• Investigative Magnetic Resonance Imaging
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• 제22권1호
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• pp.26-36
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• 2018

Purpose: Children born with single ventricle physiology demonstrate poor growth rate and suffer from malnutrition, which lead to increased morbidity and mortality in this population. We assume that an anabolic steroid, oxandrolone, will promote growth in these infants by improving myocardial energy utilization. The purpose of this paper is to study the efficacy of oxandrolone on myocardial energy consumption in these infants. Materials and Methods: We modeled single ventricle physiology in a lamb by prenatally shunting the aorta to the pulmonary artery and then postnatally, we monitored cardiac energy utilization by quantitatively measuring the first order reaction rate constant, $k_f$ of the creatine-kinase reaction in the heart using magnetization transfer $^{31}P$ magnetic resonance spectroscopy, home built $^1H/^{31}P$ transmit/receive double tuned coil, and transmit/receive switch. We also performed cine MRI to study the structure and dynamic function of the myocardium and the left ventricular chamber. The spectroscopy data were processed using home-developed python software, while cine data were analyzed using Argus software. Results: We quantitatively measured both the first order reaction rate constant and ejection fraction in the control, shunted, and the oxandrolone-treated lambs. Both $k_f$ and ejection fraction were found to be more significantly reduced in the shunted lambs compared to the control lambs, and they are increased in oxandrolone-treated lambs. Conclusion: Some improvement was observed in both the first order reaction rate constant and ejection fraction for the lamb treated with oxandrolone in our preliminary study.

• 천문학회지
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• 제35권3호
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• pp.151-157
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• 2002

From the data of solar wind observation by ACE spacecraft orbiting the Earth-Sun Lagrangian point, we selected 48 forward interplanetary shocks(IPSs) occurred in 2000, maximum solar activity period. Examining the profiles of solar wind parameters, the IPSs are classified by their shock drivers. The significant shock drivers are the interplanetary coronal mass ejection(ICME) and the high speed stream(HSS). The IPSs driven by the ICMEs are classified into shocks driven by magnetic clouds and by ejectas based on the existence of magnetic flux rope structure and magnetic field strength. Some IPSs could be formed as the blast wave by the smaller energy and shorter duration of shock drivers such as type II radio burst. Out of selected 48 forward IPSs, $56.2\%$ of the IPSs are driven by ICME, $16.7\%$ by HSS, and $16.7\%$ of the shocks are classified into blast-wave type shocks. However, the shock drivers of remaining $10\%$ of the IPSs are unidentified. The classification of the IPSs by their driver is a first step toward investigating the critical magnitudes of the IPS drivers commencing the magnetic storms in each class.

• 천문학논총
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• 제2권1호
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• pp.13-20
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• 1985

Magnetic reconnect ion is studied numerically by means of a two dimensional MHD code. The initial magnetic field configuration is the two-dimensional dipole field, and the simulation model involves magnetic reconnect ion driven by the magnetized plasma flow. Strong plasma jetting, plasmoid formation and its fast ejection are observed in the downstream region. The dependence of reconnection rate on the incoming energy flux is found to be very sensitive, while the magnitude of the resistivity does not influence much on the reconnection rate. The simulation results are discussed in the context of the geomagnetic substorm.

• 한국자기학회지
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• 제8권5호
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• pp.255-260
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• 1998

두께 10$\mu\textrm{m}$ 이하의 코발트계 극박형 비정질합금의 진공중 용탕급냉방법에 의한 제조조건과 자기적 특성에 대해 연구되었다. 구리 냉각롤의 회전 선속도를 55 m/s로 하였을 때, 0.05 kgf/cm2 이하의 용탕분사압 조건에서 극박형 리본이 얻어졌다. 합금 두께는 용탕분사 가스압력의 감소에 비례하여 직선적으로 감소하였으며, 이와 동시에 폭의 감소도 함께 일어났다. 이는 극박형 합금을 만들기 위해 용탕분사압을 극단적으로 감소시키면 노즐구의 양단부에서 용융금속과 노즐 사이의 마찰효과가 크게 나타나 유효분사압이 현저히 감소하는 데에 기인하는 것으로 해석되었다. 저주파(1 kHz) 실효투자율은 대략 2차 함수의 관계로 리본 두께의 감소에 따라 저하되었다. 반면 보자력은 두께의 감소에 반비례하여 증가하였는데, 이들 현상은 거의 전적으로 표면효과의 증대에 의한 자벽이동의 억제에 그 원인이 있는 것으로 판단되었다. 그러나 고주파(1 MHz) 실효투자율은 두께의 감소에 따라 증가하였는바 이는 와전류 발생이 억제되어 자기장 방향으로의 자화회전이 보다 용이해지기 때문으로 생각되었으며, 결과적으로 극박화에 의해 MHz 대역에서 우수한 저손실 성질을 나타내는 자심 특성의 실현이 가능하였다.

