considered that glycine is produced by the reaction of the chem{HOCO} radical and the aminomethyl radical(chem{CH_2NH_2}) on interstellar grain surface:_x000d_
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chem{HOCO} + chem{CH_2NH_2} chem{H_2NCH_2COOH}.hspace{15pt} (1)_x000d_
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chem{HOCO} is produced by the reaction of chem{OH} + chem{CO} chem{HOCO} and/or chem{HCOOH} chem{HOCO} + chem{H}. However, chem{HOCO} and chem{CH_2NH_2} have not been investigated in interstellar medium. Recently, we determined the accurate molecular constants of chem{HOCO}.footnote{T. Oyama ., . . . {bf 134}, 174303 (2011).} Thus, accurate rest frequencies were derived from the constants. In the present study, we carried out the observations of chem{HOCO} in the massive star-forming region Sgr B2(M), having variety of interstellar molecules, with Nobeyama 45 m radio telescope. Although chem{HOCO} could not be detected in Sgr B2(M), the upper limit of the column density was derived to be 9.010 cm via the spectrum in the 88 GHz region by the rotational diagram method. If the reaction (1) is a main process of the glycine production in this region, an extremely deep search is needed to detect glycine. _x000d
Precise determination of the isotopic ratios of HC3N in the massive star-forming region Sgr B2(M)
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Previous issue date: 6Made available in DSpace on 2018-01-29T23:04:19Z (GMT). No. of bitstreams: 3
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Previous issue date: 6Isotopic ratio is a critical parameter in understanding galactic chemical evolution. In addition, carbon isotopic ratio of an organic molecule reflects its formation mechanism. In the present study, we observed the simplest cyanopolyyne chem{HC_3N} and its isotopomers in the massive star-forming region Sgr B2(M) with Nobeyama 45 m radio telescope. The column density and the rotational temperature of chem{HC_3N} were determined to be 1.610 cm and 163 K, respectively. The ratios of the column densities for the C isotopomers were derived to be [chem{H^{13}CCCN}]:[chem{HC^{13}CCN}]:[chem{HCC^{13}CN}] = 1:1.03(4):0.99(3), where the rotational temperature was fixed to that of HCN. The ratios are almost the same, suggesting no isotopic fractionation for the specific carbon atoms in HCN. Therefore, it is considered that the C isotope exchange reactions do not contribute to make difference among the column densities of the three C isotopomers in the relatively warm region of Sgr B2(M). In contrast, the reported ratios in TMC-1 and L1527 are 1:1.0(1):1.4(2)footnote{S. Takano ., . . {bf 329}, 1156 (1998).} and 1:1.01(2):1.35(3),footnote{M. Araki ., {bf 833}, 291 (2016).} respectively, where the ratios show higher abundance of HCCCN._x000d_
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We also observed the transitions in the vibrational excited states of chem{HC_3N}. The rotational temperature of 362 K in the , , and excited states was obviously different from that of the vibrational ground state
DETECTION OF CH3CN IN DIFFUSE CLOUD TOWARD GALACTIC CENTER SGRB2(M)
No full textOrganic molecules have been detected mainly in dense clouds. As diffuse clouds are a previous phase of dense clouds in evolutionary history of interstellar clouds, detection of organic molecules in diffuse clouds can reveal a longer history of organic molecules. Despite of its importance, emission lines from molecules in diffuse clouds are difficult to detect because of inactive excitation by collisions and active cooling by radiations. However, for CHCN, a rotation around a molecular axis cannot be cooled by radiations. Thus, this molecule can be detected by absorption having a relatively strong line from rotational levels, because these levels are well populated. In our previous work, this rotational behavior was formulated as ``Hot Axis Effect" [1]. In this work, to detect this molecule in diffuse clouds that are more diffuse than the known diffuse clouds carrying organic molecules [2], we have been searched for absorption lines of the = 4–3 transition of CHCN at 73 GHz toward the galactic center SgrB2(M) by using Nobeyama 45 m telescope. As a result, this transition was detected in the diffuse cloud of SgrB2 envelop. The column density was derived to be 2 10 cm. Therefore, we detected an organic molecule in the diffuse cloud that are more diffuse than the known diffuse cloud carrying CHCN [2] because this molecule detected shows the low excitation temperature of 3 K and the high kinetic temperature of 70 K.
