• Horticulture, Environment, and Biotechnology : HEB
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• 제59권6호
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• pp.827-833
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• 2018

Plasma lighting systems have been engineered to simulate sunlight. The objective of this study was to determine the effects of plasma lighting on tomato plant growth, photosynthetic characteristics, flowering rate, and physiological disorders. Tomato plants were grown in growth chambers at air temperatures of $25/23^{\circ}C$ (light/dark period), in a $16h\;day^{-1}$ light period provided by four different light sources: 1 kW and 700 W sulfur plasma lights (1 SPL and 0.7 SPL), 1 kW indium bromide plasma light, and 700 W high pressure sodium lamp (0.7 HPS) as a control. The totaldry weight and leaf area at 0.7 SPL were approximately 1.2 and 1.3 times greater, respectively, than that of 0.7 HPS at the 62 days after sowing (DAS). The maximum light assimilation rate was observed at 1 SPL at the 73 DAS. In addition, the light compensation and saturation points of the plants treated with plasma lighting were 98.5% higher compared with HPS. Those differences appeared to be related to more efficient light interception, provided by the SPL spectrum. The percentage of flowering at 0.7 SPL was 30.5%, which was higher than that at 0.7 HPS; however, there were some instances of severe blossom end rot. Results indicate that plasma lighting promotes tomato growth, flowering, and photosynthesis. Therefore, a plasma lighting system may be a valuable supplemental light source in a greenhouse or plant factory.

• Journal of Radiation Protection and Research
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• 제43권3호
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• pp.114-119
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• 2018

Background: The retrospective dosimetry using RTL quartz can be improved by information for an optical sensitivity of sample connected with the equivalent dose determination. Materials and Methods: The quartz sample from a volcanic rock of Japan was used. After correcting the thermal quenching effect, RTL peaks of quartz were separated by the CGCD method cooperated with the general order kinetics. The number of overlapped glow peaks were ascertained by the $T_m-T_{stop}$ method. The optical sensitivity was examined by comparing the change of intensity on RTL glow peaks measured after exposure to light from a solar simulator with various illumination times. Results and Discussion: Seven glow peaks appeared to be overlapped on the RTL glow curve. The general order kinetics model was appropriate to separate glow peaks. After exposure to light from a solar simulator from a few minutes to 416 hr, the signals for peaks P4 and P5 decayed following the form of $f(t)=a_1e^{-{\lambda}1t}$, while the signals for peaks P6 and P7 decayed by the form of $f(t) = a_1e^{-{\lambda}1t}+a_2e^{-{\lambda}2t}+a_3e^{-{\lambda}3t}$. Conclusion: For dosimetric peaks, the times taken to reduce the RTL signal to half of its initial value were 70 sec for the peak P4, 54 s for the peak P5, 9,840 sec for the peak P6 and 26,580 sec for the peak P7, respectively. We conclude that the optical sensitivity of peaks P4, and P5 gives much higher than that of peaks P6 and P7.

• 한국식품위생안전성학회지
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• 제23권2호
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• pp.121-128
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• 2008

본 연구는 Lightcycler (Roche)를 이용한 Real-Time PCR(LC-PCR)기법을 통하여 원유시료에서 신속, 정확하게 황색포도상구균을 검출하는 기법을 개발하고자 하였다. coagulase 전구체를 coding하는 113 bp의 coa 유전자의 증폭, melting curve 분석 및 DNA염기서열을 분석하여 황색포도상구균 특유의 유전자 검출하는 기법을 개발하였다. 또한 분리된 균주중 메치실린에 내성을 나타내는 균주를 검출하고자 penicillin-binding protein, PBP2a (mecA)를 coding 하는 209 bp의 mecA 유전자의 증폭, melting curve 분석 및 DNA염기서열을 분석하여 메치실린내성 황색 포도상구균을 real-time PCR 기법으로 검출하는 기술을 개발하였다. 본 실험에 따르면 647개의 원유시료중 6개의 시료에서 황색포도상구균이 검출되었으며 이중 2개의 시료에서 분리된 황생포도상구균이 메치실린내성 황색포도상구균임을 확인하였다. 또한 DNA 검출한계는 10 fg으로 기존 PCR에 비해 매우 감도가 우수한 것을 확인하였다. 또한 3개의 원유시료에서 돼지나 소의 삼출성 피부염의 원인균인 Staphylococcus chromogenes가 분리되었다.

