• Title/Summary/Keyword: S-N line

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Algebraic Analysis for Partitioning Root and Stem Lodging in Rice Plant

  • Chang, Jae-Ki;Yeo, Un-Sang;Lee, Jeom-Sig;Oh, Byong-Geun;Kim, Jeong-Il;Yang, Sae-Jun;Ku, Yeon-Chung;Kim, Ho-Yeong;Sohn, Jae-Keun
    • KOREAN JOURNAL OF CROP SCIENCE
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    • v.51 no.6
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    • pp.539-543
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    • 2006
  • Lodging is classified as root lodging caused by the loss of supporting force in the root, bending caused by the deformation of the stem and breaking where the stem breaks down as loads exceeding critical elasticity were applied. This research excluded breaking which is not in a state of equilibrium and tried to partition the level of lodging using an algebraic model in root lodging and stem lodging, or bending. When a vertical load was applied, the deformation of the stem of rice plant showed the form of a quadratic equation. The trace of the panicle neck in the process of lodging was an ellipse-shape. When loading was pure root lodging, the trace of the panicle neck became a circle of which culm length is the radius. When it was a pure stem lodging, the trace of the panicle neck is an ellipse of which major axis is culm length and minor axis is 0.64* culm length. When both stem lodging and root lodging occurred in a natural setting, the partitioning of lodging can be calculated by a formula using eccentricity of an ellipse, S=e*100/0.768(S is the ratio of stem lodging in the whole lodging, e is eccentricity of the ellipse). This method is expected to be useful in simple lodging partitioning. We could also calculate the partitioning of stem lodging and root lodging as units of angles as an accuracy method, by using a straight line calculated by differentiating a quadratic equation of stem deformation at the origin of the coordinates. These two methods for dividing root and stem lodging showed different values. However, each of them showed almost same values with different lodging degree in one plant.

Changes of Tracheal Anastomosis Site in Growing Rats (흰쥐에서 기관절제 단단 문합부의 성장에 따른 변화)

  • 박희철
    • Journal of Chest Surgery
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    • v.26 no.5
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    • pp.343-348
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    • 1993
  • Growth of suture line and anastomosis is required for long-term success after the tracheal and bronchial surgery in infant and pediatric patient. We used various suture materials in these cases, but the results were differ. To select the adequate suture material in tracheal surgery, we tried next. Tracheal anastomoses were performed in 150 Sprague Dawley rats, aged 4 to 8 [mean 5.8] weeks and weight 62 to 106[mean 83.6] gram, to compare polydioxanone[PDS] 7-0, polyglactin 910[Vicryl]7-0, and polypropylene [prolene] 8-0 suture materials. In 150 rats, only 29[20%] were lived over 300 days, and the weight was 250 to 320[mean 289.5]gram. Cross sectional area of the anastomoses and two or three tracheal rings below anastomosis site were measured under microscope, and calculated and compared as Hsieh`s equition. Cross-sectional area,anastomosis site/normal site 100, were 89.4 $\pm$ 5.34% in PDS group[n=9], 75.7 $\pm$ 6.06% in Vicrylgroup [n = 10], and 80.8$\pm$ 4.06% in Prolene group[n = 10]. Histopathologic studies were done for all autopsies or put in death around 300 days postoperatively. PDS absorblion was not seen 16 weeks after suture but disappeared over 24 weeks slide. Vicryl absorbtion was noted postoperative 8 to 16 weeks, with marked tissue reaction. Prolene showed least tissue reaction, but the suture material was persisted with regional fibrotic capsule.Causes of death were respiratory failure in 76 cases, tracheal rupture in 22 cases, hemorrhage, biting, starvation and etc. in 23 cases. With the brief review of literatures, we report the results.