[1] Araki et al. Astronomical Journal, 148, 87 (2014)
[2] Muller et al., AA, 535, 103 (2011
Detection of CH3CN in diffuse cloud toward galactic center SgrB2(M)
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Previous issue date: 6Made available in DSpace on 2018-12-12T22:38:32Z (GMT). No. of bitstreams: 4
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Previous issue date: 6Organic molecules have been detected mainly in dense clouds. As diffuse clouds are a previous phase of dense clouds in evolutionary history of interstellar clouds, detection of organic molecules in diffuse clouds can reveal a longer history of organic molecules. Despite of its importance, emission lines from molecules in diffuse clouds are difficult to detect because of inactive excitation by collisions and active cooling by radiations. However, for CH3CN, a rotation around a molecular axis cannot be cooled by radiations. Thus, this molecule can be detected by absorption having a relatively strong line from J = K rotational levels, because these levels are well populated. In our previous work, this rotational behavior was formulated as “Hot Axis Effect” [1]. In this work, to detect this molecule in diffuse clouds that are more diffuse than the known diffuse clouds carrying organic molecules [2], we have been searched for absorption lines of the JK = 43–33 transition of CH3CN at 73 GHz toward the galactic center SgrB2(M) by using Nobeyama 45 m telescope. As a result, this transition was detected in the diffuse cloud of SgrB2 envelop. The column density was derived to be 2 × 1014 cm−2 . Therefore, we detected an organic molecule in the diffuse cloud that are more diffuse than the known diffuse cloud carrying CH3CN [2] because this molecule detected shows the low excitation temperature of ∼ 3 K and the high kinetic temperature of ∼ 70 K.
[1] Araki et al. Astronomical Journal, 148, 87 (2014)
[2] Muller et al., A&A, 535, 103 (2011
Detection of ch3nco in the galactic center star-forming region sagittarius b2(m) by radio astronomical observations
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Previous issue date: 23Large difference of chemical compositions between molecular clouds and comets is a big question for astrochemistry. The case of a pre-biotic molecule \chem{CH_3NCO} is one of them. The abundance ratio of [\chem{CH_3NCO}]/[\chem{HNCO}] is high in the comet 67P ( 4, [1]), although it is low (0.02 0.3, e.g., [2]) in molecular clouds. An abundance of \chem{CH_3NCO} is expected to be held and/or increased during evolutionary process of a cloud. A pair of an old core and a young core having the similar chemical compositions needs to be investigated for this evolutionary process. In this work, we aimed to detect \chem{CH_3NCO} in the middle (M) core, which is relatively older than the north (N) core, in the Galactic Center star-forming region Sagittarius B2 with the 45 m telescope of Nobeyama Radio Observatory. The rotational transitions of = 10 9 to 13 12 for \chem{CH_3NCO} were detected in the 85 114 GHz region. The column density and the rotational temperature are derived to be = (4.3 2.1) cm and = (32 9) K, respectively, assuming local thermal equilibrium. Similarly, an abundance of \chem{HNCO} is estimated to be = (1.3 0.5) cm ( = 21 2 K), giving the ratio of [\chem{CH_3NCO}]/[\chem{HNCO}] = 0.032. Thus, as a simplest model, it is suggested that an abundance of \chem{CH_3NCO} is held during evolutionary process of the Sagittarius B2 region.
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\noindent [1] Goesmann et al., Science, 349, 689 (2015). [2] Halfen et al., ApJ, 812, L5 (2015)
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