• Journal of The Korean Astronomical Society
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• v.40 no.4
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• pp.141-145
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• 2007

Here we analyze if the ionized shells associated with giant HII regions represent the progenitors of the larger neutral hydrogen supershells detected in the Milky Way and other spiral and dwarf irregular galaxies. We calculate the evolutionary tracks that 12 HII shells found by Relano et al. (2005, 2007) would have if they expanded into the interstellar medium because of multiple supernovae explosions occurring inside the cavity. We find, contrary to Relano et al. (2007), that the evolutionary tracks of these HII shells are inconsistent with the observed parameters of the largest and most massive neutral hydrogen supershells. Thus, an additional energy source to the multiple supernovae explosions is required in order to explain the origin of the most massive neutral hydrogen shells.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.75.2-75.2
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• 2010

We have studied the statistical properties of turbulence in molecular clouds identified in the Boston University - Five College Radio Astronomy Observatory (BU-FCRAO) Galactic Ring Survey (GRS). Toward this end, the probability density function (PDF) and velocity distribution were measured for about 50 molecular clouds. We found there exists a good correlation between the PDF width and the velocity dispersion for these molecular clouds. In order to investigate how general properties of astrophysical turbulence depends on the plasma parameters such as magnetic field strength and sonic Mach number, we performed three-dimensional MHD simulations. We then examined if the observed characteristics of interstellar turbulence are consistent with theoretical results from MHD simulations.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.66.1-66.1
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• 2010

Using two-dimensional numerical hydrodynamic simulations, we investigate the star formation rate (SFR) in turbulent, multiphase, galactic gaseous disks. Our simulation domain is axisymmetric, and local in the radial direction and global in the vertical direction. Our models include galactic rotation, vertical density stratification, self-gravity, radiative heating and cooling, and thermal conduction, but do not include spiral-arm features. Turbulence in our models is driven by momentum feedback from supernova explosion events occurring in localized dense regions formed by thermal and gravitational instabilities. Self-consistent radiative heating, representing enhanced/reduced FUV photons from the star formation, is also taken into account. By controlling three parameters (the gas surface density, the stellar disk density, and the angular rotation rate) that characterize local galactic disks, we explore how the SFR depends on the background environmental state. We also discuss the relation between the SFR and the gas surface density found in our numerical models in comparison with observations.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.73.1-73.1
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• 2010

We use three-dimensional hydrodynamic simulations to investigate the characteristics of turbulence driven in rotating, vertically-stratified disk. Our models are isothermal, and local in the in-plane direction while global in the vertical direction. We allow localized regions with density larger than the threshold value to explode and inject kinetic energy to the surrounding medium in the real space rather than Fourier space, mimicking supernova explosions thought to be the dominant turbulence source. This work extends our previous study where we studied turbulence in a non-rotating, uniform environment. We find that the galaxy rotation does not make a significant difference in the turbulence level at saturation, since the associated shear velocity is much smaller than the explosion velocity. We analyze the properties of turbulence in our models and compare them with those from the uniform-density models. We also discuss the astrophysical implication of our findings.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.60.2-60.2
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• 2010

We have studied the abundance ratio of HNC and HCN toward the Red MSX Sources (RMS) using HCN (J=1-0), HNC (J=1-0), $H^{13}CN$ (J=1-0), $HN^{13}C$ (J=1-0),and $N_2H^+$ (J=1-0) lines observed with the Mopra 22 m radio telescope. The RMS are massive young stellar objects identified by the MSX satellite data combined with the 2MASS data. HCN and HNC (a geometrical isomer of HCN) are among the most basic interstellar molecules. According to our analysis, the column density of HCN is found to be correlated with that of HNC. Additionally, the [HNC]/[HCN] abundance ratio is sensitive to the core temperature because HNC is depleted in high temperature regions. This result is consistent with the previous results seen in low mass starless or protostellar cores.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.59.1-59.1
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• 2010

We present wide-field near-IR imaging polarimetry of 30 Doradus, using the InfraRed Survey Facility(IRSF) 1.4 m telescope at the South African Astronomical Observatory. We obtained polarimetry data in J, H, and Ks bands using the JHKs-simultaneous imaging polarimeter SIRPOL. 30 Doradus is located in the Large Magellanic Cloud(LMC) and it is the most active starburst region known in the Local group of galaxies. 30 Doradus is one of the best field to examine the behavior of the interstellar medium and star-formation mechanism under different conditions. We will investigate the structure of magnetic field in 30 Doradus region.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.89.1-89.1
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• 2010

