• 천문학논총
• /
• 제11권1호
• /
• pp.91-107
• /
• 1996

We determine analytically the onset of thin-shell formation time of fast wind bubble with power-law energy injection $E_{in}=E_0t^s$, and power-law ambient density structure, ${\rho}_0(r)={\bar{\rho}}(r/{\bar{r}})^{-{\omega}}$. Thin-shell formation time, $t_{sf}$ can be estimated by minimizing the total time elapsed before the complete cooling of shocked gas. For uniform medium (${\omega}=0$) and constant energy injection (s = 1), the onset of shell formation is found to be at $t_{sf}=5.2{\times}10^3yr$, which agrees Quite well with the results of FCT 1D numerical calculation. We solve the line transfer problem with previous result derived by numerical calculation in order to calculate line profile of [OIII] (${\lambda}=5007{\AA}$) forbidden line. In general, radiative outer shell causes the formation of double peaked line profile. Each peak corresponds to approaching and receeding shells with large velocities. Our line profiles show good agreements with observation of expanding shell structure.

• 대한기계학회논문집
• /
• 제19권11호
• /
• pp.2995-3002
• /
• 1995

The cooling problem of the hot internal pipe flow has been investigated. Simultaneous conduction, convection, and radiation were considered with azimuthally varying convective heat loss at the pipe wall. A complex, nonlinear integro-differential radiative transfer equation was solved by the discrete ordinates method (or called S$_{N}$ method). The energy equation was solved by control volume based finite difference technique. A parametric study was performed by varying the conduction-to-radiation parameter, optical thickness, and scattering albedo. The results have shown that initially the radiatively active medium could be more efficiently cooled down compared with the cases otherwise. But even for the case with dominant radiation, as the medium temperature was lowered, the contribution of conduction became to exceed that of radiation.n.

• Bulletin of the Korean Chemical Society
• /
• 제20권10호
• /
• pp.1181-1185
• /
• 1999

The reaction of FeC5H5+ ion with ferrocene molecule is investigated using FT-ICR mass spectrometry. FeC5H5+ ions are generated by dissociative ionization of ferrocenes using an electron beam. The reaction gives rise to the formation of the adduct ion, Fe2(C5H5)3+, in competition with charge transfer reaction leading to the formation of ferrocene molecular ion, Fe(C5H5)2+·. The branching ratio of the adduct ion increases as the internal energy of the reactant ion decreases and correspondingly the branching ratio for the charge transfer reaction product decreases. The observed rate of the addition reaction channel is slower than that of the charge transfer reaction. The observation of the stable adduct ions in the low-pressure ICR cell is attributed to the radiative cooling of the activated ion-molecule complex. The mechanism of the reaction is presented to account for the observed experimental results.

• 천문학회보
• /
• 제44권2호
• /
• pp.72.1-72.1
• /
• 2019

Symbiotic stars are wide binary systems of a white dwarf and a mass losing giant, exhibiting various activities mainly attributed to accretion of a fraction of slow stellar wind emanating from the giant. We perform 3 dimensional hydrodynamical simulations using the FLASH code to investigate the formation and physical structures of an accretion disk in symbiotic stars with binary separation in the range of 2-4 au. Radiative cooling is introduced in the flow in order to avoid acute pressure increase in the vicinity of the accretor that may prevent stable disk formation. By setting the same density condition in front of the bow shock generated in two different velocity fields, the role of ram pressure balancing between the disk and the wind is examined. We find that three main streams (direct stream from the giant, stream following the accretion wake, and stream passing through the bow shock front) all feed the disk, and their individual contributions on the mass accretion onto the white dwarf are explored.

• 천문학회보
• /
• 제45권1호
• /
• pp.52.1-52.1
• /
• 2020

We propose semi-analytic models for the electron momentum distribution in weak shocks that accounts for both in situ acceleration and reacceleration through diffusive shock acceleration (DSA). In the former case, a small fraction of incoming electrons is assumed to be reflected at the shock ramp and pre-accelerated to the so-called injection momentum, pinj, above which particles can diffuse across the shock transition and participate in the DSA process. This leads to the DSA power-law distribution extending from the smallest momentum of reflected electrons, pref, all the way to the cutoff momentum, peq, constrained by radiative cooling. In the latter case, fossil electrons, specified by a power-law spectrum with a cutoff, are assumed to be re-accelerated from pref up to peq via DSA. We show that, in the in situ acceleration model, the amplitude of radio synchrotron emission depends strongly on the shock Mach number, whereas it varies rather weakly in the re-acceleration model.

• 천문학회보
• /
• 제46권1호
• /
• pp.51.1-51.1
• /
• 2021

Spiral arms greatly affect gas flows and star formation in disk galaxies. We use local 3D simulations of vertically-stratified, self-gravitating, gaseous disks under a stellar spiral potential to study the effects of spiral arms on galactic star formation as well as formation of gaseous spurs/feathers. We adopt the TIGRESS framework to handle radiative heating and cooling, star formation, and ensuing supernova (SN) feedback. We find that more than 90% of star formation takes place inside spiral arms. The global star formation rate (SFR) in models with spiral arms is enhanced by less than a factor of 2 compared to the no-arm counterpart. This supports the picture that spiral arms do not trigger star formation but rather redistribute star-forming regions. Correlated SN feedback produces interarm feathers in both magnetized and unmagnetized models. These feathers live short, have parallel magnetic fields along their length, and are bounded by SN feedback in the lateral direction, in contrast to instability-induced feathers formed in our previous isothermal simulations.

