• 천문학회지
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• 제48권1호
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• pp.9-20
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• 2015

We study the evolution of the energy spectrum of cosmic-ray electrons accelerated at spherically expanding shocks with low Mach numbers and the ensuing spectral signatures imprinted in radio synchrotron emission. Time-dependent simulations of diffusive shock acceleration (DSA) of electrons in the test-particle limit have been performed for spherical shocks with parameters relevant for typical shocks in the intracluster medium. The electron and radiation spectra at the shock location can be described properly by the test-particle DSA predictions with instantaneous shock parameters. However, the volume integrated spectra of both electrons and radiation deviate significantly from the test-particle power-laws, because the shock compression ratio and the flux of injected electrons at the shock gradually decrease as the shock slows down in time. So one needs to be cautious about interpreting observed radio spectra of evolving shocks based on simple DSA models in the test-particle regime.

• 천문학회지
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• 제34권4호
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• pp.293-295
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• 2001

A numerical scheme that incorporates a self-consistent cosmic-ray (CR, hereafter) injection model into the combined gas dynamics and CR diffusion-convection code has been developed. The hydro/CR code can follow in a very cos-effective way the evolution of CR modified shocks by adopting subzone shock-tracking and multi-level Adaptive Mesh Refinement techniques. The injection model is based on interactions of the suprathermal particles with self-generated MHD waves in quasi-parallel shocks. The particle injection is followed numerically by filtering the diffusive flux of suprathermal particles across the shock to upstream region according to a velocity-dependent transparency function, which represents the fraction of leaking suprathermal particles. In the strong shock limit of Mach numbers $\ge$20, significant physical processes such as the injection and acceleration seem to become independent of M, while they are sensitively dependent on M for M < 10. Although some particles injected early in the evolution continue to be accelerated to higher energies, the postshock CR pressure reaches a time asymptotic value due to balance between acceleration and diffusion of the CR particles.

• 천문학회지
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• 제37권5호
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• pp.307-313
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• 2004

Clusters of galaxies are believed to constitute a population of astrophysical objects potentially able to emit electromagnetic radiation up to gamma-ray energies. Evidence of the existence of non-thermal radiation processes in galaxy clusters is indicated from observations of diffuse radio halos, hard X-ray and EUV excess emission. The presence of cosmic ray acceleration processes and its confinement on cosmological timescales nearly inevitably yields in predicting energetic gamma-ray emission, either directly deduceably from a cluster's multifreqency emission characteristics or indirectly during large-scale cosmological structure formation processes. This theoretical reasoning suggests several scenarios to actually detect galaxy clusters at gamma-ray wavelengths: Either resolved as individual sources of point-like or extended gamma-ray emission, by investigating spatial-statistical correlations with unidentified gamma-ray sources or, if unresolved, through their contribution to the extragalactic diffuse gamma-ray background. In the following I review the situation concerning the proposed relation between galaxy clusters and high-energy gamma-ray observations from an observational point-of-view.

• 천문학회보
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• 제32권2호
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• pp.25.1-25.1
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• 2007

• 천문학회보
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• 제31권1호
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• pp.19.1-19.1
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• 2006

• 천문학회보
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• 제31권2호
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• pp.39.1-39.1
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• 2006

• 한국진공학회:학술대회논문집
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• 한국진공학회 2013년도 제45회 하계 정기학술대회 초록집
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• pp.65.1-65.1
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• 2013

Icy dust particles in interstellar clouds are considered to play a catalytic role in molecular evolution in space. Atoms and simple molecules constituting the ice mantles of dust particles may be transformed into more complex molecules under the irradiation of UV and cosmic rays. This seminar will present our recent study results for chemistry of ice surfaces, with the emphases on the mechanistic features of elementary reactions and the implications for interstellar molecular evolution. The types of reactions studied include molecule diffusion in ice, proton and hydroxide transfers, and some UV-induced reactions wih astrobiological relevance.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2011년도 한국우주과학회보 제20권1호
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• pp.20.2-20.2
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• 2011

The NASA Antarctica balloon experiment CREAM has successfully collected the data of energetic cosmic rays during flights in past years. We will present the recent analysis results of the CREAM experiment. We will also report on the launch and recovery process of the latest flight. The silicon charge detector of the CREAM has played the key role in the precision measurement of the charge constitution of energetic cosmic rays. We proposed the upgrade of the CREAM experiment with the installment of a new large silicon charge detector on top of the CREAM instrument. The charge measurement of the large silicon detector with no material in front is expected to improve the accuracy of the CREAM charge measurement drastically when combined with the measurement of the existing double layer silicon detector. We will present the fabrication of the large silicon detector and its performance in the radiation source test as well as in the beam test.

