• The Bulletin of The Korean Astronomical Society
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• v.38 no.2
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• pp.50.1-50.1
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• 2013

Blue Compact Dwarf galaxies (BCDs) are systems which have been experiencing the bursts of star formation in their central region. As one of the origins of active star formation, tidal interaction (merger or fly-by between dwarf galaxies) has been suggested. A pair of BCDs, ESO 435-IG20 and ESO 435-IG16, are suspected to be a good example of such case. They are located at a similar redshift and separated only by ~130 kpc at their distances. In addition a bridge-like HI structure has been found between these two BCDs in the HIPASS survey. In this study, using the ATCA HI data of a much better resolution, we probe the gas morphology and kinematics of individual galaxies. We discuss how tidal interaction is responsible for the high star formation rate in this BCD pair.

• Proceedings of the Polymer Society of Korea Conference
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• 2006.10a
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• pp.337-337
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• 2006

The synthesis of an octafunctional resorcinarene based initiator for nitroxide mediated polymerization and its ability to yield random star copolymers of styrene and methyl methacrylate is studied. The effect of the initiator conformations towards its activity and the conditions that permit the formation of well-defined star block copolymers is also investigated in detail. The characterization of the initiator and the polymers were carried out by various spectro-analytical techniques. Well-defined random copolymers were obtained with controlled molecular weight and low PDI depending on the monomer feed.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.79.1-79.1
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• 2014

We present the result of near-infrared (near-IR) imaging polarimetry of star-forming regions in the Large Magellanic Cloud (LMC). We compiled near-IR photometric and polarimetric data of N159/160 regions. The photometric and polarimetric data were simultaneously obtained in J, H, and Ks bands using SIRPOL, an imaging polarimeter of the InfraRed Survey Facility (IRSF), in 2007 February. We measured Stokes parameters of point-like sources to derive their degree of polarization and polarization position angles. In this poster, we present polarization properties of these star-forming regions. We also discuss the polarization structure in these regions compared with mid-infrared dust emission structure from the Spitzer SAGE survey.

• Journal of Korean Association for Spatial Structures
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• v.14 no.4
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• pp.89-96
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• 2014

Spatial structures as like dome structure have the different dynamic characteristics from general rahmen structures. Therefore, it is necessary to accurately analyze dynamic characteristics and effectively control of seismic response of spatial structure subjected to multi-supported excitation. In this study, star dome structure that is subjected to multi-supported excitation was used as an example spatial structure. The response of the star dome structure under multiple support excitation are analyzed by means of the pseudo excitation method. Pseudo excitation method shows that the structural response is divided into two parts, ground displacement and structural dynamic response due to ground motion excitation. And the application of passive tuned mass damper(TMD) to seismic response control of star dome structures has been investigated. From this numerical analysis, it is shown that the seismic response of spatial structure under multiple support seismic excitation are different from those of spatial structure under unique excitation. And it is reasonable to install TMD to the dominant points of each mode. And it is found that the passive TMD could effectively reduce the seismic responses of dome structure subjected to multi-supported excitation.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.2
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• pp.34.2-34.2
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• 2015

We aim to investigate the formation of primordial globular clusters (GCs) in the isolated dwarf galaxy (${\sim}10^{10}M_{sun}$) with cosmological zoom-in simulations. For this, we modified cosmological hydrodynamic code, GADGET-3, in a way to include the radiative heating/cooling that enables gas particles cool down to T~10K, reionization (z < 8.9) of the Universe, UV shielding ($n_{shield}$ > $0.014cm^{-3}$), and star formation. Our simulation starts in a cubic box of a side length 1Mpc/h with 17 million particles from z = 49. The mass of each dark matter (DM) and gas particle is $M_{DM}=4.1{\times}10^3M_{sun}$ and $M_{gas}=7.9{\times}10^2M_{sun}$, respectively, thus the GC candidates can be resolved with more than hundreds particles. We found the following results: 1) mini halos with the more interactions before merging into the main halo form the more stars and thus have the higher star mass fraction ($M_{star}/M_{total}$), 2) the mini halos with the high $M_{star}/M_{total}$ can survive longer and thus spiral into closer to the galactic center, 3) the majority of them spiral into bulge, but some of them can survive until the last as baryon-dominated system, like the GC.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.42.2-42.2
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• 2014

We investigate the history of formation of ~400 galaxies in four Abell clusters at 0.04

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.61.1-61.1
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• 2014

IC 10 is one of the most well-known irregular starburst dwarf galaxies in the Local Group. Its low metal and oxygen abundance together with proximity make it an excellent laboratory to test star formation models, especially in low-metallicity systems like galaxies in the early Universe as well as many other local dwarfs. Among a number of active star forming regions, we have detected H2O kilo-maser emission in the south-east region of IC 10(IC 10 SE) using the Korean VLBI Network(KVN). This maser line is likely to be associated with a giant molecular cloud identified in IC 10 SE by former CO studies. Using the HI and CO data from the VLA and SMA archive, we probe the atomic and molecular gas properties of IC 10 SE. We discuss how the cool gas morphology and kinematics are related with maser and star formation activity in IC 10 SE.

