• Journal of Astronomy and Space Sciences
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• 제31권2호
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• pp.101-120
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• 2014

The nature of the exotic stellar corpses which reincarnate by consuming their companion is reviewed. Apart from sucking life from their partners, they are actually eating the doomed companions away by their deadly and powerful particle/radiation beams. Such situation resembles that a female "black widow" spider that eats its mate after mating. These celestial zombies are called - Millisecond pulsars (MSPs). In this review article, I will focus on the effort of Fermi Asian Network (FAN) in exploring these intricating objects over the last five years. Two special classes of MSPs are particularly striking. Since Fermi Gamma-ray Space Telescope has started surveying the gamma-ray sky, the population of "black widows" has been boosted. Another dramatic class is so-called "redbacks" (Australian cousin of "black widows") which has just emerged in the last few years. These MSPs provide us with a long-sought missing link in understanding the transition between accretion-powered and rotation-powered systems. The strategy of hunting MSPs through mulitwavelength observations of the unidentified Fermi objects is also reviewed.

• 천문학회보
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• 제39권1호
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• pp.70.1-70.1
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• 2014

We study the origin and acceleration mechanism of solar energetic particles (SEPs), which are one of the major causes of hazardous impacts in the space weather. By adopting the velocity dispersion to the multi-channel energy band observations from SOHO/ERNE and Wind/3DP, we estimate the onset time for each energy band and investigate coronal structure and CME's dynamics associated with the SEPs. Through this study we will find clues to answer the questions about the origin and acceleration of SEPs as well as their associated with flare and/or CMEs. We will apply our findings to improve the forecasting system of the solar radiation storms.

• Journal of Astronomy and Space Sciences
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• 제23권3호
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• pp.217-226
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• 2006

이 논문에서는 먼저 정지궤도에서 관측된 세 개의 Sawtooth 진동 이벤트를 보고한다. Sawtooth 진동에서는 수십에서 수백 keV 에너지대의 자기권 대전입자 플럭스가 평균 $2{\sim}3$시간의 주기로 반복적으로(10여 차례 내외) 증감한다. 플럭스가 증가 할 때는 매우 급격히 증가하고 그 후 다음 증가 때까지 서서히 감소하는 특징을 보이는데 이러한 반복적 플럭스 증감을 시간에 대한 그래프로 나타내면 마치 톱니 모양을 갖는다. 다음으로 이러한 각 Sawtooth 진동 이벤트 기간에 대해 바깥 방사선 벨트 외경계면의 변화를 연구하였다. 이를 위해 SAMPEX 저궤도 위성이 관측한 상대론적 전자 플럭스 자료를 이용하였다. 이 관측 자료를 이용하여 바깥 방사선 벨트 외경계면 위치의 L값을 결정하고 각 Sawtooth 진동 이벤트 기간 동안의 경계면 L값의 변화를 분석하였다. 분석 결과로서 바깥 방사선 벨트 외경계면이 Sawtooth 진동 각 톱니 주기에 맞추어 팽창과 수축을 반복하는 진동을 발견하였다. 구체적으로, Sawtooth 입자 플럭스가 증가 한 직후에는 바깥 방사선 벨트 외경계면이 더 밖으로 팽창하고, 그 후 Sawtooth 입자 플럭스가 다음 주기 전까지 서서히 감소하는 동안에는 다시 방사선 벨트 외경계면이 수축하는 것을 발견하였다. 한편 Sawtooth 입자 플럭스 증가 시에는 주야간 지역간의 자기권 자기장 비대칭 정도가 감소하고, 반대로 입자 플럭스 감소 시에는 주야간 지역간의 자기권 자기장 비대칭 정도가 증가하는 특징이 반복적으로 나타났다. 이로 인해 바깥 방사선 벨트 외경계면도 주기적으로 변하는 것으로 생각된다.

• 한국음향학회:학술대회논문집
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• 한국음향학회 1998년도 학술발표대회 논문집 제17권 2호
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• pp.111-114
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• 1998

Acoustical holography is one of the powerful methods in sound radiation problems. Just measuring hologram data on a plane, one can calculate whole space physical quantities such as pressure, particle velocity, and sound intensity. However, the use of finite and discrete operations introduce significant errors inevitably. This paper reviews error reduction schemes, and introduces error analysis criteria derived from modal analysis. Finally the effect of window functions is investigated by these criteria.

