• 한국정보통신학회논문지
• /
• 제23권4호
• /
• pp.416-422
• /
• 2019

본 논문은 절차적함수를 이용하여 실시간으로 3차원 구름을 모델링하고 렌더링하는 알고리즘을 제안한다. 구름 모델링은 절차적 노이즈 함수인 fbm(Fractional Brownian Motion)을 변형하여 사용하며, 이 값을 대기의 수증기 밀도 값으로 이용한다. 이 밀도 값은 파라미터로 주어진 3가지 구름의 형태를 위해 변형되며 렌더링단계의 입력 값으로 들어간다. 레이마칭(ray marching)기법을 이용한 렌더링 단계에서는 이 밀도 값을 이용하여 구름의 색상을 결정하며 이때 밀도에 따른 빛의 감소 및 산란현상은 물리적으로 계산된다. 대기모델로 렌더링 된 하늘 위에 제안한 알고리즘에 의해 구현된 구름들이 블랜딩되며, 이 때 바람의 방향에 따라 구름이 움직이도록 한다. 제안된 구름 생성 및 렌더링은 GLSL언어를 이용해서 GPU상에서 구현되었다.

• 천문학회보
• /
• 제44권1호
• /
• pp.42.1-42.1
• /
• 2019

We observed 80 dense cores ($N(H_2)$ > $10^{22}cm^{-2}$) in the Orion molecular cloud complex which contains the Orion A (39 cores), B (26 cores), and ${\lambda}$ Orionis (15 cores) clouds. We investigate the behavior of the different molecular tracers and look for chemical variations of cores in the three clouds in order to systematically investigate the effects of stellar feedback. The most commonly detected molecular lines (with the detection rates higher than 50%) are $N_2H^+$, $HCO^+$, $H^{13}CO^+$, $C_2H$, HCN, and $H_2CO$. The detection rates of dense gas tracers, $N_2H^+$, $HCO^+$, $H^{13}CO^+$, and $C_2H$ show the lowest values in the ${\lambda}$ Orionis cloud. We find differences in the D/H ratio of $H_2CO$ and the $N_2H^+/HCO^+$ abundance ratios among the three clouds. Eight starless cores in the Orion A and B clouds exhibit high deuterium fractionations, larger than 0.10, while in the ${\lambda}$ Orionis cloud, no cores reveal the high ratio. These chemical properties could support that cores in the ${\lambda}$ Orionis cloud are affected by the photo-dissociation and external heating from the nearby H II region. An unexpected trend was found in the $[N_2H^+]/[HCO^+]$ ratio with a higher median value in the ${\lambda}$ Orionis cloud than in the Orion A/B clouds than; typically, the $[N_2H^+]/[HCO^+]$ ratio is lower in higher temperatures and lower column densities. This could be explained by a longer timescale in the prestellar stage in the ${\lambda}$ Orionis cloud, resulting in more abundant nitrogen-bearing molecules. In addition to these chemical differences, the kinematical difference was also found among the three clouds; the blue excess, which is an infall signature found in optically thick line profiles, is 0 in the ${\lambda}$ Orionis cloud while it is 0.11 and 0.16 in the Orion A and B clouds, respectively. This result could be another evidence of the negative feedback of active current star formation to the next generation of star formation.

