• 천문학회보
• /
• 제36권1호
• /
• pp.35.2-35.2
• /
• 2011

We have investigated a coronal jet near the limb on 2010 June 27 by Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), SDO/Atmospheric Imaging Assembly (AIA), and STEREO. From EUV (AIA and EIS) and soft X-ray (XRT) images we identify the erupting jet feature in cool and hot temperatures. Using the high temporal and multi wavelength AIA images, we found that the hot jet preceded its associated cool jet and their structures are well consistent with the numerical simulation of the emerging flux-reconnection model. From the spectroscopic analysis, we found that the jet structure changes from blue shift to red one with time, which may indicate the helical structure of the jet. The STEREO observation, which enables us to observe this jet on the disk, shows that there was a dim loop associated with the jet. On the other hand, we found that the structure of its associated active region seen in STEREO is similar to that in AIA observed 5 days before. Based on this fact, we compared the jet morphology on the limb with the magnectic fields extrapolated from a HMI vector magnetogram of this active region observed on the disk. Interestingly, the comparison shows that the open and closed magnetic field configuration correspond to the jet and the dim loop, respectively, as the Shibata's jet model predicted.

• 지질공학
• /
• 제30권3호
• /
• pp.315-325
• /
• 2020

이 연구는 도로 비탈면에서 발생하는 산사태의 확률론적 예측에 기반된 산사태 발생에 영향을 미치는 인자의 중요도 산정 및 예측 모델을 개발하는 것이다. 산사태 예측 모델을 개발하기 위해 한반도 전 지역을 대상으로 2007년부터 2020년까지 조사된 30,615사면의 현장조사 자료를 활용하였다. 전체 131개의 변수 인자 중 지형인자 17개, 지질인자 114개(기반암 89개를 포함), 도로와의 이격거리를 사용하였다. 산사태 발생에 영향을 미치는 인자를 자동화된 머신러닝인 AutoML을 실시하여 예측 성능이 뛰어난 XRT(extremely randomized trees)를 선정하였다. 변수 중요도 분석결과 지형적 요인 10개, 지질인자 9개, 사회적 영향성인 도로와의 이격 거리와 관련된 항목순으로 급경사지 불안정에 가장 많은 영향을 주는 것으로 분석되었다. 개발된 모델의 신뢰성 검증을 수행한 결과 AUC 83.977%의 예측율을 확보한 것으로 나타났다. 이 모델은 산사태 이력을 기반으로 한 현장조사 자료만을 이용하여 변수 중요도의 순위를 도출함으로써 그에 따른 산사태 발생 가능성을 확률적 및 정량적으로 평가하였다. 향후 의사 결정자들에게 현장조사를 통한 사면진단 안전평가 시 신뢰성 있는 근거를 제공하리라 판단된다.

• Radiation Oncology Journal
• /
• 제5권2호
• /
• pp.111-117
• /
• 1987

암 환자에 있어서 영양상태는 치료에 대한 반응과 생존기간에 영향을 미치는 인자가 된다. 그래서 연하곤란은 암 환자에 중요한 영향을 끼친다고 할 수 있다. 저자들은 1983년 3월부터 1987년 3월까지 가톨릭의대 강남성모병원 방사선치료실에서 방사선 치료를 받은 1,400명의 환자 중 연하곤란 및 호흡기계 문제로 방사선 치료를 받았던 식도암 이외의 암에 의한 식도의 헙착 및 폐쇄를 일으킨 환자 16예를 대상으로 이들의 특성과 식도의 협착 및 폐쇄에 대한 방사선 치로의 효과 및 생존기간을 후향성으로 분석하여 보았다. 1. 방사선치료를 받은 환자 중 빈도는 $1\%$이었다. 2. 가장 빈번한 원인은 폐암 (14/16)이었고, 식도 중부 (14/16)가 가장 흔하게 침범되는 부위였다. 3. 방사선 치료에 대한 반응은 연하곤란의 정도와 2주 간격으로 촬영한 바륨조영사진으로 평가하였는데 계획된 방사선 치료를 종료한 환자들의 $80\%$(8/10)에서 반응을 보였다. 4. 반응이 시작되는 선량은 1,000cGy-6,010cGy의 범위에 들어 있으며 중앙치는 2,880cGy였고 평균치는 2,993 cGy였다. 5. Kaplan-Meier 방식에 의한 15주와 30주 생존율은 전예에서는 $60\%$와 $46\%$였고 계획된 방사선 치료를 종료한 환자들에서는 $77\%$와 $51\%$였다. 6. 4예에서는 연하곤란의 재발 없이 90주 이상 생존하고 있다.

• 천문학회보
• /
• 제32권1호
• /
• pp.33.1-33.1
• /
• 2007

• 천문학회보
• /
• 제37권1호
• /
• pp.89.1-89.1
• /
• 2012

We have investigated a coronal jet observed near the limb on 2010 June 27 by the Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), and Solar Optical Telescope (SOT), and the SDO/Atmospheric Imaging Assembly (AIA), Helioseismic and Magnetic Imager (HMI), and on the disk by STEREO-A/EUVI. From EUV (AIA and EIS) and soft X-ray (XRT) images we have identified both cool and hot jets. There was a small loop eruption in Ca II images of the SOT before the jet eruption. Using high temporal and multi wavelength AIA images, we found that the hot jet preceded its associated cool jet by about 2 minutes. The cool jet showed helical-like structures during the rising period. According to the spectroscopic analysis, the jet's emission changed from blue to red shift with time, implying helical motions in the jet. The STEREO observation, which enabled us to observe the jet projected against the disk, showed that there was a dim loop associated with the jet. We have measured a propagation speed of ~800 km/s for the dimming front. This is comparable to the Alfven speed in the loop computed from a magnetic field extrapolation of the HMI photospheric field measured 5 days earlier and the loop densities obtained from EIS Fe XIV line ratios. We interpret the dimming as indicating the presence of Alfvenic waves initiated by reconnection in the upper chromosphere.

