• 천문학회보
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• 제35권1호
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• pp.58.2-58.2
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• 2010

L1251B, which was revealed as a small group of protostars by the Spitzer Space Telescope (SST), presents a great site of studying chemical evolution in gas and ice as well as various dynamical processes associated with star formation (infall, rotation, and outflow). We have mapped L1251B with the Infrared Spectrograph (IRS) aboard the SST to study the chemical distribution in the phases of gas and ice and the dynamical feature related to shock in the region. Various atomic lines and the $H_2$ pure rotational lines, which trace different shock velocities, were detected. In addition, the distribution of the water and $CO_2$ ices hints variety of the ice desorption mechanism in L1251B.

• 천문학회보
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• 제46권1호
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• pp.57.1-57.1
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• 2021

The icy mantles of interstellar grains are developed by the freeze-out of interstellar molecules and atoms onto grain surfaces. The ice molecules become more complex by surface chemistry induced directly by high energy photons or by the thermal energy diffused over heated grain surface. Therefore, the ice composition is an important tracer of physical conditions where the ices form. Ices have been studied via their absorption features against continuum sources, such as young stellar objects or evolved background stars, in infrared wavelengths. The Spitzer IRS was the most sensitive spectrometer for the observations of infrared ice absorption features. We has been developing an automated analysis tool for the Spitzer IRS spectra, especially for the 15 ㎛ CO₂ bending mode. The 15 ㎛ CO₂ absorption feature is very useful for the study of accretion process in star formation since its spectral shape varies with thermal condition of the dust grains. Eventually, this tool will cover the whole range of the Spitzer IRS spectrum (5~20 ㎛).

• Ocean and Polar Research
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• 제44권4호
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• pp.269-285
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• 2022

The interaction between ocean and ice shelf is a critical physical process in relation to water mass transformations and ice shelf melting/freezing at the ocean-ice interface. However, it remains challenging to thoroughly understand the process due to a lack of observational data with respect to ice shelf cavities. This is the first study to simulate the variability and circulation of water mass both overlying the continental shelf and underneath an ice shelf and an ice tongue in the Terra Nova Bay (TNB), East Antarctica. To explore the properties of water mass and circulation patterns in the TNB and the corresponding effects on sub ice shelf basal melting, we explicitly incorporate the dynamic-thermodynamic processes acting on the ice shelf in the Regional Ocean Modeling System. The simulated water mass formation and circulation in the TNB region agree well with previous studies. The model results show that the TNB circulation is dominated by the geostrophic currents driven by lateral density gradients induced by the releasing of brine or freshwater at the polynya of the TNB. Meanwhile, the circulation dynamics in the cavity under the Nansen Ice shelf (NIS) are different from those in the TNB. The gravity-driven bottom current induced by High Salinity Shelf Water (HSSW) formed at the TNB polynya flows towards the grounding line, and the buoyance-driven flow associated with glacial meltwater generated by the HSSW emerges from the cavity along the ice base. Both current systems compose the thermohaline overturning circulation in the NIS cavity. This study estimates the NIS basal melting rate to be 0.98 m/a, which is comparable to the previously observed melt rate. However, the melting rate shows a significant variation in space and time.

• Food Science and Biotechnology
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• 제17권1호
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• pp.102-105
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• 2008

The freezing patterns of commercial frozen foods were characterized by using proton nuclear magnetic resonance ($^1H$ NMR) relaxometry and differential scanning calorimetry (DSC). The liquid-like components like unfrozen water were investigated as a function of temperature (10 to $-40^{\circ}C$) and then compared with the unfrozen water content measured by DSC. The formation of ice crystals and the reduction of water in the foods during freezing were readily observed as a loss of the NMR signal intensity. The proton NMR relaxation measurement showed that the decreasing pattern of the liquid-like components varied depending on the samples even though they exhibited the same onset temperature of ice formation at around $0^{\circ}C$. When compared with the unfrozen water content obtained by the DSC, the NMR and DSC results could be closely correlated at the temperature above $-20^{\circ}C$. However, the distinct divergence in the values between 2 methods was observed with further decreasing temperatures probably due to the solid glass formation which was not detected by DSC.

