• 지구물리
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• 제7권3호
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• pp.207-215
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• 2004

오호츠크해는 동해와 연결된 바다로 세계에서 가장 유망한 가스하이드레이트 부존지역 중 하나이다 오호츠크해의 가스하이드레이트 퇴적층의 지구물리 구조를 규명하기 위해 2003년 8월과 10월 두차례에 걸처 사할린 북동 대륙사면지역에서 오호츠크해 가스하이드레이트 국제공동연구(CHAOS) 탐사가 수행되었다. 이번 탐사에서는 고해상도 천부지층 탄성파 수중음향(hydroacoustic) 자료 등을 획득하였다. 스파커 음원을 이용하여 얻은 탄성파 단면도에는 가스하이드레이트 BSR이 뚜렷하지 않지만 BSR 깊이 부근에 분산적으로 나타나는 진폭이 강화된 반사층들이 관찰되었다. 따라서 사용하는 음원의 주파수에 따라 BSR의 반사특성이 다르게 나타남을 알 수 있다. 또한 BSR깊이에서 해저면으로 상승한 좁은 폭의 가스기둥 (gas chimney)들이 다수 발견되었다. 이 기둥들은 내부음향특성이 전혀 보이지 않는 (wipe-out : WO)그룹과 주변에 비해 상대적으로 강한 반사특성(enhanced reflection; ER)을 보이는 그룹으로 나누어진다. 이런 반사특성 차이는 기둥내에 가스 또는 가스하이드레이트 중 어떤 물질이 집중적으로 충적되었는지에 따라 구별되는 현상으로 해석된다. 수중음향자료에는 지층으로부터 해수중으로 수백 의 높이까지 뿜어져 오르는 많은 가스분출기둥들이 관찰되었다. 가스분출기둥들은 가스하이드레이트 안정영역에 해당하는 상대적으로 깊은 수심에서 관찰된다. 이는 지층의 가스기둥 주변을 둘러싼 가스하이드레이트 퇴적층이 가스가 스며들지 못하는 차단벽을 형성하면서 심부에서 공급되는 가스의 대부분이 가스기둥을 따라 해저면까지 운반되며 이에 따라 가스기둥 위의 표층에서 해수중으로 분출하는 가스분출기둥이 형성된다.

• Asian Pacific Journal of Cancer Prevention
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• 제15권7호
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• pp.3151-3156
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• 2014

Background: Sorafenib is a promising drug for advanced hepatocellular carcinoma (HCC); however, treatment may be discontinued for multiple reasons, such as progressive disease, adverse events, or the cost of treatment. The consequences of sorafenib discontinuation and continuation are uncertain. Materials and Methods: We retrospectively analyzed 88 HCC patients treated with sorafenib from July 2007 to January 2013. Overall survival (OS), post-disease progression overall survival (pOS), and time to disease progression (TTP) were compared for survival analysis. Cox proportional hazard regression was performed to assess the effect of important factors on OS in the overall patient population and on pOS in patients who continued sorafenib treatment. Results: Sorafenib was discontinued and continued in 24 and 64 patients, respectively. The median OS (355 vs 517 days respectively; p=0.015) and median post-PD OS (260 vs 317 days, respectively; p=0.020) were statistically different between the discontinuation and continuation groups. Neither the median time to first PD nor the time to second PD were significantly different between the 2 groups. In the discontinuation group, 3 of the 24 patients (12.5%) suffered disease outbreaks. In Cox proportional hazard regression analysis after correction for confounding factors, BCLC stage (p=0.002) and PD site (p=0.024) were significantly correlated with pOS in patients who continued sorafenib treatment. Conclusions: Sorafenib discontinuation may cause HCC flares or outbreaks. It is advisable to continue sorafenib treatment after first PD, particularly in patients with Barcelona Clinic Liver Cancer stage B disease or only intrahepatic PD.

