• 천문학논총
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• 제30권2호
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• pp.241-245
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• 2015

In this work we present the results of light curve analysis for two cataclysmic variables detected recently in the SDSS project: SDSS J090350.73+330036.1 and J150240.98+333423.9. Photometric observations of the first were obtained during a superoutburst in May 2010. Our observations clearly indicate the presence of superhumps in the light curves, suggesting SDSS J090350.73+330036.1 is an SU UMa dwarf nova. We determined the period of the superhumps. We also carried out fitting using a spiral-arm model in order to determine parameters of the accretion disk, hot line, and other components of this system. Photometric observations of the second, J150240.98+333423.9, were obtained during the post-maximum decline, during April-June 2012. Photometric variability of this system has been studied in an inactive state. We obtained its parameters via a combined model fitted to the observed light curves by ${\chi}^2$ minimization.

• The Plant Pathology Journal
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• 제39권6호
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• pp.538-547
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• 2023

Rapid apple decline (RAD) is a complex phenomenon affecting cultivated apple trees and particularly dwarf rootstocks on grafted young apple trees. Since its first appearance in the United States, RAD has been reported worldwide, for example in Canada, South America, Africa, and Asia. The phenomenon has also been observed in apple orchards in Korea, and it presented similar symptoms regardless of apple cultivar and cultivation period. Most previous reports have suggested that RAD may be associated with multiple factors, including plant pathogenic infections, abiotic stresses, environmental conditions, and the susceptibility of trees to cold injury during winter. However, RAD was observed to be more severe and affect more frequently apple trees on the Malling series dwarf rootstock. In this study, we reviewed the current status of RAD worldwide and surveyed biotic and abiotic factors that are potentially closely related to it in Korea.

• 한국산림과학회지
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• 제100권4호
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• pp.623-629
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• 2011

파이토플라스마에 감염된 뽕나무의 각 부위를 nested-PCR법과 경쟁 PCR법을 이용하여 파이토플라스마의 검출 범위 및 밀도 변화를 조사하였다. 파이토플라스마에 부분 감염된 뽕나무를 총 5부위(A. 빗자루병이나 오갈병 증상을 보인 잎의 엽병, B. 병징을 보인 잎이 있는 가지의 아래쪽 건전해 보이는 잎의 엽병, C. 병징을 보인 잎의 가지 부위, D. 병징을 보이지 않은 가지 쪽의 영병이나 가지, E. 잔뿌리)로 구분하였다. AS-1/AS-2 프라이머를 이용한 nested-PCR 결과, 파이토플라스마는 모든 시료에서 검출되었으며, 파이토플라스마의 검출범위는 P1/P7 프라이머를 이용한 direct-PCR 산물에서는 희석액이 $10^4$배까지 검출되었고, AS-1/AS-2 프라이머를 이용하여 nested-PCR를 수행한 결과, PCR 산물을 $10^{13}$배 희석한 시료까지 파이토플라스마가 검출되었다. 경쟁 PCR 결과, 뽕나무 파이토플라스마의 밀도는 $7.94{\times}10^{18}-10^{12}copies/{\mu}L$의 범위내에 존재하였으며, 년 중 파이토플라스마가 모든 시료에서 존재하였다. 초기생장시기에는 "B"부위와 "C"부위에서 파이토플라스마 밀도가 높게 나타났으나 "A"부위와 "D"부위에서는 이보다 낮게 나타났다. 휴면기에는 "C"부위와 "E"부위가 "D"부위보다 밀도가 높았다. 모든 시료 중 "C"부위와 "A"부위에서 년 중 파이토플라스마 밀도가 안전적으로 존재하였다. 본 연구 결과, nested-PCR 법과 경쟁 PCR법은 식물체내의 파이토플라스마의 정확한 검출과 밀도변화를 알아볼 수 있는 유용한 방법이다.