• 천문학논총
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• 제32권1호
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• pp.105-107
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• 2017

We present results of AKARI/IRC near-infrared (NIR) slit-spectroscopy ($2.5-5.0{\mu}m$, R ~ 100) of Galactic sources, focusing on ice absorption features. We investigate the abundance of $H_2O$ and $CO_2$ ices and other ice species (CO and XCN ices) along lines of sight towards Galactic H $\small{II}$ regions, massive YSOs, and infrared diffuse sources. Even among those different kinds of astronomical objects, the abundance ratio of $CO_2$ to $H_2O$ ices does not vary significantly, suggesting that the pathway to $CO_2$ ice formation driven by UV irradiation is not effective at least among the present targets.

• 천문학회보
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• 제44권2호
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• pp.49.2-49.2
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• 2019

We present results from our long-term observing campaign, using the NASA IRTF at Maunakea, to obtain 2 - 4 ㎛ spectra of 118 red point sources in the line of sight to the Galactic Center (GC). Our sample is largely composed of point sources selected from near- and mid-infrared photometry, but also includes a number of massive young stellar objects. Many of these sources show high foreground extinction as shown by deep 3.4 ㎛ aliphatic hydrocarbon absorption feature, which is a characteristic of the diffuse ISM and comes from the long line of sight through the diffuse medium toward the Central Molecular Zone (CMZ), the central 300 pc region of the GC. The deep 3.1 ㎛ H₂O ice absorption band coming from the local, dense material in the GC CMZ suggests that most sources are likely located in the GC CMZ. A few of these sources show weak CCH₃OH ice absorption at 3.535 ㎛, which can provide a strong constraint on the CCH₃OH ice formation in the unique environment of the CMZ. From the best-fitting models, the optical depths of these features are determined and used to generate a well-rounded view of the ice composition across the GC CMZ and the spectral characteristics of massive YSOs in the GC.

• 대기
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• 제22권1호
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• pp.73-85
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• 2012

The collision efficiency data for collision between graupel or hail particles and cloud drops that take into account the differences of particle density are applied to the Takahashi cloud model. The original setting assumes that graupel or hail collision efficiency is the same as that of the cloud drops of the same volume. The Takahashi cloud model is run with the new collision efficiency data and the results are compared with those with the original. As an initial condition, a thermodynamic profile that can initiate strong convection is provided. Three different CCN concentration values and therefore three initial cloud drop spectra are prescribed that represent maritime (CCN concentration = 300 $cm^{-3}$), continental (1000 $cm^{-3}$) and extreme continental (5000 $cm^{-3}$) air masses to examine the aerosol effects on cloud and precipitation development. Increase of CCN concentration causes cloud drop sizes to decrease and cloud drop concentrations to increase. However, the concentration of ice particles decreases with the increase of CCN concentration because small drops are difficult to freeze. These general trends are well captured by both model runs (one with the new collision efficiency data and the other with the original) but there are significant differences: with the new data, the development of cloud and raindrop formation are delayed by (1) decrease of ice collision efficiency, (2) decrease of latent heat from riming process and (3) decrease of ice crystals generated by ice multiplication. These results indicate that the model run with the original collision efficiency data overestimates precipitation rates.

• 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.

• 대한원격탐사학회지
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• 제39권6_2호
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• pp.1651-1669
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• 2023