• 한국항해항만학회:학술대회논문집
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• 한국항해항만학회 2011년도 춘계학술대회
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• pp.27-28
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• 2011

태양 흑점수의 증감주기 (약 11년)에 따른 태양폭발 (태양에서의 플레어 현상)은 태양 코로나 물질을 대방출하는 태양폭풍을 야기한다. 미국해양대기청 (NOAA: National Oceanic and Atmospheric Administration)은 태양 흑점활동이 2013년과 2014년 사이에 극대화 될 것이라고 예상했다. 강력한 태양폭풍의 영향이 지구에 미쳤을 경우 인공위성을 이용한 전세계 측위시스템의 교란, 각종 통신수단 및 TV, 라디오 방송 등이 영향을 받을 것으로 예상된다. 실제로 1989년 태양폭풍은 캐나다에서 정전사태를 일으켜 9시간동안 약 600만명이 정전으로 인한 피해를 입은 사례가 있다. 이와 같은 초강력 태양폭풍은 인공위성의 수명을 약 5~10년정도 단축시켰으며 이로 인한 경제적 손실 및 파급효과를 고려하면 액수는 수십조 원에 달할 것으로 예상된다. 최근 2011년 2월 15일 10시 45분경 (지역시)에 발생했던 X급 태양폭발에 의해 발생한 태양폭풍의 영향이 2011년 2월 18일 오전 10시 30분경 우리나라 (보현산 관측소)에서 관측되었다. 본 논문에서는 현재 흑점수가 증가하고 있는 시점에서 2월 18일의 태양폭발 일주일 전후 자기장 데이터를 비교하고, 또한 대전에서 관측한 RINEX 데이터를 이용하여 측위결과를 비교 분석하였다. 태양폭풍이 지구에 도달한 2011년 2월 18일의 자기장 관측 값은 일주일 전후 데이터와 비교하여 Proton이 요동하는 결과를 보였고, 대전지역에서의 측위결과도 태양폭풍 일주일 전후와 비교하여 최대 1m이상의 측위오차를 보였다.

• 천문학논총
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• 제30권2호
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• pp.559-563
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• 2015

Monitor of All-sky X-ray Image (MAXI) is a Japanese X-ray all-sky surveyer mounted on the International Space Station (ISS). It has been scanning the whole sky since 2009 during every 92-minute ISS rotation. X-ray transients are quickly found by the real-time nova-search program. As a result, MAXI has issued 133 Astronomer's Telegrams and 44 Gamma-ray burst Coordinated Networks so far. MAXI has discovered six new black holes (BH) in 4.5 years. Long-term behaviors of the MAXI BHs can be classified into two types by their outbursts; a fast-rise exponential-decay type and a fast-rise flat-top one. The slit camera is suitable for accumulating data over a long time. MAXI issued a 37-month catalog containing 500 sources above a ~0.6 mCrab detection limit at 4-10 keV in the region ${\mid}{b}{\mid}$ > $10^{\circ}$. The SSC instrument utilizing an X-ray CCD has detected diffuse soft X-rays extending over a large solid angle, such as the Cygnus super bubble. MAXI/SSC has also detcted a Ne emission line from the rapid soft X-ray nova MAXI J0158-744. The overall shapes of outbursts in Be X-ray binaries (BeXRB) are precisely observed with MAXI/GSC. BeXRB have two kinds of outbursts, a normal outburst and a giant one. The peak dates of the subsequent giant outbursts of A0535+26 repeated with a different period than the orbital one. The Be stellar disk is considered to either have a precession motion or a distorted shape. The long-term behaviors of low-mass X-ray binaries (LMXB) containing weakly magnetized neutron stars are investigated. Transient LMXBs (Aql X-1 and 4U 1608-52) repeated outbursts every 200-1000 days, which is understood by the limit-cycle of hydrogen ionization states in the outer accretion disk. A third state (very dim state) in Aql X-1 and 4U 1608-52 was interpreted as the propeller effect in the unified picture of LMXB. Cir X-1 is a peculiar source in the sense that its long-term behavior is not like typical LMXBs. The luminosity sometimes decreases suddenly at periastron. It might be explained by the stripping of the outer accretion disk by a clumpy stellar wind. MAXI observed 64 large flares from 22 active stars (RS CVns, dMe stars, Argol types, young stellar objects) over 4 years. The total energies are $10^{34}-10^{36}$ erg $s^{-1}$. Since MAXI can measure the spectrum (temperature and emission measure), we can estimate the size of the plasma and the magnetic fields. The size sometimes exceeds the size of the star. The magnetic field is in the range of 10-100 gauss, which is a typical value for solar flares.

