• 한국초지조사료학회지
• /
• 제5권2호
• /
• pp.121-126
• /
• 1985

본(本) 시험(試驗)은 sorghum식물(植物)에 있어서 Cyanogenic glycosides의 합성(合成) 및 축적형태(蓄積形態)를 구명(究明)하기 위하여 sorghum hybrid의 Pioneer과 sorghum X sudangrass hybrid의 Sioux를 공시품종(供試品種)으로 하여 포장(圃場) 및 Phytotron시험(試驗)으로 실시(實施)하였다. Phytotron의 주(晝)/야간(夜間) 온도(溫度)는 30/25, 25/20, 28/18 및 $18/8^{\circ}C$로 하였으며 온도처리(溫度處理)는 출현기(出現期), 4 엽기(葉期), 6 엽기(葉期) 및 8 엽기(葉期)를 대상(對象)으로 실시(實施)하였다. 1979-'80년간(年間) 얻어진 시험결과(試驗結果)를 요약(要約)하면 다음과 같다. 1. HCN의 합성(合成) 및 축적(蓄積)은 출현(出現)과 동시(同時)에 이루어져 출현후(出現后) 5 - 7 일(日) 이 경과된 2 엽기식물(葉期植物)에서 각각(各各) Pioneer 931 2384ppm 및 Sioux 1798ppm으로 최고농도수준(最高濃度水準)에 달한다. 그러나 이들 함량(含量)은 생육(生育)이 진행(進行)됨에 따라 급격(急激)히 감소(減少)되어 출수기(出穗期)에는 각각(各各) 173ppm 및 70ppm으로 하락(下落)된다. 2. 생육기간중(生育期間中) HCN의 농도변화(濃度變化)는 LWR 및 LAR와는 정(正)(+)의 상관(相關)이 초장생육(草長生育)과는 부(負)(-)의 상관(相關)($P{\leqq}0.1%$)이 있다. 3 . 식물체중(植物體中) HCN 분포(分布)는 유수(幼穗)가 형성(形成)되기 이전(以前)의 유식물(幼植物)에서는 엽부위(葉部位)에 다량(多量) 분포(分布)되어 있으나 유수형성기(幼穗形成期) 이후(以后)에는 엽(葉)과 경부위간(莖部位間) HCN농도(濃度) 차이(差異)가 크지 않다. 4. Cyanogenic glycosides의 합성(合成)은 온도(溫度)가 상승(上昇)됨에 따라 비례적(比例的)으로 증가(增加)하나 식물체내(植物體內)의 HCN 축적(蓄積)은 고온(高溫)($30/25^{\circ}C$)에서 보다 저온(低溫)($18/8^{\circ}C$)에서 보다 크게 일어난다. 5. Cyanogenic glycosides의 합성(合成) 및 축적(蓄積)은 질소질비료(窒素質肥料) 및 NRA의 영향(影響)을 크게 받으므로 sorghum 식물체내(植物體內)에서의 HCN농도(濃度)는 $NO_3$축적(蓄積)과 높은 정(正)(+)의 상관(相關)이 있다.

• 천문학회지
• /
• 제38권2호
• /
• pp.245-248
• /
• 2005

We present mm observations with the IRAM 30m radiotelescope of the HCN (J=1-0) and HCO+ (J=1-0) emission lines from Giant Moleculat Clouds (GMC) in the disk of the Andromeda Galaxy, The selected GMC targets have various morphology and environments, including locations within spiral arms or in interarm regions and with galactocentric radii ranging from 2.4 to 15.5 kpc over the disk. The radial distributions of the ratios HCN/CO and HCO+ /CO are discussed and their values are compared to other galaxies.

• 한국자기공명학회논문지
• /
• 제12권2호
• /
• pp.89-95
• /
• 2008

Function of protein is frequently related with tautomeric states of histidine sidechains. Thus, several NMR experiments were developed to determine the tautomeric states of histidines. However, poor sensitivity of these experiments caused by long duration of magnetization transfer periods is unavoidable. Here, we alleviate the sensitivity of HCN experiment for determining the tautomeric states of histidine residues using TROSY principle to suppress transverse relaxation of $^{13}C$ spins during long polarization transfer delays involving $^{13}C-^{15}N$ scalar couplings. In addition, this experiment was used to assign the sidechain resonances of histidines. These assignments can be used to follow the pH-titration of histidine sidechains.