• 대한원격탐사학회지
• /
• 제38권6_1호
• /
• pp.1181-1189
• /
• 2022

구름은 대기 중에 떠 있는 작은 물방울이나 얼음 알갱이들 또는 혼합물 등으로 구성되며 지구 표면의 약 2/3를 덮고 있다. 위성영상내에서의 구름은 일부 다른 지상 물체 또는 지표면과 유사한 반사도 특성으로 인해 구름과 구름이 아닌 영역을 분리하는 구름탐지는 매우 어려운 작업이다. 특히 뚜렷한 특징을 가지는 두꺼운 구름과 달리 얇은 반투명 구름은 위성영상내에서 구름과 배경의 대비가 약하고 지표면과 혼합되어져 나타나기 때문에 대부분 구름탐지에서 쉽게 놓쳐지고 많은 어려움을 주는 대상으로 작용한다. 이러한 구름탐지의 반투명 구름의 한계점을 극복하기 위해, 본 연구에서는 머신러닝 기법(Random Forest [RF], Convolutional Neural Networks [CNN])을 활용하여 반투명 구름을 중점으로 한 구름탐지 연구를 수행하였다. Reference자료로는 MOderate Resolution Imaging Spectroradiometer (MODIS)에서 제공하는 MOD35자료에서 Cloud Mask와 Cirrus Mask를 활용하였으며 반투명 구름 픽셀을 고려한 모델 훈련을 위해 훈련 데이터의 픽셀 비율을 구름, 반투명 구름, 청천이 약 1:1:1이 되도록 구성하였다. 연구의 정성적 비교 결과, RF와 CNN 모두 반투명 구름을 포함한 다양한 형태의 구름 등을 잘 탐지하였고, RF 모델 결과와 CNN 모델 결과를 혼합한 RF+CNN경우에는 개별 모델의 한계점을 개선시키며 구름탐지가 잘 수행되어진 것을 확인하였다. 연구의 정량적 결과 RF의 전체 정확도(OA) 값은 92%, CNN은 94.11%를 보였고, RF+CNN은 94.29%의 정확도를 보였다.

• 한국정밀공학회:학술대회논문집
• /
• 한국정밀공학회 2011년도 춘계학술대회 논문집
• /
• pp.99-100
• /
• 2011

• 대기
• /
• 제21권2호
• /
• pp.131-142
• /
• 2011

Spectral solar irradiances were observed using a visible and UV Multi-Filter Rotating Shadowband Radiometer on the rooftop of the Science Building at Yonsei University, Seoul ($37.57^{\circ}N$, $126.98^{\circ}E$, 86 m) during one year period in 2006. 1-min measurements of global(total) and diffuse solar irradiances over the solar zenith angle (SZA) ranges from $20^{\circ}$ to $70^{\circ}$ were used to examine the effects of clouds and total optical depth (TOD) on enhancing four solar irradiance components (broadband 395-955 nm, UV channel 304.5 nm, visible channel 495.2 nm, and infrared channel 869.2 nm) together with the sky camera images for the assessment of cloud conditions at the time of each measurement. The obtained clear-sky irradiance measurements were used for empirical model of clear-sky irradiance with the cosine of the solar zenith angle (SZA) as an independent variable. These developed models produce continuous estimates of global and diffuse solar irradiances for clear sky. Then, the clear-sky irradiances are used to estimate the effects of clouds and TOD on the enhancement of surface solar irradiance as a difference between the measured and the estimated clear-sky values. It was found that the enhancements occur at TODs less than 1.0 (i.e. transmissivity greater than 37%) when solar disk was not obscured or obscured by optically thin clouds. Although the TOD is less than 1.0, the probability of the occurrence for the enhancements shows 50~65% depending on four different solar radiation components with the low UV irradiance. The cumulus types such as stratoculmus and altoculumus were found to produce localized enhancement of broadband global solar irradiance of up to 36.0% at TOD of 0.43 under overcast skies (cloud cover 90%) when direct solar beam was unobstructed through the broken clouds. However, those same type clouds were found to attenuate up to 80% of the incoming global solar irradiance at TOD of about 7.0. The maximum global UV enhancement was only 3.8% which is much lower than those of other three solar components because of the light scattering efficiency of cloud drops. It was shown that the most of the enhancements occurred under cloud cover from 40 to 90%. The broadband global enhancement greater than 20% occurred for SZAs ranging from 28 to $62^{\circ}$. The broadband diffuse irradiance has been increased up to 467.8% (TOD 0.34) by clouds. In the case of channel 869.0 nm, the maximum diffuse enhancement was 609.5%. Thus, it is required to measure irradiance for various cloud conditions in order to obtain climatological values, to trace the differences among cloud types, and to eventually estimate the influence on solar irradiance by cloud characteristics.

