• The Bulletin of The Korean Astronomical Society
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• v.32 no.2
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• pp.51.1-51.1
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• 2007

• The Bulletin of The Korean Astronomical Society
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• v.27 no.2
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• pp.29-29
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• 2002

• The Bulletin of The Korean Astronomical Society
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• v.21
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• pp.6.2-7
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• 1996

• The Bulletin of The Korean Astronomical Society
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• v.31 no.2
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• pp.70.2-70.2
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• 2006

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.43.1-43.1
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• 2018

Star formation in galaxies predominantly takes place in giant molecular clouds (GMCs). While it is widely believed that UV radiation feedback from young massive stars can destroy natal GMCs by exciting HII regions and driving their expansion, our understanding on how this actually occurs remains incomplete. To quantitatively assess the effect of UV radiation feedback on cloud disruption, we conduct a series of theoretical studies on the dynamics of HII regions and its role in controlling the star formation efficiency (SFE) and lifetime of GMCs in a wide range of star-forming environments. We first develop a semi-analytic model for the expansion of spherical dusty HII regions driven by the combination of gas and radiation pressures, finding that GMCs in normal disk galaxies are destroyed by gas-pressure driven expansion with SFE < 10%, while more dense and massive clouds with higher SFE are disrupted primarily by radiation pressure. Next, we turn to radiation hydrodynamic simulations of GMC dispersal to allow for self-consistent star formation as well as inhomogeneous density and velocity structures arising from supersonic turbulence. For this, we develop an efficient parallel algorithm for ray tracing method, which enables us to probe a range of cloud masses and sizes. Our parameter study shows that the net SFE, lifetime (measured in units of free-fall time), and the importance of radiation pressure (relative to photoionization) increase primarily with the initial surface density of the cloud. Unlike in the idealized spherical model, we find that the dominant mass loss mechanism is photoevaporation rather than dynamical ejection and that a significant fraction of radiation escapes through low optical-depth channels. We will discuss the astronomical.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.50.2-50.2
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• 2013

In the process of star formation, the density and temperature of associated material, which are the physical conditions for the molecular chemistry, vary dramatically. As a result, the connection between physical and chemical conditions has been used to trace the evolutionary stages in star formation. One chemical tracer for the physical conditions in star forming material is the [HCN]/[HNC] abundance ratio since the ratio strongly depends on the kinetic temperature in molecular clouds. Here we investigate the [HCN]/[HNC] abundance ratios in objects related to the massive star formation. For the investigation, we carried out $H^{13}CN$ and $HN^{13}C$ line observation toward objects in three different evolutionary stages of massive star formation: Infrared dark clouds (IRDCs), High-mass protostellar object (HMPOs), and Ultra-compact HII regions (UCHIIs). According to our observational results, both $H^{13}CN$ and $HN^{13}C$ lines have been detected toward 19 IRDCs, 25 HMPOs, and 31 UCHIIs. We will discuss about the [HCN]/[HNC] abundance ratios in different evolutionary stages of massive star formation and associate the results with the physical conditions of the targets.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.57.1-57.1
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• 2014

We present the preliminary results of CO outflow survey toward the 56 Very Low Luminosity Object (VeLLO) candidates at CO J=2-1 and J=3-2 transitions with two radio telescopes of the Caltech Submillimeter Observatory (CSO) and the Atacama Submillimeter Telescope Experiment (ASTE). The survey is aimed to understand the origin of the formation of low-mass stars or substellar objects. The VeLLO is a very faint (${\leq}0.1$ $L_{\odot}$) object deeply embedded in dense molecular clouds and believed to be a proto-brown dwarf which will be a brown dwarf or a faint protostar which has just formed with little mass accretion or which is in quiescent stage of episodic accretion. The candidates were searched for over all nearby ($d{\leq}450$ pc) Gould belt clouds and listed in a new catalogue of the VeLLO candidates by Kim et al. (2014 submitted). To diagnose present status and future fate of the VeLLOs, we conducted a systematic observation for the CO molecular outflows of the 56 VeLLOs to infer how accretion is being made around the VeLLOs. We found 17 VeLLO candidates either having a prominent wing in line profiles or showing bipolar intensity distribution of high velocity components. We will discuss the physical properties of these CO outflows and the identity of the VeLLO candidates.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.52.1-52.1
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• 2018