• ALGAE
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• 제19권3호
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• pp.207-216
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• 2004

Characteristics of photosynthesis-light and photosynthesis-temperature relationships were seasonally compared among 4 species, two temperate Sargassurn (S. ringgoldianum and S. spathulophyllum) and two temperate kelp (Ecklonia cava and Eisenia bicyclis), growing in the same habitat in Oura Bay, Shimoda, central Japan. The photosynthesis-irradiance (P-I) curve of each species at the in situ temperature and the photosynthesis-temperature (P-T) curve at near saturation irradiance (400μmol·m^(-2)·s^(-1)) were determined by using differential gas-volumeters. Maximum photosynthetic rates (Prnax) for P-I curves of the two Sargassurn species were higher from summer to autumn than from winter to spring, while those of the two kelp species showed little difference among seasons. Net photosynthetic rates (Pn) at 100-400μmol·m^(-2)·s^(-1) of the Sargassurn species were higher than those of the kelp species in autumn, spring and summer, while in winter the rates were about the same between the Sargassurn and kelp species. Among seasons, the light saturation index (1k) values, dark respiration rates and light compensation points of Sargassurn species differed more than those of kelp species. Optimum temperature for P-T curves of Sargassurn species was 29℃ and that of kelp species was 27℃ in summer, while in winter the former was 27℃ and the latter was 25℃. Pn at 400 μmol·m^(-2)·s^(-1) at 10-33℃ of Sargassurn species were considerably higher than those of kelp species from spring to summer, while from autumn to winter the rates at 5-27℃ were about the same between the two. At supra-optimum temperatures, Pn of kelp species decreased more sharply than those of Sargassurn species in each season. These facts indicate that the two temperate Sargassurn species have a higher potential photosynthetic performance under warmer conditions than the two temperate kelp species even though they grow in the same habitat.

• 천문학회보
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• 제37권1호
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• pp.32.2-32.2
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• 2012

Gamma Ray Bursts (GRBs) are the most energetic events in the universe, and are known to arise from the death of massive stars in many cases. Their extreme brightness makes it possible to detect them at very high redshift (z > 6.5), well into the epoch of re-ionization, providing us with an opportunity to investigate the deaths of the first stars when the universe was much younger than 1 Gyr. Here, we report the discovery of GRB 100905A, a GRB at $z$ - 7.5 (age of the universe at 700 Myr). Our observation revealed a strong spectral break between z and J band, allowing us to estimate its photometric redshift. Its gamma-ray light curve shows a very short duration of about 0.7 sec, the shortest duration event at z > 5. Investigation of this and three other known GRBs at z > 6.5 reveals that they are all short duration bursts. This is puzzling, considering that GRBs from death of massive stars do not show short duration. We suggest two possible explanations for this: (i) the BAT light curves of the high redshift GRBs suffered from observational selection effect where we are only observing the very tip of the light curve; (ii) the stars in the early universe had a peculiar nature that are different from ordinary stars at lower redshifts.

• 천문학회보
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• 제35권1호
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• pp.48.1-48.1
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• 2010

Four of nine exoplanets found by microlensing were detected by the resonant caustic, which represents the merging of the planetary and central caustics at the position when the projected separation of a host star and a bounded planet is s~1. One of the resonant caustic lensing events, OGLE-2005-BLG-169, was a caustic-crossing high-magnification event with A_max ~800 and the source star was much smaller than the caustic, nevertheless the perturbation was not obviously apparent on the light curve of the event. In this paper, we investigate the perturbation pattern of the resonant caustic to understand why the perturbations induced by the caustic do not leave strong traces on the light curves of high-magnification events despite a small source/caustic size ratio. From this study, we find that the regions with small magnification excess around the center of the resonant caustic are rather widely formed, and the event passing the small-excess region produces a high-magnification event with a weak perturbation that is small relative to the amplification caused by the star and thus does not noticeably appear on the light curve of the event. We also find that the positive excess of the inside edge of the resonant caustic and the negative excess inside the caustic become stronger and wider as q increases, and thus the resonant caustic-crossing high-magnification events with the weak perturbation occur in the range of q $\leq$ 10-4. We determine the probability of the occurrence of events with the small excess $|\varepsilon|{\leq}3%$ in high-magnification events induced by a resonant caustic. As a result, we find that for the Earth-mass planets with a separation of ~2.5 AU the resonant caustic high-magnification events with the weak perturbation can occur with a significant frequen.