• 천문학회보
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• 제38권2호
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• pp.89.1-89.1
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• 2013

We present a multiwavelength study of the X-class flare, which occurred in active region (AR) NOAA 11339 on 3 November 2011. The EUV images recorded by SDO/AIA show the activation of a remote filament (located north of the AR) with footpoint brightenings about 50 min prior to the flare occurrence. The kinked filament rises-up slowly and after reaching a projected height of ~49 Mm, it bends and falls freely near the AR, where the X-class flare was triggered. Dynamic radio spectrum from the Green Bank Solar Radio Burst Spectrometer (GBSRBS) shows simultaneous detection of both positive and negative drifting pulsating structures (DPSs) in the decimetric radio frequencies (500-1200 MHz) during the impulsive phase of the flare. The global negative DPSs in solar flares are generally interpreted as a signature of electron acceleration related to the upward moving plasmoids in the solar corona. The EUV images from AIA $94{\AA}$ reveal the ejection of multiple plasmoids, which move simultaneously upward and downward in the corona during the magnetic reconnection. The estimated speeds of the upward and downward moving plasmoids are ~152-362 and ~83-254 km/s, respectively. These observations strongly support the recent numerical simulations of the formation and interaction of multiple plasmoids due to tearing of the current-sheet structure. On the basis of our analysis, we suggest that the simultaneous detection of both the negative and positive DPSs is most likely generated by the interaction/coalescence of the multiple plasmoids moving upward and downward along the current-sheet structure during the magnetic reconnection process. Moreover, the differential emission measure (DEM) analysis of the active region reveals presence of a hot flux-rope structure (visible in AIA 131 and $94{\AA}$) prior to the flare initiation and ejection of the multi-temperature plasmoids during the flare impulsive phase.

• 천문학회보
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• 제35권1호
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• pp.26.1-26.1
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• 2010

In this talk we outline the current understanding of solar flares, mainly focusing on magnetohydrodynamic (MHD) processes. A flare causes plasma heating, mass ejection, and particle acceleration which generates high-energy particles. The key physical processes producing a flare are: the emergence of magnetic field from the solar interior to the solar atmosphere (flux emergence), formation of current-concentrated areas (current sheets) in the corona, and magnetic reconnection proceeding in a current sheet to cause shock heating, mass ejection, and particle acceleration. A flare starts with the dissipation of electric currents in the corona, followed by various dynamic processes that affect lower atmosphere such as the chromosphere and photosphere. In order to understand the physical mechanism for producing a flare, theoretical modeling has been develops, where numerical simulation is a strong tool in that it can reproduce the time-dependent, nonlinear evolution of a flare. In this talk we review various models of a flare proposed so far, explaining key features of individual models. We introduce the general properties of flares by referring observational results, then discuss the processes of energy build-up, release, and transport, all of which are responsible for a flare. We will come to a concluding viewpoint that flares are the manifestation of the recovering and ejecting processes of a global magnetic flux tube in the solar atmosphere, which has been disrupted via interaction with convective plasma while rising through the convection zone.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2010년도 한국우주과학회보 제19권1호
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• pp.25.1-25.1
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• 2010