• 천문학회보
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• 제43권2호
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• pp.43.1-43.1
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• 2018

Young pulsar wind nebulae, powered by energetic central pulsars, are often observed as bright extended sources in the X-ray band. They are believed to accelerate electrons and positrons to very high energy and can possibly explain the positron excess observed by Fermi and AMS. The electron distribution in these PWNe can be best studied by X-ray satellites because emission in the X-ray band is produced by direct synchrotron radiation of the electrons and positrons. We present NuSTAR studies of PWNe and discuss the implication. Future studies to help further our understanding of particle acceleration will be briefly discussed.

• Journal of Astronomy and Space Sciences
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• 제24권2호
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• pp.125-134
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• 2007

이 연구에서는 태양 및 지자기 활동에 의해 발생한 우주환경변화가 우리나라 위성인 아리랑위성1호(KOMPSAT-1)의 궤도에 미치는 영향을 분석하였다. 인공위성의 궤도변화는 정상적인 상태에서도 자연적인 섭동에 의해 지속적으로 발생하지만, 거대한 태양폭발에 의한 지구 주변 우주환경이 급격히 변화할 때 고층대기의 밀도변화로 인해 크게 발생한다. 특히 이러한 현상은 아리랑위성 1호와 같이 저궤도 상에서 운영되는 위성에 직접적인 영향을 미친다. 이 때, 태양활동에 의한 지구 주변 우주환경의 변화는 크게 두 가지로 구분할 수 있다. 하나는 태양 플레어 (Flare)가 폭발했을 때 고에너지 복사(Radiation)로 인해 지구 고층대기가 가열되어 팽창하고 이런 결과로 고층대기에 있는 중성입자밀도가 급격히 증가하는 것이다. 다른 하나는 코로나 물질 방출(Coronal Mass Ejections) 등에 의해 발생한 지자기폭풍기간 동안 플라즈마 대류와 입자들의 하강으로 전기장이 강해져 상당량의 줄가열(Joule heating)과 하강입자가열(precipitating particle heating)이 발생하고 이로 인해 중성입자밀도가 증가하는 것이다. 두 가지 원인에 대한 영향을 구분하여 알아보기 위해, 우리는 태양 및 지자기 자료를 면밀히 분석하여 2001년에서 2002년 동안 5개의 기간을 선정하였다. 그 결과 위성의 대기저항가속도는 태양의 극자외선(Extreme Ultra-Violet)의 증가와 함께 약 하루 정도의 시간 지연을 가지고 유사하게 변화하고 있음을 확인하였다(R=0.92). 그리고 지자기폭풍이 발생한 기간동안 대기저항가속도는 지자기폭풍에 의한 Dst 변화와 상당히 유사하게 그리고 거의 동시에 급격히 변화하는 것을 확인하였다. 마지막으로 우리는 위성의 대기저항가속도의 변화는 전반적으로는 오랜 기간 동안 고에너지 복사에 의한 효과로 나타나고 있으나 짧은 기간(하루 미만) 동안 크게 발생하는 대기저항가속도의 변화는 지자기폭풍에 의한 효과로 보고 있다.

• 한국의학물리학회지:의학물리
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• 제33권4호
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• pp.114-120
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• 2022

Purpose: Particle beam therapy is advantageous over photon therapy. However, adequately delivering therapeutic doses to tumors near critical organs is difficult. Nanoparticle-aided radiation therapy can be used to alleviate this problem, wherein nanoparticles can passively accumulate at higher concentrations in the tumor tissue compared to the surrounding normal tissue. In this study, we investigate the dose enhancement effect due to gold nanoparticle (GNP) when Carbon-12, He-4, and proton beams are irradiated on GNP. Methods: First, monoenergetic Carbon-12 and He-4 ion beams of energy of 283.33 MeV/u and 150 MeV/u, respectively, and a proton beam of energy of 150 MeV were irradiated on a water phantom of dimensions 30 cm×30 cm×30 cm. Subsequently, the secondary-particle information generated near the Bragg peak was recorded in a phase-space (phsp) file. Second, the obtained phsp file was scaled down to a nanometer scale to irradiate GNP of diameter 50 nm located at the center of a 4 ㎛×4 ㎛×4 ㎛ water phantom. The dose enhancement ratio (DER) was calculated in intervals of 1 nm from the GNP surface. Results: The DER of GNP computed at 1 nm from the GNP surface was 4.70, 4.86, and 4.89 for Carbon-12, He-4, and proton beams, respectively; the DER decreased rapidly with increasing distance from the GNP surface. Conclusions: The results indicated that GNP can be used as radiosensitizers in particle beam therapy. Furthermore, the dose enhancement effect of the GNP absorbed by tumor cells can aid in delivering higher therapeutic doses.