• 천문학회지
• /
• 제33권2호
• /
• pp.111-121
• /
• 2000

Many models of globular cluster formation assume the presence of cold dense clouds in early universe. Here we re-examine the Fall & Rees (1985) model for formation of proto-globular cluster clouds (PGCCs) via thermal instabilities in a protogalactic halo. We first argue, based on the previous study of two-dimensional numerical simulations of thermally unstable clouds in a stratified halo of galaxy clusters by Real et al. (1991), that under the protogalactic environments only nonlinear (${\delta}{\ge}1$) density inhomogeneities can condense into PGCCs without being disrupted by the buoyancy-driven dynamical instabilities. We then carry out numerical simulations of the collapse of overdense douds in one-dimensional spherical geometry, including self-gravity and radiative cooling down to T = $10^4$ K. Since imprinting of Jeans mass at $10^4$ K is essential to this model, here we focus on the cases where external UV background radiation prevents the formation of $H_2$ molecules and so prevent the cloud from cooling below $10^4$ K. The quantitative results from these simulations can be summarized as follows: 1) Perturbations smaller than $M_{min}\~(10^{5.6}\;M{\bigodot})(nh/0.05cm^{-3})^{-2}$ cool isobarically, where nh is the unperturbed halo density, while perturbations larger than $M_{min}\~(10^8\;M{\bigodot})(nh/0.05cm^{-3})^{-2}$ cool isochorically and thermal instabilities do not operate. On the other hand, intermediate size perturbations ($M_{min} < M_{pgcc} < M_{max}$) are compressed supersonically, accompanied by strong accretion shocks. 2) For supersonically collapsing clouds, the density compression factor after they cool to $T_c = 10^4$ K range $10^{2.5} - 10^6$, while the isobaric compression factor is only $10^{2.5}$. 3) Isobarically collapsed clouds ($M < M_{min}$) are too small to be gravitationally bound. For supersonically collapsing clouds, however, the Jeans mass can be reduced to as small as $10^{5.5}\;M_{\bigodot}(nh/0.05cm^{-3})^{-1/2}$ at the maximum compression owing to the increased density compression. 4) The density profile of simulated PGCCs can be approximated by a constant core with a halo of $p{\infty} r^{-2}$ rather than a singular isothermal sphere.

• 정보보호학회논문지
• /
• 제24권5호
• /
• pp.795-807
• /
• 2014

많은 연구 끝에 VANET의 상용화를 눈앞에 두고 있다. VANET은 차량용 애드혹 네트워크의 약자로서, Cloud와 융합하는 방향으로 연구가 진행되고 있다. 하지만 놀랍게도 VANET 기반 클라우드로 진화한데 가장 큰 역할을 한 것은 차량과 통신기술의 발달이다. 이러한 기술이 확산되는 단계에서 연구자들은 항상 보안과 프라이버시에 대해 고민해 왔다. 게다가 VANET처럼 프라이버시, 익명철회, 경로추적 등 상반된 보안 이슈들이 서로 얽힌 상황은 연구자들을 더욱 고민에 빠지게 했다. 최근 Hussain 등은 VANET 기반 클라우드 프레임워크인 VuC (VANET using Clouds)를 제안하였다. VuC는 VANET과 클라우드가 VANET 사용자(서비스 가입자)에게 서비스를 제공하기 위해 협력하는 환경을 말한다. 본 논문은 Hussain 등이 제안한 VANET 기반 클라우드 프레임워크인 VuC에 초점을 두고 있으며, 특히 앞서 말한 프라이버시, 익명철회, 경로추적에 대한 문제를 다루고 있다. 제안하는 기법은 다중 익명화를 통해 프라이버시를 보호한다. 또한 비컨(Beacon)메시지를 클라우드에 저장하여 경로추적과 익명 철회에 활용한다. 익명철회 권한을 가진 기관들은 연합하여 사용자 노드가 선택한 경로를 특정 시간 동안 추적할 수 있으며, 필요한 경우 신원을 확인할 수 있다. 제안된 기법은 안전하고 조건부 익명성을 보장하며 기존의 기법에 비해 연산량이 적다.