해빙(sea ice)은 현재 전 세계 해양 면적의 약 7%를 차지하고 있으며 계절적, 연간 변화를 보이고 주로 극지방과 고위도 지역에 나타난다. 해빙은 대규모 공간 규모에서 다양한 종류로 형성되며 석유 및 가스탐사, 기타 해양활동이 급속히 증가하는 발해해는 해양 구조물 피해 및 해상 운송, 해양 생태계에 심각한 영향을 미치기 때문에 시계열 모니터링을 통해 해빙의 면적 및 유형 분류를 분석하는 것이 매우 중요하다. 현재 고해상도 위성영상 및 현장 실측 자료를 바탕으로 해빙의 종류 및 영역에 대한 연구가 진행되고 있지만 현장 실측자료를 획득하여 해빙 모니터링에는 한계가 있다. 고해상도 광학 위성영상은 광범위에서 해빙의 유형을 육안으로 탐지하고 식별할 수 있고, 짧은 시간해상도를 갖는 해양위성인 천리안 2B호(Geostationary Ocean Color Imager-II, GOCI-II)를 이용하여 해빙 모니터링의 공백을 보완할 수 있다. 이 연구에서는 고해상도 광학위성영상을 이용하여 생산된 학습자료를 기반으로 규칙기반 기계학습 모델을 훈련시키고 이를 GOCI-II 영상에서 탐지를 수행함으로써, 해빙 모니터링 활용 가능성을 알아보고자 하였다. 학습 자료는 발해(Bohai Sea)의 2021-2022년 랴오둥만(Liaodong Bay)을 대상으로 추출하였으며, GOCI-II를 활용한 Random Forest (RF) 모델을 구축하여 기존 normalized difference snow index (NDSI) 지수 기반 및 고해상도 위성영상에서 획득된 해빙 영역과 정성적 및 정량적 비교 분석하였다. 본 연구 결과 해빙의 영역을 과소평가한 NDSI 지수 기반 결과와 달리 비교적 자세한 해빙 영역을 탐지하였으며 유형별 해빙을 분류할 수 있어 해빙 모니터링이 가능함을 확인하였다. 향후 지속적인 학습 자료 및 해빙형성에 영향인자 구축을 통해 탐지 모델의 정확도를 향상시킨다면 고위도 해양 지역에서 해빙 모니터링 분야에 활용할 수 있을 것으로 기대된다.

• 한국식품과학회지
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• 제27권5호
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• pp.783-788
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• 1995

본 연구는 동결속도 및 동결저장온도가 취반된 쌀의 이화학적 특성에 미치는 영향을 살펴보고자, 단열재를 이용하여 최대 빙결정 형성신간이 3시간, 5시간, 7시간 그리고 12시간인 동결속도로 24시간 동안 동결하였고, 동결된 시료는 각각 $-20^{\circ}C$와 $-70^{\circ}C$의 냉동고에서 3개월간 저장하여 동결저장동안에 각 시료의 노화도 그리고 조직감의 변화를 조사하였다. 동결된 쌀밥의 미세구조 및 표면구조는 빙결정을 동결치환에 의해 제거한후 scanning electron microscopy(SEM)으로 관찰하였다. 취반된 쌀의 노화도는 동결속도, 동결저장온도, 저장기간에 따라 큰 영향을 받아 최대 빙결정 형성시간이 3시간에서 12시간으로 길어짐에 따라 노화도는 14.85%에서 40.00%로 증가하였고, 동결된 쌀밥의 동결저장 중 노화도는 $-20^{\circ}C$에서 저장한 것이 $-70^{\circ}C$의 경우보다 노화된 정도로 크고, 빠른 진행을 보였다. 동결된 시료를 해동한 후의 경도는 동결시키지 않은 대조구와 비교할 때 크게 증가하였으며, 또한 동결속도가 늦어질수록 더 큰 증가를 보였다. 하지만, 3개월간 저장한 후에는 경도가 다시 감소하였다. 한편, 부착성은 대조구와 비교하여 24시간 동안 동결된 쌀밥에서는 감소하였으며 3개월간 저장한 후에는 다시 증가하는 경향을 보였다. 동결된 취반된 쌀의 빙결정의 크기는 동결속도가 늦어짐에 따라 커졌고 그 수는 상대적으로 적었다. 또한 3개월간 저장한 후에는 얼음의 재결정화에 의해 시료의 빙결정은 더욱 커져 취반된 쌀의 구조가 많이 파손되었음을 확인할 수 있었다. 결론적으로 최대빙결정형성시간을 단축하여 취반된 쌀을 동결시키는 것과 낮은 온도에서 저장하는 것이 빙결정의 형성과 성장에 따른 전분의 노화와 조직감의 변화를 억제할 수 있다고 판단되었다.