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Open Ended Folded-Slot Antenna with a Wide n-Shaped Slot for Ultra-Wideband Applications

  • Yoo, Jin-Ha;Lee, Young-Soon
    • International Journal of Internet, Broadcasting and Communication
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    • v.12 no.2
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    • pp.83-89
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    • 2020
  • A microstrip feedline based open ended folded-slot antenna is proposed for ultra-wideband (UWB) applications. The prototype of the proposed antenna is fabricated on the FR4 dielectric substrate. The proposed antenna has a wide n-shaped slot that is useful for designing circuit components on the same printed circuit board (PCB) as that of the radio frequency (RF) modules. The proposed antenna use two kinds of slots as radiators, and each slots have different characteristics because of the different type of ends of the slot. The wideband characteristic can be obtained by resonances of each slot which are occurred at different frequencies. The measured impedance bandwidth (S11≤ -10 dB) is 2.9-11.56 GHz, and the antenna peak gain is 2-4 dBi over the UWB range. The antenna has a stable omni-directional radiation pattern and only a small group-delay variation across the UWB passband. In addition, we present a modified design with band-notched characteristics of a 5 GHz wireless local area network (WLAN) frequency band.

HCN(1-0) OBSERVATIONS OF STARLESS CORES

  • SOHN J,;LEE C, W,;LEE H, M.;PARK Y.-S.;MYERS P. C.;LEE Y.;TAFALLA M.
    • Journal of The Korean Astronomical Society
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    • v.37 no.4
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    • pp.261-263
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    • 2004
  • We present a progress report on HCN(1-0) line observations toward starless cores to probe inward motions. We have made a single pointing survey toward the central regions of 85 starless cores and performed mapping observations of 6 infall candidate starless cores. The distributions of the velocity difference between HCN(1-0) hyperfine lines and the optically thin tracer $N_2H^+$(1-0) are significantly skewed to the blue, meaning that HCN(1-0) frequently detects inward motions. Their skewness to the blue is even greater than that of CS(2-1) Lee et al., possibly implying more infall occurrence than CS(1-0). We identify 19 infall candidates by using several characteristics illustrating spectral infall asymmetry seen in HCN(1-0) hyperfine lines, CS(3-2), CS(2-1), $DCO^+(2-1)$ and $N_2H^+$ observations. The HCN(1-0) F(O-l) with the least optical depth usually shows a similar intensity distribution to that of $N_2H^+$ which closely traces the density distribution of the cores, indicating that HCN(1-0) is less chemically affected and so believed to reflect kinematics occurring in rather inner regions of the cores. Detailed radiative transfer model fits of the spectra are underway to analyze central infall kinematics in starless cores.

Role of Intracellular $Ca^{2+}$ Signal in the Ascorbate-Induced Apoptosis in a Human Hepatoma Cell Line

  • Lee , Yong-Soo
    • Archives of Pharmacal Research
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    • v.27 no.12
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    • pp.1245-1252
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    • 2004
  • Although ascorbate (vitamin C) has been shown to have anti-cancer actions, its effect on human hepatoma cells has not yet been investigated, and thus, the exact mechanism of this action is not fully understood. In this study, the mechanism by which ascorbate induces apoptosis using HepG2 human hepatoblastoma cells is investigated. Ascorbate induced apoptotic cell death in a dose-dependent manner in the cells, was assessed through flow cytometric analysis. Contrary to expectation, ascorbate did not alter the cellular redox status, and treatment with antioxidants (N-acetyl cysteine and N,N-diphenyl-p-phenylenediamine) had no influence on the ascorbate-induced apoptosis. However, ascorbate induced a rapid and sustained increase in intracellular $Ca^{2+}$ concentration. EGTA, an extracellular $Ca^{2+}$ chelator did not significantly alter the ascorbate-induced intracellular $Ca^{2+}$ increase and apoptosis, whereas dantrolene, an intracellular $Ca^{2+}$ release blocker, completely blocked these actions of ascorbate. In addition, phospholipase C (PLC) inhibitors (U-73122 and manoalide) significantly suppressed the intracellular $Ca^{2+}$ release and apoptosis induced by ascorbate. Collectively, these results suggest that ascorbate induced apoptosis without changes in the cellular redox status in HepG2 cells, and that the PLC-coupled intracellular $Ca^{2+}$ release mechanism may mediate ascorbate-induced apoptosis.