Cassini/VIMS 관측에 의하면 타이탄의 3 마이크론 파장영역에서 다른 파장 대와 달리 메탄 분자만으로는 관측 값에 맞는 모델을 만들기 힘든 특이한 형태의 흡수 밴드 영역이 발견되었다 (Bellucci et al. 2009, Icarus, v. 201, p. 198). 이 파장영역은 행성뿐만 아니라 ISM (Interstellar Medium)과 혜성 등에서 연구 되고 있는 C-H stretching band와 흡사한 구조를 가지고 있다. 이러한 구조는 타이탄 연무 속에 포함된 유기물질에 의한 것으로 추정된다. 본 연구는 최근까진 개발된 복사방정식 모델과 2006년 Cassini/VIMS가 관측한 고도에 따른 solar occultation 데이터를 비교하여 밴드구조의 실체를 알아보는 것이 주 목적이다. 우리는 고도 별로 다르게 나타나는 흡수밴드의 파장 영역을 세밀히 나눈 후 메탄과 함께 유기물질의 연무가 더해진 모델을 만들었다. 도출된 유기물질의 구조가 관측된 밴드 구조에 미치는 영향을 알아보고 앞으로의 연구 방향을 제시 할 것이다.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.68.2-68.2
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• 2010

Diffuse interstellar atomic hydrogen (HI) gases are easily shaped into shell-like features by energetic processes such as stellar winds and supernova explosions. The physical characteristics and the Galactic distribution of HI shells and shell-like structures, therefore, are closely related to those of the energy sources. Recently, Inner-Galaxy Arecibo L-band Feed Array (I-GALFA) low-latitude HI survey has been completed. I-GALFA HI survey covers the central part of the first quadrant ($31^{\circ}{\lesssim}1{\lesssim}77^{\circ}$ at b = $0^{\circ}$, ${\mid}b{\mid}\lesssim\;12^{\circ}$) with spatial and velocity resolutions of 3.35′and 0.184 km/s, respectively. The high-angular and high-velocity resolutions enable in-depth investigation of HI shells including the ones of smaller angular sizes. We have found 36 shell candidates with the naked eye. Their angular sizes are distributed from $\sim0.4^{\circ}$ to $\sim12^{\circ}$. About sixteen of them appear to be expanding. We examine associated features at other wavebands and discuss their origin.

• Journal of The Korean Astronomical Society
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• v.47 no.1
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• pp.15-39
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• 2014

Polarization is a basic property of light and is fundamentally linked to the internal geometry of a source of radiation. Polarimetry complements photometric, spectroscopic, and imaging analyses of sources of radiation and has made possible multiple astrophysical discoveries. In this article I review (i) the physical basics of polarization: electromagnetic waves, photons, and parameterizations; (ii) astrophysical sources of polarization: scattering, synchrotron radiation, active media, and the Zeeman, Goldreich-Kylafis, and Hanle effects, as well as interactions between polarization and matter (like birefringence, Faraday rotation, or the Chandrasekhar-Fermi effect); (iii) observational methodology: on-sky geometry, influence of atmosphere and instrumental polarization, polarization statistics, and observational techniques for radio, optical, and $X/{\gamma}$ wavelengths; and (iv) science cases for astronomical polarimetry: solar and stellar physics, planetary system bodies, interstellar matter, astrobiology, astronomical masers, pulsars, galactic magnetic fields, gamma-ray bursts, active galactic nuclei, and cosmic microwave background radiation.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.48.2-48.2
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• 2018

SPHEREx is expected to provide us with the opportunity of unbiased sampling of small Solar System objects along with near-infrared ($0.75-5.0{\mu}m$) spectroscopic (R ~ 41) information. The estimated numbers of detections are tens of thousands for asteroids, thousands for Trojans, hundreds for comets, and several for Kuiper Belt Objects, Centaurs and Scattered Disk Objects. Wide spectral range covering many bands from carbon-bearing molecules and ices will enable us to systematically survey the volatile materials throughout the Solar System. SPHEREx will, for the first time, produce the near-infrared spectral map of the zodiacal light to pin-down the relative contributions of various populations of Solar System objects and interstellar dust to the dust grains in the interplanetary space. The study of the zodiacal light is also important to remove the foreground for the EBL (extragalactic background light) study, one of the main topics of the mission.