• 천문학회보
• /
• 제40권1호
• /
• pp.58.3-59
• /
• 2015

Dynamical expansion of H II regions plays a key role in dispersing surrounding gas and therefore in limiting the efficiency of star formation in molecular clouds. We use analytic methods and numerical simulations to explore expansions of spherical dusty H II regions, taking into account the effects of direct radiation pressure, gas pressure, and total gravity of the gas and stars. Simulations show that the structure of the ionized zone closely follows Draine (2011)'s static equilibrium model in which radiation pressure acting on gas and dust grains balances the gas pressure gradient. Strong radiation pressure creates a central cavity and a compressed shell at the ionized boundary. We analytically solve for the temporal evolution of a thin shell, finding a good agreement with the numerical experiments. We estimate the minimum star formation efficiency required for a cloud of given mass and size to be destroyed by an HII region expansion. We find that typical giant molecular clouds in the Milky Way can be destroyed by the gas-pressure driven expansion of an H II region, requiring an efficiency of less than a few percent. On the other hand, more dense cluster-forming clouds in starburst environments can be destroyed by the radiation pressure driven expansion, with an efficiency of more than ~30 percent that increases with the mean surface density, independent of the total (gas+stars) mass. The time scale of the expansion is always smaller than the dynamical time scale of the cloud, suggesting that H II regions are likely to be a dominant feedback process in protoclusters before supernova explosions occurs.

• 천문학논총
• /
• 제32권1호
• /
• pp.169-173
• /
• 2017

We provide a new physical insight on the hot molecular clouds near the nucleus of the obscured AGNs. We performed near-infrared spectroscopic observations of heavily obscured AGNs in order to reveal physical characteristics of molecular clouds, especially focused on the CO fundamental ro-vibrational absorption around $4.7{\mu}m$. We have made systematic moderate-resolution spectroscopic observations toward 30 representative (U)LIRGs using the AKARI/IRC, and some of the ULIRGs showed the strong CO absorption feature. For three bright (U)LIRGs that show a steep red continuum with the deep CO absorption feature, IRAS 08572+3915, UGC 05101, and IRAS 01250+2832, we have also made high-resolution spectroscopic observations using the Subaru/IRCS. We have successfully detected many absorption lines up to highly excited rotational levels, and these lines are very deep and extremely broad. The derived physical conditions of molecular clouds are extreme; the gas temperature is as high as several 100 to a 1000 K, the $H_2$ column density is larger than $10^{22}cm^{-2}$, and the gas density is greater than $10^7cm^{-3}$. Such hot and dense molecular clouds must exist around the central engine of the AGN.

• 한국안전학회지
• /
• 제25권5호
• /
• pp.22-26
• /
• 2010

The ignitability(minimum ignition energy, MIE) of a suspended dust clouds is very important aspect of technical safety indices. This paper reported the experimental results dealing with the influence of discharge circuit on the MIE of a suspended dust clouds. The movement of a suspended dust clouds was also observed with the high speed camera. The Hartmann vertical-tube apparatus(MIKE-3) described in the international standard of IEC and Polypropylene (PP, 50% volume-average, D50: $761{\mu}m$) resin powders were used in this experiment. The following results were obtained: (1) the MIE of a suspended PP powder depended markedly on the discharge circuit; in other words, when a resistor was connected in series with the discharge sparking circuit(RC), the lowest value(31mJ) of MIE was obtained for a suspended PP powder comparison with the other circuits(C circuit; 370mJ or LC circuit; 71mJ). (2) the discharge duration time is more important than other factors with regard to MIE of a suspended PP powder.