• 천문학회지
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• 제51권1호
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• pp.17-25
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• 2018

Detecting exoplanets around giant stars sheds light on the later-stage evolution of planetary systems. We observed the M giant HD 18438 and the K giant HD 158996 as part of a Search for Exoplanets around Northern circumpolar Stars (SENS) and obtained 38 and 24 spectra from 2010 to 2017 using the high-resolution Bohyunsan Observatory Echelle Spectrograph (BOES) at the 1.8m telescope of Bohyunsan Optical Astronomy Observatory in Korea. We obtained precise RV measurements from the spectra and found long-period radial velocity (RV) variations with period 719.0 days for HD 18438 and 820.2 days for HD 158996. We checked the chromospheric activities using Ca $\text\tiny{II}$ H and $H{\alpha}$ lines, HIPPARCOS photometry and line bisectors to identify the origin of the observed RV variations. In the case of HD 18438, we conclude that the observed RV variations with period 719.0 days are likely to be caused by the pulsations because the periods of HIPPARCOS photometric and $H{\alpha}$ EW variations for HD 18438 are similar to that of RV variations in Lomb-Scargle periodogram, and there are no correlations between bisectors and RV measurements. In the case of HD 158996, on the other hand, we did not find any similarity in the respective periodograms nor any correlation between RV variations and line bisector variations. In addition, the probability that the real rotational period can be as longer than the RV period for HD 158996 is only about 4.3%. Thus we conclude that observed RV variations with a period of 820.2 days of HD 158996 are caused by a planetary companion, which has the minimum mass of 14.0 $M_{Jup}$, the semi-major axis of 2.1 AU, and eccentricity of 0.13 assuming the stellar mass of $1.8 M_{\odot}$. HD 158996 is so far one of the brightest and largest stars to harbor an exoplanet candidate.

• KSBB Journal
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• 제11권3호
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• pp.295-302
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• 1996

Rubisco의 parameter들을 측정하는 것은 광합성 연구에 대단히 중요한데, 본 연구에서는 방사성통위 원소를 사용하는 방법 이 아닌 photometric assay 방 법을 사용하여 parameter를 측정하였다. Rubisco 의 activation과 carbamylation에 미치는 고 CO2 놓도의 효과를 연구하기 위하여, 정상 $CO_2$ 농도 (350 ppm)와 고 $CO_2$ 농도(650 ppm)에서 기른 kidney bean (Phaseolus vulgaris L.) 잎을 각각 재료로 하여, dual beam(334 nm9-} 405 nm) spectro­p photometer를 사용하여 rubisco의 initial activity 와 total activity, carbamylation rate 및 量을 측정 비교하였으며, SDS-PAGE에 의해 rubisco의 전기 영통 profile을 분석하였다. 정상 $CO_2$ 농도에서의 initial activity와 total activity는 $41.2{\mu}M/m^2/s 와 52.2{\mu}M/m^2/s$이며, 고 $CO_2$ 농도에서는 $27.4{\mu}M/m^2/s 와 46.1{\mu}M/m^2/s$로서, 350 ppm에서 650 ppm으로 $CO_2$ 농도를 증가시키면 rubisco의 initial activity와 total activity가 갑소되었다. 또한 carbamylation율도 정상 $CO_2$ 농도에서는 79%이며, 고 $CO_2$ 농도에서는 58.9%로서, $CO_2$ 농도의 증가에 따라 감소되 었다. Rubisco 의 量은 정상 $CO_2$농도에서는 $1.94 {\mu}M/m^2$$ 임에 반해 고 $CO_2$ 농도에서는 $1.58{\mu}M/m^2$ 로서, $CO_2$2 농도는 증가되었는데 그 量은 감소되었다. 이와 같이 고 $CO_2$농도에셔 rubisco의 activity가 감소되는 것은 rubisco의 carbamylation에 기인되는 것으로 생각된다. SOS-PAGE 분석에서 50kO 분자량의 large s subunit와 14.5 kO의 분자량을 가지는 small subu n mt를 동정하였는데, 고 $CO_2$ 농도와 정상 $CO_2$ 농도 의 50kD와 14.5 kO band의 intensity를 비교하면 두 구 사이에 큰 차이가 발견되지 않았다. 고 CO2 농도에서 정상 $CO_2$ 농도로 switch한 rubisco의 parameter는 정상 $CO_2$ 농도에서의 pa­r rameter와 거의 비슷한 값을 나타내였는데, 이는 350 ppm의 정상 $CO_2$ 농도에 의해 rubisco의 acti­v vity가 회복되었음을 의미한다.

• Archives of Plastic Surgery
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• 제40권5호
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• pp.610-615
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• 2013

Background Cephalometric analysis is essential for planning treatment in maxillofacial and aesthetic facial surgery. Although photometric analysis of the Korean nose has been attempted in the past, anthropometry of the deeper nasal structures in the same population based on computerized tomography (CT) has not been published. We therefore measured three anthropometric parameters of the nose on CT scans in our clinical series of patients. Methods We conducted the current retrospective study of a total of 100 patients (n=100) who underwent a CT-guided radiological measurement at our institution during a period ranging from January of 2008 to August of 2010. In these patients, we took three anthropometric measurements: the nasofrontal angle, the pyramidal angle, and the linear distance between the nasion and the tip of the nasal bone. Results The mean nasofrontal angle was $131.14^{\circ}$ in the male patients and $140.70^{\circ}$ in the female patients. The mean linear distance between the nasion and the tip of the nasal bone was 21.28 mm and 18.02 mm, respectively. The mean nasal pyramidal angle was $112.89^{\circ}$ and $103.25^{\circ}$ at the level of the nasal root, $117.49^{\circ}$ and $115.60^{\circ}$ at the middle level of the nasal bone, and $127.99^{\circ}$ and $125.04^{\circ}$ at the level of the tip of the nasal bone, respectively. Conclusions In conclusion, our data will be helpful in the preparation of silicone implants for augmentation and/or corrective rhinoplasty in ethnic Korean people.

• 천문학논총
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• 제30권2호
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• pp.665-669
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• 2015

The Kepler mission has shown that small planets are extremely common. It is likely that nearly every star in the sky hosts at least one rocky planet. We just need to look hard enough-but this requires vast amounts of telescope time. MINERVA (MINiature Exoplanet Radial Velocity Array) is a dedicated exoplanet observatory with the primary goal of discovering rocky, Earth-like planets orbiting in the habitable zone of bright, nearby stars. The MINERVA team is a collaboration among UNSW Australia, Harvard-Smithsonian Center for Astrophysics, Penn State University, University of Montana, and the California Institute of Technology. The four-telescope MINERVA array will be sited at the F.L. Whipple Observatory on Mt Hopkins in Arizona, USA. Full science operations will begin in mid-2015 with all four telescopes and a stabilised spectrograph capable of high-precision Doppler velocity measurements. We will observe ~100 of the nearest, brightest, Sun-like stars every night for at least five years. Detailed simulations of the target list and survey strategy lead us to expect $15{\pm}4$ new low-mass planets.