• 한국정보디스플레이학회:학술대회논문집
• /
• 한국정보디스플레이학회 2006년도 6th International Meeting on Information Display
• /
• pp.130-133
• /
• 2006

In order to study the relationship between the discharge characteristics of an ac PDP and the surface conductivity of MgO thin film, the surface current across a ring shaped MgO film was measured by exposure to monochromatic vacuum ultraviolet from the synchrotron radiation source whose wavelength ranges from 60nm to 240nm $(5.5eV{\sim}25eV)$. The experimental results show that the surface current begins to increase rapidly at the photon energy of about 9 eV which might correspond to the valence band edge of MgO. The difference in the surface current level correlate well with the differences in the preparation method of MgO films and their respective discharge characteristics such as the firing, minimum sustain voltages, address voltage margin and address discharge delay time.

• 한국정보디스플레이학회:학술대회논문집
• /
• 한국정보디스플레이학회 2003년도 International Meeting on Information Display
• /
• pp.1155-1156
• /
• 2003

The advanced analysis techniques such as high resolution X-ray absorption spectroscopy (XAS), X-ray scattering, and photoelectron emission microscope (PEEM) using synchrotron radiation are probably able to open new opportunities for improving the performances of oxide cathodes with more clear and deep understanding.

• The Korean Journal of Ceramics
• /
• 제5권4호
• /
• pp.368-370
• /
• 1999

Using DC faced target sputtering method we grow AIN the films on the $Al_2O_3$(0001) substrate with varying thickness(17$\AA$-1000$\AA$). We measured x-ray diffraction(XRD) profiles by synchrotron radiation($\lambda$=1.12839 $\AA$) with four circle diffractometer. The full width half maximum(FWHM) of rocking curve for the AIN (0002) diffraction of the film grown at $500^{\circ}C$ was $0.029^{\circ}$. Also, we confirmed that the stress between AIN thin film and $Al_2O_3$(0001) substrate was reduced as increasing AIN film thickness, and the critical thickness of 400~500 $\AA$, defined as a lattice constant in the film agrees with that in a bulk without stress, was obtained.

• 천문학회지
• /
• 제48권1호
• /
• pp.9-20
• /
• 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.

• 천문학회보
• /
• 제37권1호
• /
• pp.67.1-67.1
• /
• 2012

Shocks are evolved when the relativistic jets in active galactic nuclei (AGNs), black hole binaries, supernova remnants (SNR) and gamma-ray bursts (GRBs) interact with the surrounding medium. The high energy particles are believed to be accelerated by the diffusive shock acceleration and the strong magnetic field is generated by Weibel instability in the shock. When ultrarelativistic electrons with strong magnetic field cool by the synchrotron emission, the radiation is observed in gamma-ray burst and the near-equipartitioned magnetic field in the external shock delays the afterglow emission. In this paper, we performed the 3D particle-in-cell (PIC) simulations to understand the characteristics of these relativistic shock and particle acceleration. Forward and reverse shocks are shaped while the unmagnetized injecting jet interacts with the unmagnetized ambient medium. Both upstream and downstream become thermalized and the particle accelerations are shown in each transition region of the shock structures.

• 천문학회보
• /
• 제42권2호
• /
• pp.45.1-45.1
• /
• 2017

A Korean VLBI Network Key Science Program, the Interferometric Monitoring of Gamma-ray Bright AGNs (iMOGABA) program continues to aim at revealing the origins of the gamma-ray flares that are often detected in active galactic nuclei (AGNs). Here in this presentation, we would like to present what we have learned about the Gamma-ray bright AGNs based on the recent results of the Korean VLBI Network Key Science Program: the iMGOABA. The results will include a) the source properties of the whole samples obtained from a single-epoch observation, and b) some of scientific highlights for the iMOGAGBA on specific sources. From those highlighted works, we find that the Gamma-ray bright AGNs become fainter at higher frequencies, yielding optically thin spectra at mm wavelengths. Based on the studies on specific sources, taking into account the synchrotron self-absorption model of the relativistic jet, we estimated the magnetic field strength in the mas emission region during the observing period.

• 한국방사선학회논문지
• /
• 제4권3호
• /
• pp.27-31
• /
• 2010

엑스선 영상의 공간분해능은 영상획득 장치에 사용되는 광학소자의 성능에 의해 결정된다. 8.5keV에서 높은 공간분해능 달성이 가능한 존 플레이트를 설계하였다. 방사광을 이용하는 대신 엑스선 튜브를 사용하는 영상시스템에서는 80nm의 공간분해능을 달성할 수 있음을 광선추적 기법을 이용하여 예측하였다. 전자빔 석판인쇄술을 이용하여 최외곽 폭 40nm를 갖는 존 플레이트가 제작하였다.

• 한국진공학회:학술대회논문집
• /
• 한국진공학회 1997년도 제12회 학술발표회 논문개요집
• /
• pp.25-26
• /
• 1997

• 천문학회지
• /
• 제47권1호
• /
• pp.15-39
• /
• 2014

Polarization is a basic property of light and is fundamentally linked to the internal geometry of a source of radiation. Polarimetry complements photometric, spectroscopic, and imaging analyses of sources of radiation and has made possible multiple astrophysical discoveries. In this article I review (i) the physical basics of polarization: electromagnetic waves, photons, and parameterizations; (ii) astrophysical sources of polarization: scattering, synchrotron radiation, active media, and the Zeeman, Goldreich-Kylafis, and Hanle effects, as well as interactions between polarization and matter (like birefringence, Faraday rotation, or the Chandrasekhar-Fermi effect); (iii) observational methodology: on-sky geometry, influence of atmosphere and instrumental polarization, polarization statistics, and observational techniques for radio, optical, and $X/{\gamma}$ wavelengths; and (iv) science cases for astronomical polarimetry: solar and stellar physics, planetary system bodies, interstellar matter, astrobiology, astronomical masers, pulsars, galactic magnetic fields, gamma-ray bursts, active galactic nuclei, and cosmic microwave background radiation.

• 천문학회보
• /
• 제43권1호
• /
• pp.35.2-35.2
• /
• 2018

Magnetic fields in clusters of galaxies play a critical role in shaping up the intracluster medium. Their existence has been established through observations of synchrotron emission, especially from radio relics and halos, as well as observations of rotation measure. In the so-called Sausage relic, which is one of Mpc-size giant radio relics detected in the outskirts of merging clusters, for instance, the magnetic fields are believed to have a few ${\mu}G$ strength and a Mpc scale. The observed magnetic fields are conjectured to be produced by the process of small-scale turbulence dynamo. To investigate the dynamo origin, we simulate the development of turbulence and the follow-up amplification of magnetic fields in galaxy clusters using a three-dimensional magnetohydrodynamical(MHD) code. Turbulence is induced in highly stratified backgrounds expected in clusters, and driven sporadically mimicking major mergers. We here present preliminary results, aiming to answer whether the turbulence dynamo scenario can explain observed magnetic fields in clusters of galaxies.