• 천문학회보
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• 제37권1호
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• pp.88.1-88.1
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• 2012

We observed a surge associated with an Ellerman bomb using the Fast Imaging Solar Spectrograph(FISS) of the New Solar Telescope at Big Bear Solar Observatory. The surge was seen in absorption and varied rapidly both in H alpha and Ca II 8542 line. It originated from the Ellerman bomb, and was impulsively accelerated to 20km/s of the blueshift(upward) motion. Then the gradual change from blueshift of 20km/s to redshift of 40km/s occurred in 20 minutes. Based on the measured line-of-sight velocities, we estimated the material reached up to about 5,000km height. We inferred physical parameters of the surge by adopting the cloud model, and found that the temperature of the surge material was about 25,000K and the non-thermal velocity was about 10km/s. Our results suggest that the surge might be heated intensely after it was ejected from the Ellerman bomb.

• 천문학회보
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• 제36권1호
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• pp.37.2-37.2
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• 2011

Our previous study on tiny pores (R < 2") observed by HINODE/Solar Optical Telescope (SOT) revealed that the plasma in the pores at the photosphere is always moving down and the pores are surrounded by the strong downward motions (highly red-shifted) of neighboring granulations. From this study, we speculated that the flow motions above the pore should be related with the motions at the photosphere, since the pore is strong magnetic field region. Meanwhile, SNU and KASI installed Fast Imaging Solar Spectrograph (FISS) in the Cude room of the 1.6 m New Solar Telescope (NST) at Big Bear Solar Observatory. FISS is a unique system that can do imaging of H-alpha and Ca II 8542 band simultaneously, which is quite suitable for studying of dynamics of chromosphere. To get some clue on the relationship between the photospheric and low-chromospheric motions at the pore region, we took a coordinate observation with NST/FISS and Hinode/SOT for new emerging active region (AR11117) on October 26, 2010. In the observed region, we could find two tiny pores and two small magnetic islands (SMIs), which have similar magnetic flux with the pores but does not look dark. Magnetic flux density and Doppler velocities at the photosphere are estimated by applying the center-of-gravity (COG) method to the HINODE/spectropolarimeter (SP) data. The line-of-sight motions above the photosphere are determined by adopting the bisector method to the wing spectra of Ha and CaII 8542 lines. As results, we found the followings. (1) There are upflow motion on the pores and downflow motion on the SMIs. (2) Towards the CaII 8542 line center, upflow motion decrease and turn to downward motion in pores, while the speed of down flow motion increases in the SMIs. (3) There is oscillating motion above pores and the SMIs, and this motion keep its pattern along the height. (4) As height increase, there is a general tendency of the speed shift to downward on pores and the SMIs. This is more clearly seen on the other regions of stronger magnetic field. In this talk, we will present preliminary understanding of the coupling of pore dynamics between the photosphere and the low-chromosphere.

• 천문학회보
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• 제38권2호
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• pp.86.2-86.2
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• 2013

Ellerman bombs(EBs) are emission features at the wings of the H alpha spectral line. They are believed to be a kind of a magnetic reconnection feature in the low chromosphere or near photosphere. It was previously reported that surges often occur in association with EBs. However, previous observations were restricted to imaging observation. Using Fast Imaging Solar Spectrograph installed in New Solar Telescope at Big Bear Solar Observatory, California, we observed 5 EBs and associated surges with high-spatial and high-spectral resolutions. In this presentation, we will show the results and discuss the physical properties.

• 천문학회보
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• 제38권1호
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• pp.61.2-61.2
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• 2013

We study chromospheric oscillations including umbral flashes and running penumbral waves in a sunspot using scanning spectroscopy in H-alpha and Ca II 8542A, with the Fast Imaging Solar Spectrograph (FISS) at the 1.6 meter New Solar Telescope at Big Bear Solar Observatory. A bisector method is applied to spectral observations to construct chromospheric Doppler velocity maps. Temporal sequence analysis of these shows enhanced high-frequency oscillations inside the sunspot umbra in both lines. Their peak frequency gradually decreases outward from the umbra. The oscillation power is found to be associated with magnetic-field strength and inclination, with different relationships in different frequency bands.