• 고려인삼학회:학술대회논문집
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• 고려인삼학회 1988년도 학술대회지
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• pp.141-146
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• 1988

북미가 원산지인 왜생삼(Panax trifolius L.)은 인삼속(오가과)에 속하며 카나다 남부에서 북미에 걸쳐 서식한다. 왜생삼 잎에서 4종류의 프라보느이드와 5종류의 진세노사이드로 확인된 총 9종류의 화합물을 분리하였다. 2종류의 진세노사이드로 확인된 총 9종류의 화합물을 분리하였다. 2종류의 프라보노이드는 kaempferol-3,7-dirhamnoside와 kaempferol-3-gluco-7rhamnoside로 각각 확인되었다. 4종류의 진세노사이드는 각각 notoginsenoside-Fe, ginsenoside-Rd, ginsenoside-Rc와 ginsenoside-$Rb_3$로 확인되었으며, 이들 왜생삼의 ginsenoside 공통된 골격구조는 (20S)-protopanaxadiol인 것으로 밝혀졌다. 프라보노이드와 진세노사드의 동정은 왜생삼의 뿌리, 줄기, 잎, 꽃과 열매에서 추출하여 2차원 박층 그로마토그라피(2D-TLC)와 고압 액체크로마토그라피(HPLC)로 하였다. 왜생삼과 근연종인 고려인삼(Panax ginseng C.A. Meyer)및 미국삼(Panx quinquefolium L.)의 뿌리, 줄기, 잎, 꽃과 열매에서 추출한 프라보노이드와 진세노시드의 정량은 고압 액체크로마토그래피 만을 사용하여 분석하였다. 화합물 1,3과 4로 명명한 kaempferol 유도체인 프라보노이드 3가지는 왜생삼의 뿌리에 $10.8\%,\;2.8\%$와 $8.4\%$가 각기 함유되어 있었으나 고려인삼과 미국삼에서는 함유되어 있지 않았다. 오가과 인삼속식물 뿌리에서 프라보노이드가 확인, 동정된 것은 이것이 처음이다.

• 천문학회보
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• 제37권2호
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• pp.81-81
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• 2012

Since the ultraviolet (UV) flux of an integrated population is a good tracer of recent star formation activities, UV observations provide an important constraint on star formation history (SFH) in galaxies. We present UV color-magnitude relations (CMRs) of early-type dwarf galaxies in the Virgo cluster, based on Galaxy Evolution Explorer (GALEX) UV data and the Extended Virgo Cluster Catalog (EVCC, Kim, S. in prep.). The EVCC covers an area 5.4 times larger (750 deg2) than the footprint of the classical Virgo cluster catalog by Binggeli and collaborators. We secure 1304 galaxies as members of the Virgo cluster and 526 galaxies of them are new objects not contained in the VCC. Morphological classification of galaxies in the EVCC is based on the optical image ("Primary Classification") and spectral feature ("Secondary Classification") of the SDSS data. We find that dwarf lenticular galaxies (dS0s) show a surprisingly distinct and tight locus separated from that of ordinary dwarf elliptical galaxies (dEs), which is not clearly seen in previous CMRs. The dS0s in UV CMRs follow a steeper sequence than dEs and show bluer UV-optical color at a given magnitude. Most early type dwarf galaxies with blue UV colors (FUV-r < 6 and NUV-r < 4) are identified as those showing spectroscopic hints of recent or ongoing star formation activities. We explore the observed CMRs with population models of a luminosity-dependent delayed exponential star formation history. The observed CMR of dS0s is well matched with models with relatively long delayed star formation. Our results suggest that dS0s are most likely transitional objects at the stage of subsequent transformation of late-type progenitors to ordinary red dEs in the cluster environment. In any case, UV photometry provides a powerful tool to disentangle the diverse subpopulations of early-type dwarf galaxies and uncover their evolutionary histories.

• 천문학회보
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• 제40권1호
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• pp.57.2-57.2
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• 2015

We have proposed a deep observing program to survey more than 3,000 sq. degree of southern sky with the KMTNet telescopes to search for ultra-faint dwarf galaxies. Recently, the test observations for our survey were made in B, V, R, I-band. We will report the performance of the KMTNet camera system and our detailed strategy in both of observations and analysis for the three-year survey.

