• Journal of Astronomy and Space Sciences
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• 제2권1호
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• pp.7-18
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• 1985

Accretion rate가 $M=10^{16}g/sec$ 와 $M=10^{18}g/sec$인 경우의 정상상태의 Accretion disk의 모델들을 만들었다. 중심에 있는 별은 백색왜성으로 가정하고 질량은 $1M_\odot$이고 반경은 $10^9cm$로 보았다. 이 모델을 왜신성인 Z cha와 Z Cam에 응용하였다.

• 천문학회보
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• 제46권2호
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• pp.35.1-35.1
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• 2021

Variability in young stellar objects (YSOs) can be caused by various time-dependent phenomena associated with star formation, including accretion rates, geometric changes in the circumstellar disks, stochastic hydromagnetic interactions between stellar surfaces and inner disk edges, reconnections within the stellar magnetosphere, and hot/cold spots on stellar surfaces. Among these YSO variability phenomena, bursts of accretion, which are the most remarkable variability, usually occur sporadically, making it challenging to catch the bursting moments observationally. However, the burst accretion process significantly affects the chemical conditions of the disk and envelope of a YSO, which can be used as a prominent tracer of episodic accretion. I will introduce our ensemble studies of YSO variability at mid-IR and submillimeter and also cover the ALMA observations of several YSOs in the burst accretion phase, especially in the view of chemistry.

• 한국항공우주학회지
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• 제39권8호
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• pp.689-701
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• 2011

본 연구에서는 착빙 환경 요소와 결빙 형상 파라미터의 관계를 자가조직도와 분산분석을 활용하여 분석하였다. 결빙 형상에 영향을 미치는 외기 조건으로 자유류 속도, 대기온도, 대기중 물방울 함유량(LWC), 액적의 평균 직경(MVD)을 선정하였다. 그리고 결빙 형상의 특징이 되는 파라미터로 최대 두께, 결빙한계(Icing limit), 결빙 진행 방향, 결빙면적을 선정하였다. 자가 조직도의 결과는 결빙형상 파라미터에 관계가 있는 외기 조건에 대한 정성적인 관계를 제시하였고 분산분석의 결과는 형상 파라미터에 대한 외기 조건의 영향력의 상대적인 크기와 순위를 정량적으로 제시하였다.

• 조명전기설비학회논문지
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• 제17권3호
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• pp.95-102
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• 2003

전선착설로 인한 전력설비에의 피해를 방지하기 위하여, 전선착설을 예측하고 적절한 전선착설 방지대책을 제시하는 것은, 전선착설로 인한 피해 발생의 가능성과 전력계통의 안정적 운영의 양 측면을 동시에 고려하여야 하기 때문에 고도한 판단과 결단이 필요한 문제로써, 지식공학적 수법을 적용하는 것이 매우 효과적인 분야이다. 이에 따라, 전선착설의 예측과 방지대책 수립에 관련된 경험적 지식을 지식베이스화하여 전문가 시스템을 구축하고, 사례 데이터를 이용한 시뮬레이션을 통하여 제안 기법의 유효성을 확인하였다.

• 대한전기학회:학술대회논문집
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• 대한전기학회 1992년도 하계학술대회 논문집 A
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• pp.193-195
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• 1992

Snow accretion on transmission lines may cause critical accidents such as sleet jump, tower collpases, etc,. In order to assist power system operators to prevent thses accidents, aprototype expert system had been developed. The system has basic functions of forecasting snow accretion on transmission lines and making a list of all feasible and effective deicing countermeasures. The knowledge of the effect of weather conditions on the snow accretion process continue main rule base. Simulation results show that the proposed system is very promising.

• 천문학회지
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• 제29권spc1호
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• pp.231-232
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• 1996

The local instabilities of accretion disks were extensively studied, with the considerations of radial advection, thermal diffusion and different disk geometry, dominated pressure and optical depth. Two inertial-acoustic modes in a geometrically thin, radiative cooling dominated disk depart from each other if very little advection is included. A geometrically slim, advection-dominated disk is found to be always stable if it is optically thin. However, if it is optically thick, the thermal diffusion has no effect on the stable viscous mode but has a significant contribution to enhance the thermal instability.

• 천문학논총
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• 제17권1호
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• pp.11-14
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• 2002

Our examination of the relations of spherically symmetric accretion on a massive point object to viscous drag, neglecting gas pressure and using self-similar transformation, shows the behaviors of the asymptotic solutions? in the regions near to and far from the center. The viscosity reduces the free-fall velocity by the factor $(1\;+\;\zeta) ^{-1}$, and causes flattening in the density distribution. Therefore, the viscosity leads to the reduction of the mass accretion rate.

• 천문학회보
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• 제46권2호
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• pp.66.3-67
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• 2021

Low-mass stars form by the gravitational collapse of dense molecular cores. Observations and theories of low-mass protostars both suggest that accretion bursts happen in timescales of ~100 years with high accretion rates, so called episodic accretion. One mechanism that triggers accretion bursts is infalling fragments from the outer disk. Such fragmentation happens when the disk is massive enough, preferentially activated during the embedded phase of star formation (Class 0 and I). Most observations and models focus on the gas structure of the protostars undergoing episodic accretion. However, the dust and ice composition are poorly understood, but crucial to the chemical evolution through thermal and energetic processing via accretion burst. During the burst phase, the surrounding material is heated up, and the chemical compositions of gas and ice in the disk and envelope are altered by sublimation of icy molecules from grain surfaces. Such alterations leave imprints in the ice composition even when the temperature returns to the pre-burst level. Thus, chemical compositions of gas and ice retain the history of past bursts. Infrared spectral observations of the Spitzer and AKARI revealed a signature caused by substantial heating, toward many embedded protostars at the quiescent phase. We present the AKARI IRC 2.5-5.0 ㎛ spectra for embedded protostars to trace down the characteristics of accretion burst across the evolutionary stages. The ice compositions obtained from the absorption features therein are used as a clock to measure the timescale after the burst event, comparing the analyses of the gas component that traced the burst frequency using the different refreeze-out timescales. We discuss ice abundances, whose chemical change has been carved in the icy mantle, during the different timescales after the burst ends.

• 천문학회지
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• 제34권1호
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• pp.31-33
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• 2001

The collision effects in particles of the accretion disk are examined by the use of small perturbation. The collision force is assumed to be equal to 2 vV. From the equations governing collisions of such particles the local dispersion relation is obtained.

• 한국전산유체공학회:학술대회논문집
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• 한국전산유체공학회 2009년 춘계학술대회논문집
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• pp.21-26
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• 2009

Ice accretion is one of the potential hazards in airplane flight, adversely affecting aircraft aerodynamic. There are two distinct icing analysis that can be simulated. One is predicting the effect of ice on the aerodynamic performance of airfoils when ice geometry is known. The other is simulating ice accretion. This work presents the method of icing accretion analysis. This work presents an Eulerian approach to calculate the droplet collection efficiency on the 2D airfoil. The initial flow solution are obtained the FLUENT and copled with droplet motion in the ambient condition.