Synthesis, Antibacterial, Docking and Anticancer Evaluation of N-Substituted Benzoyl Derivatives

  • Arthi, P.;Shobana, S.;Srinivasan, P.;Rahiman, A. Kalilur
    • Journal of Integrative Natural Science
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    • v.7 no.4
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    • pp.241-252
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    • 2014
  • A series of N-benzoylated ligands incorporating three different benzoyl groups 2,2'-(benzoyliminodiethylene)-4-substituted phenols ($L^{1,4,7}$), 2,2'-(4-nitrobenzoyliminodiethylene)-4-substituted phenols ($L^{2,5,8}$) and 2,2'-(3,5-dinitrobenzoyliminodiethylene)-4-substituted phenols ($L^{3,6,9}$) were synthesized and characterized by IR, $^1H$ NMR, $^{13}C$ NMR and mass spectroscopy. The In vitro antibacterial activity of investigated ligands were tested against human pathogenic bacteria such as four Gram (-) Enterococcus faecalis, Pseudomonas aeruginosa, Staphylococcus aureus, Vibrio cholera, Vibrio harveyi and two Gram (+) Staphylococcus aureus, Streptococcus mutans. Furthermore, docking studies were undertaken to gain insight into the possible binding mode of these compounds with the binding site of the topoisomerase II (PDB: 4FM9) enzyme which is involved in DNA superhelicity and chromosome seggregation. The N-benzoylated derivatives $L^{5,7,8}$ have significant anticancer activity as Topoisomerase inhibitors. The ligands $L^5$ and $L^8$ were tested for their anticancer activity against human liver adenocarcinoma (HepG2) cell line with the MTT assay.

Water and Methanol Maser Observations toward NGC 2024 FIR 6 with KVN

  • Choi, Minho;Kang, Miju;Byun, Do-Young;Lee, Jeong-Eun
    • The Bulletin of The Korean Astronomical Society
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    • v.37 no.2
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    • pp.103.2-103.2
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    • 2012
  • NGC 2024 FIR 6 is a star formation site in Orion and may contain a hypercompact H II region, FIR 6c, and a low-mass protostar, FIR 6n. The FIR 6 region was observed in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz, using KVN in the single-dish telescope mode. The water maser spectra displayed several velocity components and month-scale time variabilities. Most of the velocity components may be associated with FIR 6n while one component was associated with FIR 4, another young stellar object in the 22 GHz beam. A typical life time of the water-maser velocity-components is about 8 months. The components showed velocity fluctuations with a typical drift rate of about 0.01 km/s/day. The methanol class I masers were detected toward FIR 6. The methanol emission is confined within a narrow range around the systemic velocity of the FIR 6 cloud core. The methanol masers did not show a detectable time-variability. The methanol masers suggest the existence of shocks driven by either the expanding H II region of FIR 6c or the outflow of FIR 6n.

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Being a front-line dentist during the Covid-19 pandemic: a literature review

  • Fallahi, Hamid Reza;Keyhan, Seied Omid;Zandian, Dana;Kim, Seong-Gon;Cheshmi, Behzad
    • Maxillofacial Plastic and Reconstructive Surgery
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    • v.42
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    • pp.12.1-12.9
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    • 2020
  • Coronavirus is an enveloped virus with positive-sense single-stranded RNA. Coronavirus infection in humans mainly affects the upper respiratory tract and to a lesser extent the gastrointestinal tract. Clinical symptoms of coronavirus infections can range from relatively mild (similar to the common cold) to severe (bronchitis, pneumonia, and renal involvement). The disease caused by the 2019 novel coronavirus (2019-nCoV) was called Covid-19 by the World Health Organization in February 2020. Face-to-face communication and consistent exposure to body fluids such as blood and saliva predispose dental care workers at serious risk for 2019-nCoV infection. As demonstrated by the recent coronavirus outbreak, information is not enough. During dental practice, blood and saliva can be scattered. Accordingly, dental practice can be a potential risk for dental staff, and there is a high risk of cross-infection. This article addresses all information collected to date on the virus, in accordance with the guidelines of international health care institutions, and provides a comprehensive protocol for managing possible exposure to patients or those suspected of having coronavirus.