• 천문학회보
• /
• 제46권1호
• /
• pp.30.2-30.2
• /
• 2021

The extended Lyα nebulae (also known as Lyα blobs or LABs) observed at z=2-6 can provide clues to galaxy formation in the early universe. The connection of LABs with the overdensities of compact Lyα emitters suggests that they are associated with matter density peaks in the universe and thus likely to evolve into the present-day groups and clusters of galaxies. However, the mechanism powering the extended Lyα emission in LABs is remained controversial. The detection of polarization signals that follow the theoretically predicted trend is interpreted as strong evidence supporting that the LABs are caused primarily by the resonance scattering of Lyα originating from star-forming galaxies and AGNs. However, Trebitsch et al. (2016) claimed that the radial profile of polarization could be better explained by the scenario in which Lyα photons are produced in the cooling gas surrounding galaxies and then self-scattered by the gas, rather than by the scattering scenario of photons originating from the central galaxies. In this presentation, using LaRT, a state-of-art Lyα radiative transfer code, it is demonstrated that the observed polarization pattern can be reproduced even with the scattering scenario.

• Current Research on Agriculture and Life Sciences
• /
• 제31권1호
• /
• pp.38-44
• /
• 2013

본 연구의 목적은 온실설계 시 야간복사열 손실량 예측을 위한 천공온도를 산정하는데 필요한 적절한 계산식을 제시하는 것이다. 대구지역의 운량에 따른 야간천공온도를 야간복사계를 이용하여 측정하고 기존의 식들을 이용하여 계산하였다. 천공온도를 계산하기 위한 최적의 식을 찾아내기 위하여 측정값과 계산 값을 비교하였다. 운량의 크기에 따라 대기온도와 천공온도의 차이가 달랐으며 운량이 감소함에 따라 온도차는 점차 증가하였다. 맑은 날이 구름 낀 날과 비온 날에 비해 약 10~20배 정도의 더 높은 온도차를 나타내었으며 온도차가 큰 맑은 날이 복사냉각이 크다는 것을 확인할 수 있었다. 맑은 날에 대하여 계산된 천공온도와 측정된 천공온도와의 상관성을 분석한 결과 Bliss식과 Clark and Allen 식이 다른 식들에 비해 상관성이 비교적 더 높은 것으로 나타났다. 구름낀 날에 대해 계산된 천공온도와 측정온도와의 상관성을 분석한 결과 Fuentes 식이 가장 잘 맞는 것으로 나타났다. 구름낀 날의 천공온도를 산정할 수 있는 새로운 식을 제안하였다.

• 한국농림기상학회지
• /
• 제5권4호
• /
• pp.261-265
• /
• 2003

복잡지형상의 일 최저기온 공간내삽 과정에서 유용한 설명변수로 등장한 찬 공기 유입량은 적용면적, 즉 공간규모에 따라 그 값이 크게 변하므로, 지형기후학적 최저기온 내삽모형의 실용화를 위해서는 최적규모를 파악해야 한다. 본 연구에서는 동질적인 중규모 기후구역을 대표하는 기준 관측값에 대한, 같은 구역 내 여러 지점의 기온편차를 계산하고, 이를 다양한 반경의 주변지역 찬 공기 유입량에 회귀시켜 일 최저기온에 미치는 지형의 최적 영향권을 도출하고자 하였다. 경남 하동의 배 과원지대에 1 ${\times}$ 1 km 구역을 설정하고 8개 지점에서 2002년 9월부터 2003년 2월까지 10분 간격으로 기온을 측정하였다. 동일 구역 내 기상청 자동기상관측자료를 기준으로 삼아 복사냉각일의 최저기온 편차를 8개 지점별로 얻었다. 연구지역의 고도를 10 m 해상도의 수치고도모형으로 표현하고 이를 토대로 8개 지점의 냉기 유입량을 계산하였다. 이 때 10 m 단위로 100 m까지 반경을 증가시키면서 유입량의 평활화 평균값을 계산하여 최저기온 편차를 회귀시켰다. 그 결과 복사냉각일의 국지적인 최저기온 결정에는 반경 50 m 범위 (약 1 ha) 주변지역 지형이 가장 유효함을 알 수 있었다.

• 대한원격탐사학회지
• /
• 제33권2호
• /
• pp.249-255
• /
• 2017

남극은 기후변화를 이해하는데 있어 중요한 지역 중 하나이며, 선행연구에 따르면 온난화뿐만 아니라 냉각화도 일어나는 복합적인 지역이다. 그렇기 때문에 남극 에너지 수지의 장기간 변화에 대한 파악이 필요하다. 에너지 수지 요소 중 하나인 순복사는 알베도의 영향을 받으며, 이때 알베도는 negative radiative forcing을 일으키는 요소로 작용한다. 남극의 기후 변화 및 얼음-알베도 피드백에서 두 요소 사이의 관계를 면밀하게 분석하기 위해서는 두 요소 사이의 상관관계를 분석할 필요가 있다. 본 연구에서는 위성 자료를 활용하여 남극에서의 순복사량을 계산하고, 장기간 변화를 분석하였다. 순복사는 연구기간 동안 내륙에서 음의 분포를 보였으며, 해양에서는 양의 분포를 보였다. 순복사의 연간 변화의 경우 해양에서 알베도와 반대되는 변화가 관측되었다. 시계열 패턴은 알베도와 순복사가 서로 대칭되어 나타났으며, 두 요소 사이의 상관관계는 남극 내륙에서 -0.73의 높은 음의 상관관계를 보였으며 해양에서는 -0.32의 음의 상관관계를 보였다.