• 한국항해항만학회지
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• 제35권6호
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• pp.477-482
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• 2011

태양 흑점수의 증감주기 (약 11년)에 따른 태양폭발 (태양에서의 플레어 현상)은 태양 코로나 물질을 대방출하는 태양폭풍을 야기한다. 미국해양대기청 (NOAA: National Oceanic and Atmospheric Administration)은 태양 흑점활동이 2013년과 2014년 사이에 극대화 될 것이라고 예상했다. 강력한 태양폭풍의 영향이 지구에 미쳤을 경우 인공위성을 이용한 전 세계 측위시스템의 교란, 각종 통신수단 및 TV, 라디오 방송 등이 영향을 받을 것으로 예상된다. 실제로 1989년 태양폭풍은 캐나다에서 정전사태를 일으켜 9시간동안 약 600만 명이 정전으로 인한 피해를 입은 사례가 있다. 이와 같은 초강력 태양폭풍은 인공위성의 수명을 약 5~10년 정도 단축시키며 이로 인한 경제적 손실 및 파급효과를 고려하면 액수는 수십조 원에 달할 것으로 예상된다. 최근 2011년 2월 15일 10시 45분경 (01:30 - UTC)에 발생했던 X급 태양폭발에 의해 발생한 태양폭풍의 영향이 2011년 2월 18일 오전 10시 30분경 우리나라 (보현산 관측소)에서 관측되었다. 본 논문에서는 현재 흑점수가 증가하고 있는 시점에서 2월 18일의 태양폭발 일주일 전후 지자기 데이터를 비교하고, 또한 대전과 서울지역에서 관측한 RINEX 데이터를 이용하여 측위결과를 비교 분석하였다. 태양폭풍이 지구에 도달한 2011년 2월 18일의 지자기 관측값은 일주일 전후 데이터와 비교하여 양자(Proton) 자력계 관측결과가 요동하였고, 대전과 서울지역에서의 측위결과도 태양폭풍 일주일 전후와 비교하여 2월 18일에 가장 큰 측위오차를 보였다.

• 한국항해항만학회지
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• 제35권9호
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• pp.701-706
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• 2011

Radio waves including GPS signals, various TV communications, and radio broadcasting can be disturbed by a strong solar storm, which may occur due to solar flares and produce an ionospheric delay anomaly in the ionosphere according to the change of total electron content. Electron density irregularities can cause deep signal fading, frequently known as ionospheric scintillation, which can result in the positioning error using GPS signal. This paper proposes a detection algorithm for the ionosphere delay anomaly during a solar storm by using multi-reference stations. Different TEC grid which has irregular electron density was applied above one reference station. Then the ionospheric delay in zenith direction applied different TEC will show comparatively large ionospheric zenith delay due to the electron irregularity. The ionospheric slant delay applied an elevation angle at reference station was analyzed to detect the ionospheric delay anomaly that can result in positioning error. A simulation test was implemented and a proposed detection algorithm using data logged by four reference stations was applied to detect the ionospheric delay anomaly compared to a criterion.

