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강영운,안지은,서정혁,박선희,윤혜정 한국식품위생안전성학회 2014 한국식품위생안전성학회지 Vol.29 No.4
The present study demonstrated the development and validation of the method for the quantificationof phenol in food using gas chromatography coupled with mass spectrometry (GC-MS). After spiking of interanlstandard (Phenol-d5) to food, those samples were extracted with organic solvent mixture (acetone : dichloromethane= 1 : 1, v/v) using ultra sonic extractor and cleaned by gel permeation chromatography (GPC) technique. The amountof phenol was determined by GC/MS. To validate the developed method, we evaluated parameters were the selectivity,linearity, accuracy, precision, and recovery. To demonstrate the selectivity of the method, blank samples of rice,corn, and fish(mackerel) were prepared and subjected to GC-MS analysis. To verify the linearity of the method, sixdifferent standard concentrations of phenol at 0.01, 0.05, 0.1, 0.5, 1 and 2.5 mg/kg were evaluated. The correlationcoefficient (r2) of calibration curve was 0.9999. The recovery rate for phenol standard calculated by internal standardmethod were 82.2~101.5% for samples fortified with 0.25, 0.50, and 1.0 mg/kg, respectively. Also the repeatabilityand reproducibility for validation of precision were 0.2~5.5%. According to the result of the validation, this establishedmethod was suitable for AOAC guideline. The limit of detection (LOD) for phenol analysis were 0.03~0.1 mg/kg, and the limit of quantification (LOQ) were 0.1~0.3 mg/kg. Therefore, we established the optimal analysis methodfor determination of phenol in food using GPC and GC/MS.
강영운,김호일,이우백,오규동,KANG YOUNG WOON,KIM HOIL,LEE WOO BAIK,OH KYU DONG 한국천문학회 2000 天文學論叢 Vol.15 No.suppl1
We have reviewed the magnetic activity in close binaries. Solar like magnetic activity indicators such as photometric spots, chromo spheric emission, coronal X-ray and radio emission, and flare activity are commonplace in many cool stars with convective envelopes. Using the UV spectra we confirmed the strength of stellar activity increases with more rapid rotation and later spectral types which corresponds to the increasing depth of the star's convective envelope. Apart from very young stellar objects such as T Tauri stars, the stars with the highest levels of activity are close binary systems composed of cool stars, i.e., the chromospherically active binaries such as RS CVn, BY Dra, W UMa and related systems. The IUE low and high dispersion spectra of V711 Tau, VW Cep and SW Lac are used for ultraviolet photometry and for a variation study of chromospheric activity. Evidence of chromospherically activity is indicated by the intensity variation of the Mg II emission line with orbital phase.
강영운,김호일,이우백,오규동 한국천문학회 2000 天文學論叢 Vol.15 No.2
We have reviewed the magnetic activity in close binaries. Solar like magnetic activity indicators such as photometric spots, chromo spheric emission, coronal X-ray and radio emission, and flare activity are commonplace in many cool stars with convective envelopes. Using the UV spectra we confirmed the strength of stellar activity increases with more rapid rotation and later spectral types which corresponds to the increasing depth of the star's convective envelope. Apart from very young stellar objects such as T Tauri stars, the stars with the highest levels of activity are close binary systems composed of cool stars, i.e., the chromospherically active binaries such as RS CVn, BY Dra, W UMa and related systems. The IUE low and high dispersion spectra of V711 Tau, VW Cep and SW Lac are used for ultraviolet photometry and for a variation study of chromospheric activity. Evidence of chromospherically activity is indicated by the intensity variation of the Mg II emission line with orbital phase.
Asymmetric Light curves of Contact and Near-Contact Binaries
강영운,Rittipruk, Pakakaew,Kang, Young-Woon 한국천문학회 2012 天文學會報 Vol.37 No.2
We attempt to investigate the main reason of the asymmetrical light curves of contact and near-contact eclipsing binary base on the hypothesis that cool spot was produced on late type star while hot spot was produced from transferred material from their companion star hitting surface. We select 7 eclipsing binary systems which showed asymmetric light curves and mass transfer. Period variation and mass transfer rate were obtained from O-C diagram. Radial velocity curves and light curves of those 7 eclipsing binary system were adopted from available literature in order to obtain the absolute dimension. For four contact eclipsing binary system (AD Phe, EZ Hya, AG Vir and VW Boo), their component stars belonged to spectral type G to K was fitted by cool spot model. While the other two near-contact systems (RT Scl and V1010 Oph) and one contact system (SV Cen) was fitted by cool spot model. The densities of the materials are adopted from stellar model which calculate by stellar structure code. The calculated spot temperature turns out to agree with the photometric solution but there are no correlate between period variation rate and type of spot.