• 한국전자거래학회지
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• 제19권2호
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• pp.109-124
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• 2014

정보보안 인식과 중요성이 시대적으로 고조됨에 따라 각 산업부문별로 조직의 정보자산을 보호하기 위해 정보보호 점검기준을 기반으로 한 정보보호 평가 인증 등의 제도가 마련되어 시행되고 있다. 본 논문은 정보보호 점검기준 간의 문맥적인 유사성과 차이점에 대해 규명하기 위하여 지식네트워크를 이용하여 분석한 결과로 ISMS와 PIMS, 금융 IT부문 경영실태평가, 금융 IT부문 보호업무 모범규준, 정보보안 관리실태 평가 상에 나타난 점검기준간의 관계는 다음과 같이 설명할 수 있다. 첫째, 본 논문에서 연구된 정보보호 점검기준은 공통적으로 정보시스템 및 정보통신망에서의 정보자산의 보호와 침해대응, 운영통제에 관한 부분을 다루고 있다. 둘째, 금융권에서는 앞선 공통부분 외에도 IT 경영 및 감사활동에 관한 적정성을 상대적으로 중요하게 다루고 있다. 셋째, ISMS의 점검기준은 PIMS, 금융 IT부문 경영실태평가, 금융 IT부문 보호업무 모범규준, 정보보안 관리실태 평가의 대부분의 내용을 포함하고 있는 것으로 확인된다.

• 천문학회보
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• 제37권2호
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• pp.112.2-112.2
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• 2012

For the study of fine-scale structure and dynamics in the solar chromosphere, the Fast Imaging Solar Spectrograph (FISS) was installed in 1.6m New Solar Telescope at Big Bear Solar Observatory in 2010. The instrument, installed at a vertical table of the Coude lab, is properly working and producing data for science. From the analysis of the data, however, we noticed that a couple of problems exist that deteriorate image quality : lower light level and poorer resolution of the CaII band data. After several tests, we found that the relay optics at the right position is crucial role for the spatial resolution of raster-scan images. By using resolution target, we re-aligned relay optics and other components of the spectrograph. Here we present the result of optical test and new data taken by the FISS.

• 천문학회보
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• 제43권2호
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• pp.46.1-46.1
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• 2018

The Fast Imaging Solar Spectrograph (FISS) on the Goode Solar Telescope (GST) at Big Bear Solar Observatory is the imaging Echelle spectrograph developed by the Solar Astronomy Group of Seoul National University and the Solar and Space Weather Group of Korea Astronomy and Space Science Institute. The instrument takes spectral data from a region on the Sun in two spectral bands simultaneously. The imaging is done by the organization of intensity data obtained from the fast raster scan of the slit over the field of view. Since the scan repeats many times, the whole set of data can be used to construct the movies of monochromatic intensity at arbitrary wavelengths within the spectral bands, and those of line-of-sight velocity inferred from different spectral lines. So far there are two standard observing configurations: one recording the $H{\alpha}$ line and the Ca II 8542 line simultaneously, and the other recording the Na I D2 line and Fe I 5435 line simultaneously. We have developed the procedures to produce the standard data for each observing configuration. The procedures include the spatial alignment, the correction of spectral shift of instrumental origin, and the lambdameter measurement of the line wavelength. The standard data include the movie of continuum intensity, the movies of intensity and velocity inferred from a chromospheric spectral line, the movies of intensity and velocity inferred from a photospheric line. The processed standard data will be freely available online (fiss.snu.ac.kr) to be used for research and public outreach. Moreover, the IDL procedures will be provided on request as well so that each researcher can adapt the programs for their own research.