This talk outlines the current understanding of solar flares, mainly focusing on magnetohydrodynamic (MHD) processes. A flare causes plasma heating, mass ejection, and particle acceleration that generates high-energy particles. The key physical processes related to a flare are: the emergence of magnetic field from the solar interior to the solar atmosphere (flux emergence), formation of current-concentrated areas (current sheets) in the corona, and magnetic reconnection proceeding in current sheets that causes shock heating, mass ejection, and particle acceleration. A flare starts with the dissipation of electric currents in the corona, followed by various dynamic processes which affect lower atmospheres such as the chromosphere and photosphere. In order to understand the physical mechanism for producing a flare, theoretical modeling has been developed, in which numerical simulation is a strong tool reproducing the time-dependent, nonlinear evolution of plasma before and after the onset of a flare. In this talk we review various models of a flare proposed so far, explaining key features of these models. We show observed properties of flares, and then discuss the processes of energy build-up, release, and transport, all of which are responsible for producing a flare. We come to a concluding view that flares are the manifestation of recovering and ejecting processes of a global magnetic flux tube in the solar atmosphere, which was disrupted via interaction with convective plasma while it was rising through the convection zone.

• 한국콘텐츠학회논문지
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• 제21권2호
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• pp.437-444
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• 2021

본 연구는 cardiac CT를 이용한 박출계수 산출 시 cardiac MRI와 물리적 시간 해상도 차이를 분석하여 보정함으로써 cardiac CT의 오진율을 감소시키고자 하였다. 연구 방법은 대동맥판막 역류 질환을 진단받은 138명을 대상으로 cardiac CT와 cardiac MRI의 박출계수를 산출한 후 두 검사 간 물리적 시간 해상도 차이를 cardiac CT의 박출계수에 보정한 다음 신뢰도를 평가하여, 물리적 시간 해상도 차이 보정 전, 후 cardiac CT의 오진율이 개선됐는지 평가 하였다. 연구결과, 물리적 시간 해상도 차이 보정 전 cardiac CT 박출계수의 오진율은 38.4%(53명)로 높게 나왔고, 보정 후 오진율은 23.9%(33명)로 감소하였다. 또한 Bland-Altman plot에서 확인한 보정된 cardiac CT 박출계수는 cardiac MRI의 박출계수와의 일치도가 상당히 높은 것을 알 수 있다. 결론적으로 심장판막 질환 진단시 단순한 cardiac CT의 박출계수로만 진단하는 것은 오진율을 높일 수 있으므로 cardiac MRI로 물리적 시간 해상도의 차이를 보정하면 오진율을 14.5%(20명) 감소시킬 수 있다. 그러므로 본 연구를 박출계수 산출 시 적용한다면 유용성이 높다고 사료된다.

• 천문학회지
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• 제42권6호
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• pp.175-184
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• 2009

A method of estimating the lower bound of coronal magnetic field strength in the neighborhood of an ejecting plasmoid is presented. Based on the assumption that the plasma ejecta is within a magnetic island, an analytical expression for the force acting on the ejecta is derived. The method is applied to a limb coronal mass ejection event, and a lower bound of the magnetic field strength just below the CME core is estimated. The method is expected to provide useful information on the strength of reconnecting magnetic field if applied to X-ray plasma ejecta.

• 한국방사선학회논문지
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• 제5권5호
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• pp.289-294
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• 2011

본 연구의 목적은 cardiac MRI를 이용하여 확장기와 수축기의 정량적 측정을 통해 각 단면의 심박출률의 차이를 알아보고자 하였다. 총 12명(정상 7명, 심근교 1명, 부정맥 4명)을 대상으로 심첨에서부터 대동맥궁 쪽으로 단면을 얻었다. 수축기와 확장기 영상을 확대하여 경계를 정하였고, 이 면적을 바탕으로 1, 3, 5, 6-7단면의 심박출률을 구하였다. 정상인의 평균 박출률은 각각 1, 3, 5, 6-7단면에서 67.14%, 66.24%, 65.63%, 그리고 65.29% 로 나타났다. 반면, 환자들의 평균 박출률은 각각 1, 3, 5, 6-7단면에서 61.74%, 60.92%, 60.89%, 그리고 61.89%로 나타났다. 본 연구를 통해 cardiac MRI를 이용한 특정단면의 심박출률은 각 단면마다 큰 차이가 없음을 알 수 있었고 따라서 cardic MRI를 이용한 심박출계수의 평가는 대표 단면만으로 가능함을 알 수 있었다.