• 천문학회보
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• 제39권2호
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• pp.73.1-73.1
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• 2014

We investigate the influence of the galactic magnetic field (GMF) on the arrival direction (AD) of ultra-high energy cosmic rays (UHECRs) by searching the correlation with the large-scale structure (LSS) of the universe. The deflection angle of UHECRs from sources by the GMF is reflected in a source model by introducing the Gaussian smearing angle as a free parameter. Assuming the deflections by the GMF are mainly dependent on the galactic latitude, b, we divide the regions of sky by b and analyze the correlation between the AD of UHECRs and the LSS of the universe in each region varying the smearing angle. We find the deflection is strongly dependent on the galactic latitude by the maximum likelihood estimation. Specifically, the best-fit smearing angles are $9^{\circ}$ and $84^{\circ}$ in the high galactic latitude (HGL), $-90^{\circ}$ < b < $-60^{\circ}$, and in the low galactic latitude (LGL), $-30^{\circ}$ < b < $30^{\circ}$, respectively. The strength of GMF becomes stronger from the HGL to the LGL. From the results, we can estimate the strength of GMF in each region. In the LGL, for example, if we assume UHECRs are protons, we have the order of $100{\mu}G$ GMF, which is much stronger than the expected value of conventional GMF model. However, if the primaries are heavy nuclei, which is consistent with the observational result of mass composition analysis, the order of GMF strength is a few ${\mu}G$. More data from the future experiments make it possible to study the GMF between the source of UHECRs and Earth more accurately.

• 한국방사선학회논문지
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• 제13권1호
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• pp.87-93
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• 2019

최근에 해외여행의 증가로 인하여 비행기를 이용하는 사용자수가 급격하게 증가하고 있다. 비행기는 탑승 시에 높은 고도를 유지한다. 따라서 비행 교통수단을 이용하는 승객들은 높은 고도로 인한 우주자연방사선 선량에 노출되어 방사선 장해 확률이 증가되어진다. 지구 외부로부터 기인하는 우주방사선은 지구대기밖에 400km와 1200km 사이의 고도에 위치하는 자기장 벨트인 반 엘렌대에 의해 대부분은 차단되지만 그렇지 못한 일부 우주방사선은 벤 엘런대를 투과하여 지구의 대기와 지표에 영향을 준다. 전례연구에 따르면 지구의 지표에서 고도가 100m 증가함과 동시에 0.03 mSv정도의 자연방사선량이 증가한다는 결과가 보고되었다. 이번연구는 비행기를 탑승하는 동안 탑승자가 노출될 수 있는 고도에 따른 자연방사선의 영향을 최소로 차폐하는데 목적을 두었다. 그 중에서도 방사선에 감수성이 높은 장기인 갑상선을 고도에 따른 자연방사선량으로부터 보호하고자 연구하였다. 이번 연구는 이동이 간편하고 세탁이 편리한 손수건을 선택하였다. 그리고 제작된 손수건에 다양한 차폐막을 삽입 할 수 있는 방법으로 고안하였다. 재질이 면으로 된 손수건을 선택한 이유는 사용자가 착용시 피부의 거부감을 최소화하기 위함이다. 결론적으로 본 연구에서 고안된 차폐막손수건은 우주자연방사선량을 70%이상 차폐하는 결과를 얻었다. 따라서 사용자가 높은 고도의 비행기 탑승 시 차폐막 손수건을 착용한다면 우주자연방사선으로부터 갑상선을 보호하는데 많은 도움을 줄 것으로 사료된다.