Orion Molecular Clouds Complex(OMC) 분자운에는 별 생성은 없으면서 은하면 방향으로 누워있는 큰 규모($10^{\circ}{\times}0.5^{\circ}$)의 필라멘트 구조가 있다. 본 연구는 북쪽 필라멘트(이하 NF)를 대상으로 12CO (J = 1-0) 선 관측 데이터를 이용하여 필라멘트의 운동학적 연구를 수행함으로서 은하면과의 상관관계를 알아보고자 하였다. 관측은 공간분해능은 2 arcmin인 SRAO(Seoul Radio Astronomy Observatory)의 6m 밀리미터 망원경이 사용되었고 큰 규모로 인해 은하면으로부터 먼 순서로 NF1, NF2, NF3 세 곳으로 관측 지역이 정해졌다. 연구결과 필라멘트는 매우 낮은 수준의 12CO (J = 2-1)과 티끌 분포에서 자기장을 따라 은하면 방향으로 연계되어 보였다. 밀도 분포에서는 SRAO 12CO (J = 1-0) 적분강도와 Planck 위성의 12CO (J = 2-1)과 티끌 자료를 이용했을 때, 12CO와 성간 티끌은 주로 은하면에 수직인 방향에서 밀도가 높았다. 속도 분포와 위치 속도 분석을 통해 NF는 단일 구조의 분자운 형태이고 NF2 하단에서는 회전 운동의 가능성이 확인되었다. NF3는 자기장에 의해 생성된 나선형 회전을 하고 있으며, NF2와 NF3를 따라 은하면을 향하여 12CO (J = 1-0)를 비롯한 물질이 흐르고 있음도 확인되었다. 하지만 은하면을 향하여 물질이 흐르는 원인을 제공하는 천체가 무엇인지와 NF1과 NF2 상단의 회전 운동은 확인 할 수 없었으며 이들 지역에 대한 상세한 관측이 요구된다.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.2
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• pp.47.2-47.2
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• 2019

Observations indicate that turbulence in molecular clouds of the interstellar medium (ISM) is highly supersonic (M >> 1) and strongly magnetized (β ≈ 0.1), while in the intracluster medium (ICM) it is subsonic (M <~1) and weakly magnetized (β ≈ 100). Here, M is the turbulent Mach number and β is the ratio of the gas to magnetic pressures. Although magnetohydrodynamic (MHD) turbulence in such environments has been previously studied through numerical simulations, some of its properties as well as its consequences are not yet fully described. In this talk, we report a study of MHD turbulence in molecular clouds and the ICM using a newly developed code based the high-order accurate, WENO (Weighted Essentially Non-Oscillatory) scheme. The simulation results using the WENO code are generally in agreement with those presented in the previous studies with, for instance, a TVD code (Porter et al. 2015 &, Park & Ryu 2019), but reveal more detailed structures on small scales. We here present and compare the properties of simulated turbulences with WENO and TVD codes, such as the spatial distribution of density, the density probability distribution functions, and the power spectra of kinetic and magnetic energies. We also describe the populations of MHD shocks and the energy dissipation at the shocks. Finally, we discuss the implications of this study on star formation processes in the ISM and shock dissipation in the ICM.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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• pp.173-174
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• 1996

We have mapped $17 deg^2$ region toward Galactic anticenter in $^{12}CO$ J = 1 - 0 using the 3 mm SIS receiver on the 14 m telescope at Taeduk Radio Astronomy Observatory (TRAO). The region mapped in this paper is the first target of the Galactic AntiCenter CO Survey Project (GACCOS) and was selected comparing with IRAS Sky Survey Atlas (ISSA) images at 100${\mu}m$. Molecular emission of the target area is found to be very extended and is well matching with the FIR emission boundary. There are several pieces of clouds, and as some of spectra show several peaks, there seem to be several clouds overlapped in some directions. The Velocity of Local Standard of Rest ($V_{LSR}$) of the CO emission of the mapped region ranges from -20 to +10 km/s. It is also found that the two cloudlets located around I = $180^{\circ}$ have $V_{LSR}$ = -20 km/s, which is very abnormal. The peak antenna temperature of 13 K arises near the H II Region S241.