• 천문학회보
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• 제44권1호
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• pp.40.1-40.1
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• 2019

We utilize times since infall of cluster galaxies obtained from Yonsei Zoom-in Cluster Simulation (YZiCS), the cosmological hydrodynamic N-body simulations, and star formation rates from the SDSS data release 10 to study how quickly late-type galaxies are quenched in the cluster environments. In particular, we confirm that the distributions of both simulated and observed galaxies in phase-space diagrams are comparable and that each location of phase-space can provide the information of times since infall and star formation rates of cluster galaxies. Then, by limiting the location of phase-space of simulated and observed galaxies, we associate their star formation rates at z ~ 0.08 with times since infall using an abundance matching technique that employs the 10 quantiles of each probability distribution. Using a flexible quenching model covering different quenching scenarios, we find the star formation history of satellite galaxies that best reproduces the obtained relationship between time since infall and star formation rate at z ~ 0.08. Based on the derived star formation history, we constrain the quenching timescale (2 - 7 Gyr) with a clear stellar mass trend and confirm that the refined model is consistent with the "delayed-then-rapid" quenching scenario: the constant delayed phase as ~ 2.3 Gyr and the quenching efficiencies (i.e., e-folding timescale) outside and inside clusters as ~ 2 - 4 Gyr (${\propto}M_*^{-1}$) and 0.5 - 1.5 Gyr (${\propto}M_*^{-2}$), Finally, we suggest: (i) ram-pressure is the main driver of quenching of satellite galaxies for the local Universe, (ii) the quenching trend on stellar mass at z > 0.5 indicates other quenching mechanisms as the main driver.

• 천문학회보
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• 제44권2호
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• pp.39.1-39.1
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• 2019

We trace the cosmological origin of satellites around isolated dwarf galaxies using a very high resolution (12 pc/h) cosmological hydrodynamic zoom simulation. To realistically describe the formation and evolution of small-mass stellar satellites, our model includes a full baryonic physics treatment. We find that the mini-halos form objects resembling dwarf galaxies. The majority of their star forming gas is accreted after reionization, thus the survival of a mini-halo's gas to reionization is not an important factor. Instead, the key factor seems to be the ability for a mini-halo to cool its recently accreted gas, which is more efficient in more massive halos. Although the host galaxy is only a dwarf galaxy itself, we find that ram pressure is an efficient means by which accreted mini-halos lose their gas content, both by interacting with hot halo gas but also in direct collisions with the gas disk of the host. The satellites are also disrupted by the tidal forces near the center of the host galaxy. Compared to the disrupted satellites, surviving satellites are relatively more massive, but tend to infall later into the host galaxy, thus reducing the time they are subjected to destructive environmental mechanisms and dynamical friction.

• 생태와환경
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• 제41권4호
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• pp.472-484
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• 2008

The calibrated Andong Reservoir hydro-dynamic module (PART I) of the 2-dimensional hydrodynamic and water quality model, CE-QUAL-W2 [v3.2], was applied to examine the dynamics of total phosphorus, and chlorophyll $\alpha$ concentration within Andong Reservoir. The modeling effort was supported with the data collected in the field for a five year period. In general, the model achieved a good accuracy throughout the calibration period for both chlorophyll ${\alpha}$ and total phosphorus concentration. The greatest deviation in algal concentration occurred on $10^{th}$ October, starting at the layer just beneath the surface layer and extending up to the depth of 35 m. This deviation is principally attributed to the effect of temperature on the algal growth rate. Also, on the same date, the model over-predicts hypolimnion and epilimnion total phosphorus concentration but under-predicts the high concentrated plume in the metalimnion. The large amount of upwelling of finer suspended solid particles, and re-suspension of the sediments laden with phosphorus, are thought to have caused high concentration in the epilimnion and hypolimnion, respectively. Nevertheless, the model well reproduced the seasonal dynamics of both chlorophyll a and total phosphorus concentration. Also, the model tracked the interflow of high phosphorus concentration plume brought by the turbid discharge during the Asian summer monsoon season. Two different hypothetical discharge scenarios (discharge from epilimnetic, and hypolimnetic layers) were analyzed to understand the response of total phosphorus interflow plume on the basis of differential discharge gate location. The simulated results showed that the hypolimnetic discharge gate operation ($103{\sim}113\;m$) was the most effective reservoir structural control method in quickly discharging the total phosphorus plume (decrease of in-reservoir concentration by 219% than present level).

• 대한토목학회논문집
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• 제28권6B호
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• pp.731-741
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• 2008

기존의 한강 감조구간 수치모의에 대한 연구는 단면자료 획득의 어려움이나 유도의 조위자료가 없으므로 하류 경계단을 전류지점으로 하여 모의한 논문이 대부분이나 본 연구에서는 수치해도를 바탕으로 곡릉천 합류부 이후와 임진강 하구부의 단면을 가정하고 인천검조소의 조위자료를 유도지점으로 전이시켜 서해안 조위에 의한 한강하류부에서의 수리학적 거동을 해석하였다. 모형의 적용구간은 신곡수중보로부터 한강의 법적 하류단인 김포시 유도까지 총 36.8 km에 이르는 구간으로 흐름 및 혼합거동 해석은 RMA-2 모형과 서일원(2008)이 개발한 2차원 이송-분산 해석모형인 RAM4를 이용하였다. 전류지점에서의 수위 및 종횡방향 유속 실측자료와 수치모의 결과를 비교하여 흐름해석 결과를 검증하였다. 수위 관측소의 자료가 양호하고 인천검조소에서 높은 조차가 발생하는 2006년 6월 23일~25일 동안 모의한 결과 유도지점의 조위에 따라 총 5회의 역방향 흐름이 관찰되었고 최대 역류 길이는 장항 IC까지 총 32.9 km에 이르렀다. 최대 역방향 흐름의 발생 및 소멸 과정, 최고 유속선을 따른 수위 및 유속을 분석하였으며 이에 따른 비보존성 오염물질의 혼합거동을 해석하였다. 굴포천으로부터 유입된 오염물질은 하폭방향 퍼짐이 두드러지게 일어났지만 곡릉천에서 유입된 BOD는 곡릉천 합류부를 전후하여 중앙 및 좌안측 수심이 급격히 깊어지고 최대유속선이 곡릉천 방향인 우안에서 발생하고 있으므로 횡방향 혼합이 빠르게 완료되어 오염운의 반경이 상대적으로 좁은 것을 확인할 수 있었다. 또한 1차원 이송-분산방정식의 해석해를 적용해 유도지점의 염도 값을 인천검조소로부터 추산하여 한강 하류부에서의 수평 2차원 염수 혼합거동을 해석하였다.