• The Journal of the Korea Contents Association
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• v.17 no.12
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• pp.236-246
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• 2017

As a research on culinary staffs' subjective perception of star chefs' appearance in cooking broadcast, this study analyzed the subjective tendency targeting culinary staffs in hotels & restaurants by applying Q methodology. Three research questions of this study were set up like below. First, what are the culinary staffs' acceptance types of subjective perception of star chefs' appearance in cooking broadcast? Second, what are the characteristics of homogeneous type of culinary staffs' subjective perception of star chefs' appearance in cooking broadcast? Third, what are the things in common and differences of culinary staffs' each subjective perception type of star chefs' appearance in cooking broadcast? In the results of typological analysis based on such research questions, total four types were drawn such as Acquiring expertise through cooking broadcast type(Type1, N=8), New broadcast genre recognition type(Type2, N=10), The profession of the chef reality recognition type(Type3, N=2), and Profession image of chef synergy type(Type4, N=2). Each type showed its own distinctive characteristics.

• Journal of the Korean Society of Costume
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• v.58 no.6
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• pp.69-84
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• 2008

Considering that star reflects the image of current society, analyzing fashion of celebrity is to read ideal type and demands of beauty of the era. Especially the rock music-represents youth culture that last on present day-born in 1960's, and it is considered to a significant decade in pop music history. Thus this research will analysis rock star's fashions in iconological view of E. Panofsky. The aim of this document is Clarifying how the fashion of pop stars appeared and what formed its worth. As a result of analyzing fashions of rock star in 1960's, it is available to find these sameness and difference. The Mods borrowed images of the past, and introduce the elite modernism and shows very urban style. The Folky and the Psychedelic showed post-structuralism propensity against industrial society, in the case of the Folky it induced styles that symbolize labor class to realize social worth. And as an aftereffect of war and repulsion of commercial worth, they embody nature-returning peasant look so that it shows pastoral mood in total. The Psychedelic express somewhat struggling escapism and it generated illusionary images with quests to superego and glorification to psychedelic status. The Folky and the Psychedelic are same in the side of introducing existentialism, this occurred by using ethnic factor. But the Folky showed plain outlook by pop propensity, on the other hand, the Psychedelic showed magnificent outlook such as optical art, pop art, and futurism ought to express merrymaking culture. And common feature of these is introduction of unisex mod which is came after the change of gender role. Thus each star or group has professed special ideology into their culture and it is reflected to acts which is including music and dress style. This affair is analyzed like these two things. The mass of people schemes their identity with inducing special ideology to their culture at the first. And the purpose to archive cultural hegemony in inter-social class at the next.

• Journal of The Korean Astronomical Society
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• v.36 no.3
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• pp.81-87
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• 2003

It is suggested that a flying-by star in a hot accretion disk may cool the hot accretion disk by the Comptonization of the stellar emission. Such a stellar cooling can be observed in the radio frequency regime since synchrotron luminosity depends strongly on the electron temperature of the accretion flow. If a bright star orbiting around the supermassive black hole cools the hot disk, one should expect a quasi-periodic modulation in radio, or even possible an anti-correlation of luminosities in radio and X-rays. Recently, the unprecedentedly accurate infrared imaging of the Sagittarius A$\ast$ for about ten years enables us to resolve stars around it and thus determine orbital parameters of the currently closest star S2. We explore the possibility of using such kind of observation to distinguish two quite different physical models for the central engine of the Sagittarius A$\ast$, that is, a hot accretion disk model and a jet model. We have attempted to estimate the observables using the observed parameters of the star S2. The relative difference in the electron temperature is a few parts of a thousand at the epoch when the star S2 is near at the pericenter. The relative radio luminosity difference with and without the stellar cooling is also small of order $10^{-4}$, particularly even when the star S2 is near at the pericenter. On the basis of our findings we tentatively conclude that even the currently closest pass of the star S2 is insufficiently close enough to meaningfully constrain the nature of the Sagittarius A$\ast$ and distinguish two competing models. This implies that even though Bower et al. (2002)have found no periodic radio flux variations in their data set from 1981 to 1998, which is naturally expected from the presence of a hot disk, a hot disk model cannot be conclusively ruled out. This is simply because the energy bands they have studied are too high to observe the effect of the star S2 even if it indeed interacts with the hot disk. In other words, even if there is a hot accretion disk the star like S2 has imprints in the frequency range at v $\le$ 100 MHz.