Transport of choline and its relationship to transport of cationic drugs in immortalized rat brain capillary endothelial cell line

  • Park, Hong-Mi;Lee, Kyeong-Eun;Lee, Na-Young;Kang, Young-Sook
    • Proceedings of the Korean Society of Applied Pharmacology
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    • 2003.11a
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    • pp.106-106
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    • 2003
  • Choline serves critical roles in the CNS both as a precursor of neurotransmitter and as an essential component of membrane phospholipids. The long-term maintenance of brain choline concentration is dependent on choline transport across the blood-brain barrier (BBB), And, we examined to elucidate the characteristics of transport of choline across the BBB using conditionally immortalized rat brain capillary endothelial cell line (TR-BBB) in vitro. The [$^3$H]choline in TR - BBB was increased by time dependently, but independent on Na$\^$+/, and the transport process is saturable with Michaelis-Menten constrant, Km of about 26 ${\mu}$M. The uptake of [$^3$H]choline is susceptible for inhibition by various organic cationic compounds including hemicholinium-3, tetraethylammonium chloride (TEA) and $\ell$-carnitine. Also, we investigated the relationship of transport of choline and cationic drugs. The uptake of [$^3$H]choline is inhibited by antioxidant, a-phenyl-n-tert-butyl nitrone (PBN) with IC$\sub$50/ of 1.2 mM. and by Alzheimer's disease therapeutics, such as acetyl $\ell$-carnitine, tacrine and donepezil. Also, choline uptake presented competitive inhibition with PBN, donepezil and acetyl $\ell$-carnitine in Lineweaver-Burk plot. In conclusion, TR-BBB cells express a saturable transport system for uptake of choline, and several cationic drugs may be transported into the brain by BBB choline transporter.

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A CYANOACETYLENE STUDY OF THE MOLECULAR DISK IN STAR FORMING REGIONS

  • Chung, H.S.;Kameya, Osamu;Morimoto, Masaki
    • Journal of The Korean Astronomical Society
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    • v.24 no.2
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    • pp.217-271
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    • 1991
  • We have observed dense core around young stellar objects, DR21, S140, Orion-KL, and L1551 using four millimeter-wave transitions of $HC_3N\;J$=4-3, J=5-4, J=10-9, and J=12-11. The spatial distribution of $HC_3N$ emission closely resembles the morphology of the previous CS observations that trace high density gas. These observations reveal the existence of $HC_3N$ dense cores around central IR source, elliptical in shape and almost perpendicular to the CO bipolar outflow axis. Small differences can be explained by that $HC_3N$ molecular line is more optically thin and is seen to be more detailed structure in the neighborhood of central IR sources. In S140 and Orion-KL, massive(${\sim}10\;M_{\odot}$), slowly rotating dense cores lie near at the central IR sources of bipolar outflows. The velocity channel maps of DR21 show that the bipolar outflow gas may have a correlation with the dense core of DR21. We analyzed intensities of the four lines to derive physical conditions in dense core from two methods, LTE and LVG. The column density of $HC_3N$, $N(HC_3N)$, between LTE and LVG calculations agree well with each other. The abundances of $HC_3N$ in each observing source have been estimated using the average values of $n(H_2)$ and $N(HC_3N)$ and assuming the size of dense core. The fractional $HC_3N$ abundances in massive dense cores of DR21, S140, and Orion-KL have a range of $(2-7){\times}10^{-10}$, while that of low mass dense core, L1551, has one order of magnitude greater value of $2{\times}10^{-9}$. This should be considered good agreement with the result by Morris et al.(1976). It may be considered that dense cores of DR21, S140, and Orion-KL may have almost same stage of chemical evolution, and their abundances have a small values relative to that of L1551. The column density $N(HC_3N)$ decreases with increasing distance from the densest part of the cloud, the central infrared source, and have the relation of $N(HC_3N){\varpropto}R^{\alpha}$, where a has a range of 0.65 to 0.89. The values of $n(H_2)$ are not varied with increasing distance from the dense core, and have almost same values. Therefore, it is considered that the dense cores in these regions probably consist of dense clumps in diffuse molecular gas medium, and $n(H_2)$ of each clump is ${\sim}10^5\;cm^{-3}$. Levels in the $T_{ex}$ increases with $n(H_2)$. It is considered that the $HC_3N$ dense cores are not completely thermalized. We examine the relationships between the luminosity of central infrared sources versus mass of the dense cores, and the luminosity of central infrared sources versus molecular hydrogen column density. Luminosities of the central IR sources show good correlation with mass and hydrogen column density of the dense core. Same has been found from CS observations. However, mass and size derived from $HC_3N$ observations are one order of magnitude smaller than those from CS. It can be interpreted that we see more central part of the cloud cores in $NC_3N$ lines than CS lines.

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