• 천문학회보
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• 제41권1호
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• pp.41.1-41.1
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• 2016

We present the physical properties of KIC 6220497 exhibiting multiperiodic pulsations from the Kepler photometry. The light curve synthesis represents that the eclipsing system is a semi-detached Algol with a mass ratio of q=0.243, an orbital inclination of i=77.3 deg, and a temperature difference of ${\Delta}T=3,372K$, in which the detached primary component fills its Roche lobe by ~87% and is about 1.6 times larger than the lobe-filling secondary. To detect reliable pulsation frequencies, we analyzed separately the Kepler light curve at the interval of an orbital period. Multiple frequency analyses of the eclipse-subtracted light residuals reveal 32 frequencies in the range of $0.75-20.22d^{-1}$ with semi-amplitudes between 0.27 and 4.55 mmag. Among these, four frequencies ($f_1$, $f_2$, $f_5$, $f_7$) may be attributed to pulsation modes, while the other frequencies can be harmonic and combination terms. The pulsation constants of 0.16-0.33 d and the period ratios of $P_{pul}/P_{orb}=0.042-0.089$ indicate that the primary component is a ${\delta}$ Sct pulsating star in p modes and, thus, KIC 6220497 is an oscillating eclipsing Algol (oEA) star. The dominant pulsation period of about 0.1174 d is considerably longer than the values given by the empirical relations between the pulsational and orbital periods. The surface gravity of log $g_1=3.78$ is significantly smaller than those of the other oEA stars with similar orbital periods. The pulsation period and the surface gravity of the pulsating primary demonstrate that KIC 6220497 would be the more evolved EB, compared with normal oEA stars.

• Journal of Astronomy and Space Sciences
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• 제23권4호
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• pp.319-326
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• 2006

한국천문연구원의 NEOPAT 팀과 연세대학교 천문대의 YSTAR 팀이 공동으로 호주 Siding Spring 천문대에 설치한 광시야 자동망원경 2호기를 이용하여 W UMa형 식쌍성 BL Eri의 측광관측을 수행하였다. 이 망원경을 이용하여, 호주와 한국에서 각각 자동관측 모드 및 원격관측 모드로 6일 밤을 관측하여, 새로운 VRI CCD광도곡선과, 5개의 새로운 극심시각을 얻었다. Wilson & Deviney(1971)의 쌍성모델 2005 버전을 이용하여 우리의 광도곡선을 분석하고, 새로운 광도곡선 해를 구하였다. 이 과정에서 우리가 구한 질량비 0.48은 이전의 연구자들이 구한 값과 차이를 보이고 있다. 한편 이 방성계의 접촉상태를 Wilson & Deviney모델을 적용하여 확인한 결과, 현재 BL Eri는 접촉상태에 있는 것으로 보인다.

• Journal of Astronomy and Space Sciences
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• 제26권3호
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• pp.295-304
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• 2009

대마젤란은하 중심부에 위치한 식쌍성 EROS 1010에 대한 CCD 측광관측을 2006년과 2007년에 수행하여 BV 광도곡선을 완성하였다. BV 광도곡선은 EROS팀과 OGLE팀이 각각 관측한 BR과 I 광도곡선과 함께 Wilson & Devinney 차등보정법으로 분석하여 측광학적인 해를 제시하였다. 한편 대마젤란은하의 거리지수를 $m-M=18.^m3{\sim}18.^m5$ 사이로 가정하고, EROS 1010에 대한 절대량을 구하였다.

• 천문학회지
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• 제44권3호
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• pp.97-108
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• 2011

The photometric light curves of the W-type W UMa eclipsing contact binary system BB Pegasi have been found to be extremely asymmetric over all the observed 63 years in all wavelengths UBVR. The light curves have been characterized by occultation primary minima. Hence, the morphology of these light curves has been studied in view of these different asymmetric degrees. The system shows a distinct O'Connell effect, as well as depth variation. A 22.96 years of stellar dark spots cycle has been determined for the system. Almost the same cycle (22.78 yr) has been found for the depth variation of MinI and MinII. We also present an analysis of mid-eclipse time measurements of BB Peg. The analysis indicates a period decrement of $5.62{\times}10^{-8}$ day/yr, which can be interpreted in terms of mass transfer at a rate of $-4.38{\times}10^{-8}M_{\odot}$/yr, from the more to the less massive component. The O - C diagram shows a damping sine wave covering two different cycles of 17.0 yr and 12.87 yr with amplitudes equal to 0.0071 and 0.0013 day, respectively. These unequal durations show a non-periodicity which may be explained as a result of magnetic activity cycling variations due to star spots. The obtained characteristics are consistent with similar chromospherically active stars, when applying the Applegate's (1992) mechanism.