• Bulletin of the Korean Chemical Society
• /
• 제33권12호
• /
• pp.4098-4102
• /
• 2012

The potential energy surface (PES) for the loss of HCN from the pyrimidine molecular ion has been explored using quantum chemical calculations. Possible reaction pathways to form five $C_3H_3N^{+{\bullet}}$ isomers have been obtained with Gaussian 4 model calculations. The rate constant for the HCN loss and the product branching ratio have been calculated using the Rice-Ramsperger-Kassel-Marcus theory on the basis of the obtained PES. The resultant rate constant agrees with the previous experimental result. By a kinetic analysis, it is proposed that the formation of $CH=CHC{\equiv}NH^{+{\bullet}}$ is favored near the dissociation threshold, while the formation of $CH=CHN{\equiv}CH^{+{\bullet}}$ is favored at high energies.

• 약학회지
• /
• 제4권1호
• /
• pp.43-46
• /
• 1959

A new quantitiative analytical method of prussic acid by "Microdiffusion analysis" was studied. HCN-Glucoside of ARMENIACA was hydrolysed with KOH in out-room of unit, and then concentrated sulfuric acid was poured in order to liberate the HCN gas. The liberated gas was absorbed into nickel sulfate solution of inner room of unit quantitatively. The excess of nickel sulfate was determined by EDTA Reagent using MX-indicator. By this method, the following results were obtained: (1) It was needed more than 4 hours, in order to hydrolyse completely at $50^{\circ}C$, but could be shortened to 3 hrs. at $^60{\circ}C$. (2) It was completely absorbed into nickel sulfate solution after 30min.

• 천문학회지
• /
• 제36권4호
• /
• pp.271-282
• /
• 2003

We present results of a $H^{13}CN$ J=1-0 mapping survey of molecular clouds toward the Galactic Center (GC) region of $-1.6^{\circ}{\le}{\iota}{\le}2^{\circ}$ and $-0.23^{\circ}{\le}b{\le}0.30^{\circ}$ with 2' grid resolution. The $H^{13}CN$ emissions show similar distribution and velocity structures to those of the $H^{12}CN$ emissions, but are found to better trace the feature saturated with $H^{12}CN$ (1-0). The bright components among multi-components of $H^{12}CN$ line profiles usually appear in the $H^{13}CN$ line while most of the dynamically forbidden, weak $H^{12}CN$ components are seldom detected in the $H^{13}CN$ line. We also present results of other complementary observations in $^{12}CO$ (J=1-0) and $^{13}CO$ (J=1-0) lines to estimate physical quantities of the GC clouds, such as fractional abundance of HCN isotopes and mass of the GC cloud complexes. We confirm that the GC has very rich chemistry. The overall fractional abundance of $H^{12}CN$ and $H^{13}CN$ relative to $H_2$ in the GC region is found to be significantly higher than those of any other regions, such as star forming region and dark cloud. Especially cloud complexes nearer to the GC tend to have various higher abundance of HCN. Total mass of the HCN molecular clouds within $[{\iota}]{\le}6^{\circ}$ is estimated to be ${\~}2 {\times}10^7\;M_{\bigodot}$ using the abundances of HCN isotopes, which is fairly consistent with previous other estimates. Masses of four main complexes in the GC range from a few $10^5$ to ${\~}10^7\;M_{\bigodot}$ All the HCN spectra with multi-components for the four main cloud complexes were investigated to compare the line widths of the complexes. The largest mode (45 km $s^{-1}$) of the FWHM distributions among the complexes is in the Clump 2. The value of the mode tends to be smaller at the farther complexes from the GC.