• 생태와환경
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• 제56권3호
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• pp.187-195
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• 2023

영산강의 상류에는 4개의 농업용 댐들이 축조되어 있으며 각 댐의 물은 경작지 관개용수로 거의 모두 공급되고 영산강 본류로 방류되지 않고 있다. 또한, 관개용수의 대부분도 사용 후에 영산강으로 회귀하지 않고 격리된 상태의 별도 용수간선을 통하여 영산강 하류까지 흘러가기 때문에 영산강 본류의 유량 부족 문제를 가중시키고 있다. 이러한 원인으로 영산강 유량의 71%가 하수처리수로 채워지는 결과를 초래하였으며 이에 따라 수질뿐 아니라 수생태 건강성도 우리나라 4대강 중 가장 열악한 실정이다. 따라서 본 연구에서는 영산강 수질개선을 위한 여러 가지 시나리오들을 오염삭감과 유량증대를 함께 고려하여 개발하였고 QUAL-MEV를 이용하여 각 시나리오의 장래수질을 예측·분석하였으며, 이러한 연구결과로부터 얻어진 결론은 다음과 같다. 1. 영산강의 수질개선은 오염삭감을 통해 그동안 꾸준히 시행되어 왔으나 이제 한계에 다다르고 있어 앞으로는 오염삭감만이 아니라 유량증대(해수담수화 포함) 방법이 함께 중점 추진되어야 하며, 이러한 경우에는 영산강 수질목표의 달성도 가능하다. 2. BOD는 오염삭감 그리고 T-P는 유량증대의 방법을 통해 크게 개선될 수 있다고 예측되었으므로 수질목표의 달성을 위해 오염삭감과 더불어 유량증대가 함께 도입된다면 이들 상호 간에는 시너지 효과가 크게 작용할 수 있을 것이다. 3. 그러나 유량증대사업의 원활한 추진을 위해서는 투자비용을 늘리는 것도 중요하겠으나 기존의 용수 이해관계자들간에 형성되어 있는 갈등 문제를 협의·해소키 위한 꾸준한 노력이 선행되어야 할 것이다. 4. 댐의 건설, 용수배분 조정 등 강우 유관형 유량증대 방법은 기후변화로 인해 강우가 오랜 기간 발생하지 않으면서 대가뭄이 지속될 경우에 적용의 효용성이 떨어지거나 상실될 수 있으므로 앞으로 비슷한 조건이라면 강우 무관형인 해수담수화시설을 유량증대사업 중 우선 설치대상으로 고려해야 할 것이다. 그 이유는 이러한 시설이 우리나라에서 새로 건설하기 어려운 댐의 용수확보 기능을 대체할 수 있고 대가뭄이 장기간 지속될 경우에 물관련 재해방지도 가능하여 기후변화의 적응시설로서 유용할 수 있기 때문이다.

• 천문학회보
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• 제40권1호
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• pp.83.4-84
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• 2015

We report that a strong downflow event caused three-minute oscillations in the solar atmosphere. Our observations were carried out by using the Fast Imaging Solar Spectrograph (FISS) of the 1.6 meter New Solar Telescope (NST) and the Interface Region Imaging Spectrograph (IRIS). Our main findings are as follows: (1) The strong downflow was seen at the $H{\alpha}$ absorption line at first, and then appeared at the Si IV and C II emission lines. It seems that the characteristics of the downflow are consistent with a coronal rain event. (2) After the event, oscillations of velocity were identified in the chromospheric lines and transition region lines. (3) The amplitudes of oscillations were 2km/s at Mg II line and 3km/s at C II and Si IV lines and decreased with time. (4) The period of the oscillation was 2.67 minutes at first, but gradually increased with time. Our findings are in agreement with Chae & Goode (2015)'s theory that of acoustic waves generated by a disturbance in a gravitationally-stratified medium.

• 천문학회보
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• 제38권2호
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• pp.87.1-87.1
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• 2013

Ellerman bombs(EB) are small-scale bright features observed best in the wings of H alpha line. We used the Fast Imaging Solar Spectrograph(FISS) with the 1.6m New Solar Telescope at Big Bear Solar Observatory, in order to investigate characteristics of each EB. We analyzed H alpha line profiles of EBs, and classified EBs by their contrast profiles. To analyse characteristics of EBs, we applied power-law fitting ($C={\alpha}{\Delta}{\lambda}^{-n}$) to the EB contrast profiles. The amplitude ${\alpha}$ is a measure of the strength of an EB event (or the amount of released energy), and the power-law index n is a measure of spatial concentration of energy in the higher layers of the solar atmosphere. With the two parameters, we classified EBs into a few groups. We try to understand the physical properties of each group.