• 천문학회지
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• 제35권1호
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• pp.59-65
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• 2002

Solar observations support that magnetic reconnect ion ubiquitously occurs in the chromosphere as well as in the corona. It is now widely accepted that coronal magnetic reconnect ion is fast reconnect ion of the Petschek type, and is the main driver of solar flares. On the other hand, it has been thought that the traditional Sweet-Parker model may describe chromospheric reconnect ion without difficulty, since the electric conductivity in the chromoshphere is much lower than that in the corona. However, recent observations of cancelling magnetic features have suggested that chromospheric reconnect ion might proceed at a faster rate than the Sweet-Parker model predicts. We have applied the Sweet-Parker model and Petschek model to a well-observed cancelling magnetic feature. As a result, we found that the inflow speed of the Sweet-Parker reconnect ion is too small to explain the observed converging speed of the feature. On the other hand, the inflow speeds and outflow speeds of the Petschek reconnect ion are well compatible with observations. Moreover, we found that the Sweet-Parker type current sheet is subject to the ion-acoustic instability in the chromosphere, implying the Petschek mechanism may operate there. Our results strongly suggest that chromospheric reconnect ion is of the Petschek type.

• 천문학회지
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• 제34권1호
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• pp.9-15
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• 2001

We present the results of optical differential photometry of five blazars [PKS0219+428 (3C66A), PKS 0235+164 (AO 0235+16), H0414+019, PKS 0851+202 (OJ 287) and QSO 1807+698 (3C 371)] that were observed on 7 nights between November 05, 1997 and December 29, 1998, using the B and the V band filters. We have detected microvariations in four blazars (3C66A, AO 0235+16, H04l4+019, and OJ 287). In addition, the light curve of AO 0235+16 has displayed a mini-flare when the brightness of this source was decreasing. Night-to-night variations have also been detected in 3C66A, H04l4+019, and OJ 287. The results of our observations are discussed in the framework of accretion disk phenomena (magnetic flares or hot spots in accretion disks) and jet phenomena (plasma instabilities in jets).

• 천문학회보
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• 제38권2호
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• pp.33-33
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• 2013

We are developing empirical space weather (solar flare, solar proton event, and geomagnetic storm) forecast models based on solar data. In this talk we will review our main results and recent progress. First, we have examined solar flare (R) occurrence probability depending on sunspot McIntosh classification, its area, and its area change. We find that sunspot area and its increase (a proxy of flux emergence) greatly enhance solar flare occurrence rates for several sunspot classes. Second, a solar proton event (S) forecast model depending on flare parameters (flare strength, duration, and longitude) as well as CME parameters (speed and angular width) has been developed. We find that solar proton event probability strongly depends on these parameters and CME speed is well correlated with solar proton flux for disk events. Third, we have developed an empirical storm (G) forecast model to predict probability and strength of a storm using halo CME - Dst storm data. For this we use storm probability maps depending on CME parameters such as speed, location, and earthward direction. We are also looking for geoeffective CME parameters such as cone model parameters and magnetic field orientation. We find that all superstorms (less than -200 nT) occurred in the western hemisphere with southward field orientations. We have a plan to set up a storm forecast method with a three-stage approach, which will make a prediction within four hours after the solar coronagraph data become available. We expect that this study will enable us to forecast the onset and strength of a geomagnetic storm a few days in advance using only CME parameters and the WSA-ENLIL model. Finally, we discuss several ongoing works for space weather applications.

• 천문학회보
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• 제38권2호
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• pp.89.2-89.2
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• 2013

Solar energetic transients, e.g., flares, CMEs, etc., release large amount of energy which is expected to excite acoustic waves (p-modes) by exerting mechanical impulse of the thermal expansion of the flare on the photosphere. We study the p-mode properties of flaring and dormant active regions (ARs) to find association between flare and p-mode parameters. We compute the magnetic and flare activity indices of ARs using the line-of-sight magnetograms and GOES X-ray fluxes, respectively. The p-mode parameters are computed from the ring-diagram analysis. We correct p-mode parameters for magnetic field, filling factors and foreshortening by multiple linear-regression analysis. Our analysis of several flaring and dormant ARs observed during the Carrington rotations 1980-2109, showed strong association of mode parameters with magnetic and flare activities. We find that the mode parameters are contaminated by the geometrical effect. Mode amplitude decreases with angular distance from the solar disc centre. The mode width increases with magnetic activity while amplitude showed opposite relation due to mode absorption by the sunspot. After correcting modes due to all geometrical effects, magnetic activity and filling factor, we find that the modes amplitude, and mode energy increases with flare energy while width shows opposite relation.