• Journal of Astronomy and Space Sciences
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• 제29권2호
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• pp.175-180
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• 2012

White dwarf stars have played important roles in rather diverse areas of astrophysics. This paper outlines how these stellar remnants, especially those in widely separated "fragile" binaries, have provided unique leverage on difficult astrophysical problems such as the ages of stars, the structure and evolution of the Galaxy, the nature of dark matter and even the discovery of dark energy.

• 천문학논총
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• 제8권1호
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• pp.163-168
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• 1993

At intermediate mass transfer rates, accretion disks in binary star systems undergo a thermally-driven limit cycle instability. This instability leads to outburst episodes when the disk is bright and the flow through the disk is rapid separated by long intervals when the disk is dim and the flow through it is low. This intrinsic outburst mechanism can help to understand a wide range of astrophysical phenomena from dwarf novae to soft X -ray transients involving white dwarf, neutron star, and black holes. and to a deeper understanding of the mechanism of angular transport and viscosity in the accretion disk.

• 천문학회보
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• 제42권2호
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• pp.39.3-40
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• 2017

Ultra-diffuse galaxies (UDGs) are an unusual galaxy population. They are ghostlike galaxies with fainter surface brightness than normal dwarf galaxies, but they are as large as MW-like galaxies. The key question on UDGs is whether they are 'failed' giant galaxies or 'extended' dwarf galaxies. To answer this question, we study UDGs in massive galaxy clusters. We find an amount of UDGs in deep HST images of three Hubble Frontier Fields clusters, Abell 2744 (z=0.308), Abell S1063 (z=0.347), and Abell 370 (z=0.374). These clusters are the farthest and most massive galaxy clusters in which UDGs have been discovered until now. The color-magnitude relations show that most UDGs have old stellar population with red colors, while a few of them show bluer colors implying the existence of young stars. The stellar masses of UDGs show that they have less massive stellar components than the bright red sequence galaxies. The radial number density profiles of UDGs exhibit a drop in the central region of clusters, suggesting some of them were disrupted by strong gravitational potential. Their spatial distributions are not homogeneous, which implies UDGs are not virialized enough in the clusters. With virial masses of UDGs estimated from the fundamental manifold, most UDGs have M_200 = 10^10 - 10^11 M_Sun indicating that they are dwarf galaxies. However, a few of UDGs more massive than 10^11 M_Sun indicate that they are close to failed giant galaxies.

• 천문학회지
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• 제41권5호
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• pp.121-137
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• 2008

We present optical and near-infrared imaging and long-slit spectroscopy for the blue compact dwarf galaxy (BCD) Mrk 49 in the Virgo Cluster. The surface brightness distribution analysis shows that Mrk 49 consists of an off-centered blue bright compact core of r = 10" and a red faint outer exponential envelope. The $H_{\alpha}$ image and color difference suggest that these two components have different stellar populations: a high surface brightness population of massive young stars and an underlying low surface brightness population of older stars. The redder near-infrared colors of the inner most region suggest that the near-infrared flux of Mrk 49 originates from evolved massive stars associated with the current star-forming activity. The total apparent magnitude is $B_T\;=\;14.32$ mag and the mean effective surface brightness is ${\mu}_{eff}(B)\;=\;21.56$ mag $arcsec^{-2}$. Long-slit spectroscopy shows that Mrk 49 rotates apparently as a solid body within r = 10" in a plane at position angle 55 degrees with an amplitude of about $20\;km\;sec^{-1}$. The measured radial velocity of Mrk 49 was derived as $1,535\;km\;sec^{-1}$; and the total mass of stars and gases is in the range of 3 to $6\;{\times}\;10^9\;M_{\odot}$. The mass-to-light ratios for the central region of Mrk 49 in I and B band are estimated 1.0 and 0.5, respectively. The upper limit of the dark matter to visible matter ratio seems to be < 5. The oxygen abundance is $12\;+\;\log(O/H)\;=\;8.21\;{\pm}\; 0.1$ which is about one quarter of the solar value while the relative helium abundance appears to be similar to that of the sun.