• 천문학논총
• /
• 제11권1호
• /
• pp.75-90
• /
• 1996

The vertical distribution of HCN, $HC_3N$ and $C_2N_2$ have been determined from a sequence of Voyager 1 IRIS limb tangent measurements over Titan's north polar region. This sequence yields gas distributions with ${\sim}200\;km$ altitude resolution over the 50-400 km range. The derived mixing ratios of HCN, $HC_3N$ and $C_2N_2$ are $5{\times}10^{-7}$, $7{\times}10^{-8}$ and $8{\times}10^{-9}$, respectively, at 120 km with a factor of 3 uncertainty.

• 한국화재소방학회논문지
• /
• 제12권2호
• /
• pp.43-59
• /
• 1998

화재위험성이 큰 유흥업소에서 주로 사용하는 내장재중 방염 카퍼l트, 방영 후처리 합환, 쇼파 례자동 3가지 시료에 대한 연소특성과 CO, CO2, 02, NO., S02, HCN, HCl둥 독성가스를 검출하여 화재 위험 성을 비교명가 하였다. 연소특성에 있어 방염 카페트가 방염 후처리 합판, 쇼파 레자 보다 연소가 잘 되 었고, 폭연 연소가 일어났다. 모든 시료에서 CO의 발생은 연소시작 후 1분 이내에 치사농도를 상회(上 ) 하였으나 NOx와 S02는 치사농도를 상회(上 ) 하지 않았지만. HCN는 카페트에서 쇼파 레자 보 다 20.6배, 방염 후처리 합판 보다 4.6배가 검출 되었고. HCl은 차페트에서 쇼파 례자 보다 4.48배, 방 염 후처리 합판 보다 2.47배가 검출 되었다. 이상과 같이 3종의 내장재중 방염 차페트가 화재위험성이 가장 높다는 결론을 얻을 수 있었다.

• 한국화재소방학회논문지
• /
• 제32권5호
• /
• pp.52-56
• /
• 2018

화재로 인한 피해는 열상에 의한 피해보다는 연소 독성에 의한 피해가 치명적이며, 인명피해를 줄이기 위해 화재 상황에서 젖은 수건을 사용하여 화재로부터 발생되는 독성가스를 방호하도록 권장하고 있다. 본 연구에서는 젖은 수건을 통해 실제 화재에서 발생되는 가스를 대상으로 필터링 효과를 정량화하였다. 화재가스 중 세 가지 가스($CO_2$, HCl, HCN)를 대상으로 젖은 수건의 필터효과를 확인하기 위해 FT-IR을 이용하여 필터를 통과한 가스를 실시간 분석을 하였으며, 물에 잘 녹지 않는 $CO_2$에 비해 유독가스이며, 수용성 가스인 HCl, HCN은 젖은 수건에 의해 가스가 필터링 되면서 가스 검출 시점이 지연됨을 확인하였다. 따라서 실제 화재 시 독성가스 중 특히 수용성 가스의 경우 젖은 수건을 이용하게 되면 일정 시간 피난 시간을 확보할 수 있음을 확인하였다.

• 천문학논총
• /
• 제30권2호
• /
• pp.439-442
• /
• 2015

We observed multiple CO transition lines and the HCN(1-0) line at ~ 1" (~ 34 pc) or higher resolution toward the Seyfert 2 nucleus of M51 using the IRAM Plateau de Bure Interferometer (PdBI) and the Submillimeter Array (SMA). All the images show very similar overall molecular gas distribution; there are two discrete clouds at the eastern and western sides of the nucleus, and the western cloud exhibits an elongated distribution and velocity gradient along the radio jet. In addition, high HCN(1-0)/CO(1-0) brightness temperature ratios of about unity have been observed, especially along the radio jet, similar to those observed in shocked molecular gas in our Galaxy. This strongly indicates that the molecular gas along the jet is shocked, that the radio jet and the molecular gas are interacting, and the jet is entraining both diffuse (CO) and dense (HCN) molecular gas outwards from the circumnuclear region. This is the first clear imaging of the outflowing molecular gas entrained by the AGN jet, and showing the detailed physical status of outflowing molecular gas. Since a relatively high HCN(1-0)/CO(1-0) ratio has been observed in the high velocity wing of ultraluminous infrared galaxies, it can also be explained by a similar mechanism to those we describe here.