• 천문학회보
• /
• 제43권1호
• /
• pp.53.1-53.1
• /
• 2018

During a major solar eruption, the erupting plasma is possibly out of the equilibrium ionization state because of its rapid heating or cooling. The non-equilibrium ionization process is important in a rapidly evolving system where the thermodynamical time scale is shorter than the ionization or recombination time scales. We investigate the effects of non-equilibrium ionization on EUV and X-ray observations by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamic Observatory and X-ray Telescope (XRT) on board Hinode. For the investigation, first, we find the emissivities for all the lines of ions of elements using CHIANTI 8.07, and then we find the temperature responses multiplying the emissivities by the effective area for each AIA and XRT passband. Second, we obtain the ion fractions using a time-dependent ionization model (Shen et al. 2015), which uses an eigenvalue method, for all the lines of ion, as a function of temperature, and a characteristic time scale, $n_et$, where $n_e$ and t are density and time, respectively. Lastly, the ion fractions are multiplied to the temperature response for each passband, which results in a 2D grid for each combination of temperature and the characteristic time scale. This is the set of passband responses for plasma that is rapidly ionized in a current sheet or a shock. We investigate an observed event which has a relatively large uncertainty in an analysis using a differential emission measure method assuming equilibrium ionization state. We verify whether the observed coronal plasmas are in non-equilibrium or equilibrium ionization state using the passband responses.

• 천문학회보
• /
• 제40권1호
• /
• pp.85.1-85.1
• /
• 2015

We investigate the mass and energy of erupting plasma observed in X-rays and EUV, which is associated with a coronal mass ejection (CME) and an X-class flare. The erupting plasma was observed by both the X-ray telescope (XRT) on Hinode and the Atmospheric Imaging Assembly (AIA) on Solar Dynamic Observatory (SDO). We estimate the emission measures of the erupting plasma using a differential emission measure method. The plasma erupts with a loop-like structure in X-ray and EUV. We estimate the mass of erupting plasma assuming a cylinder structure. In addition, we estimate the radiative loss, thermal conduction, thermal, and kinetic energies of the eruptive hot plasma. We find that the thermal conduction timescale is much shorter than the duration of the eruption. This result implies that additional heating during the eruption may be required to explain the hot plasma observations in X-rays.

• 천문학회보
• /
• 제40권2호
• /
• pp.51.3-52
• /
• 2015

Gamma-Ray Bursts(GRBs) are the most violent event in the universe, whose detection rate is a few in a day. The spectral lag, which is commonly observed in the observed light curves of GRBs, is a difference in arrival times of the high-energy and low-energy photons. The relation between the spectral lag and the luminosity of the observed GRBs is shown to be anti-correlated in previous studies. In reported relations to date, the isotropic luminosity has been assumed. On the other hand, GRBs are likely to emit its energy through a beamed jet. In this study, we attempt to obtain the relation between the spectral lag and the collimation-corrected luminosity. We have calculated collimation-corrected luminosities and opening angles using the observed light curves taken from a database of Swift/BAT, XRT. We expect to increase its significance level by expanding a sample size compared with those previously analyzed.

• 천문학회보
• /
• 제37권2호
• /
• pp.131.1-131.1
• /
• 2012

We use three-dimensional magnetohydrodynamic (MHD) simulations of flux emergence from solar subsurface to corona. In our previous work, we reported the relation between magnetic-field configuration and the flux expansion factor. Following these results, we investigate where an upflow is generated in an active region and how its location is related to the flux expansion factor. We also derive physical quantities of a real active region from observation data provided by Nobeyama Radioheliograph (NoRH), X-Ray Telescope (XRT), and Extreme Ultraviolet Imaging Spectrometer (EIS) onboard Hinode. These physical quantities are plasma density, temperature and flow. By comparing the simulation result and observational one, we will discuss the properties of the location producing a solar wind.

• 천문학회보
• /
• 제36권1호
• /
• pp.39.1-39.1
• /
• 2011

Coronal mass ejection (CME) plasmas have been observed in EUV and X-ray passbands as well as in white light. Mass of CME has been determined using polarized brightness observed by the Large Angle and Spectrometric Coronagraph Experiment (LASCO) on board Solar and Heliospheric Observatory (SOHO). Therefore, this mass obtained from the LASCO observation indicates the total CME mass. However, the mass of CME plasma in different temperatures can be determined in EUV and X-ray passbands using observations by SOHO/EIT, STEREO/EUVI, and Hinode/XRT. Prominence/CME plasmas have been observed as absorption or emission features in EUV and X-ray passbands. The absorption features provide a lower limit to cold mass. In addition, the emission features provide an upper limit to the mass of plasmas in temperature ranges of EUV and X-ray. We determine the mass constraints using the emission measure obtained by assuming the prominence/CME structures. This work will address the mass constraints of hot and cold plasmas in CMEs, comparing to total CME mass.