• 한국소성가공학회:학술대회논문집
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• 한국소성가공학회 2005년도 춘계학술대회 논문집
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• pp.454-457
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• 2005

Voloxidizer for hot cell demonstration that handle spend fuel of high radiation virulence in limited space should become a small size and not scatter in its exit. This study determine optimum velocity of $U_3O_8$ using Newton-Raphson Method. We have conducted fortran programing on the Newton-Raphson Method, obtained a theory results and, predicted optimum velocity on the particle size distribution of $U_3O_8$. We have conducted experimentation using acrylic experimental device for verification of theory method, sampled and analyzed using the particle size analyzer In the results, we have found maximum $5\~7\%$ error rate in the comparative value of theory and experimentation. Optimum velocity and experimental results of $U_3O_8$ for scatter prevention have applied for design of demonstration voloxidizer, and produced operation condition of voloxidizer.

• 대한방사선기술학회지:방사선기술과학
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• 제44권4호
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• pp.359-365
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• 2021

A heavy particle accelerator is a device that accelerates particles using high energy and is used in various fields such as medical and industrial fields as well as research. However, secondary neutrons and particle fragments are generated by the high-energy particle beam, and among them, the neutrons do not have an electric charge and directly interact with the nucleus to cause radiation of the material. Quantitative evaluation of the radioactive material produced in this way is necessary, but there are many difficulties in actual measurement during or after operation. Therefore, this study compared and evaluated the generated radioactive material in the concrete shield for protons and carbon ions of specific energy by using the simulation code FLUKA. For the evaluation of each energy of proton beam and carbon ion, the reliability of the source term was secured within 2% of the relative error with the data of the NASA Space Radiation Laboratory(NSRL), which is an internationally standardized data. In the evaluation, carbon ions exhibited higher neutron flux than protons. Afterwards, in the evaluation of radioactive materials under actual operating conditions for disposal, a large amount of short-lived beta-decay nuclides occurred immediately after the operation was terminated, and in the case of protons with a high beam speed, more radioactive products were generated than carbon ions. At this time, radionuclides of ⁴⁴Sc, ³H and ²²Na were observed at a high rate. In addition, as the cooling time elapsed, the ratio of long-lived nuclides increased. For nonparticulate radionuclides, ³H, ²²Na, and for particulate radionuclides, ⁴⁴Ti, ⁵⁵Fe, ⁶⁰Co, ¹⁵²Eu, and ¹⁵⁴Eu nuclides showed a high ratio. In this study, it is judged that it is possible to use the particle accelerator as basic data for facility maintenance, repair and dismantling through the prediction of radioactive materials in concrete according to the cooling time after operation and termination of operation.

• Journal of Astronomy and Space Sciences
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• 제30권4호
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• pp.247-253
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• 2013

It has long been known that the magnetospheric particles can precipitate into the atmosphere of the Earth. In this paper we examine such precipitation of energetic electrons using the data obtained from low-altitude polar orbiting satellite observations. We analyze the precipitating electron flux data for many periods selected from a total of 84 storm events identified for 2001-2012. The analysis includes the dependence of precipitation on the Kp index and the electron energy, for which we use three energies E1 > 30 keV, E2 > 100 keV, E3 > 300 keV. We find that the precipitation is best correlated with Kp after a time delay of < 3 hours. Most importantly, the correlation with Kp is notably tighter for lower energy than for higher energy in the sense that the lower energy precipitation flux increases more rapidly with Kp than does the higher energy precipitation flux. Based on this we suggest that the Kp index reflects excitation of a wave that is responsible for scattering of preferably lower energy electrons. The role of waves of other types should become increasingly important for higher energy, for which we suggest to rely on other indicators than Kp if one can identify such an indicator.