• 천문학논총
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• 제32권1호
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• pp.131-133
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• 2017

We present the latest results from the Mission Program NIRLT (PI: I.Yamamura), the near-infrared spectroscopy of brown dwarfs using the AKARI/IRC grism mode with the spectral resolution of ~ 120. The near-infrared spectra in the wavelength range between 2.5 and $5.0{\mu}m$ are especially important to study the brown dwarf atmospheres because of the presence of major molecular bands, including $CH_4$ at $3.3{\mu}m$, $CO_2$ at $4.2{\mu}m$, CO at $4.6{\mu}m$, and $H_2O$ around $2.7{\mu}m$. We observed 27 sources, and obtained 16 good spectra. Our model fitting reveals deviations between theoretical model and observed spectra in this wavelength range, which may be attributed to the physical condition of the upper atmosphere. The deviations indicate additional heating, which we hypothesize to be due to chromospheric activity. We test this effect by modifying the brown dwarf atmosphere model to artificially increase the temperature of the upper atmosphere, and compare the revised model with observed spectra of early- to mid-L type objects with $H{\alpha}$ emission. We find that the chemical structure of the atmosphere changes dramatically, and the heating model spectra of early-type brown dwarfs can be considerably improved to match the observed spectra. Our result suggests that chromospheric activity is essential to understand early-type brown dwarf atmospheres.

• Journal of Astronomy and Space Sciences
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• 제38권3호
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• pp.175-183
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• 2021

The dependencies of the chemical element abundances in stellar atmospheres with respect to solar abundances on the second ionization potentials of the same elements were investigated using the published stellar abundance patterns for 1,149 G and K giants in the Local Region of the Galaxy. The correlations between the relative abundances of chemical elements and their second ionization potentials were calculated for groups of stars with effective temperatures between 3,764 and 7,725 K. Correlations were identified for chemical elements with second ionization potentials of 12.5 eV to 20 eV and for elements with second ionization potentials higher than 20 eV. For the first group of elements, the correlation coefficients were positive for stars with effective temperatures lower than 5,300 K and negative for stars with effective temperatures from 5,300 K to 7,725 K. The results of this study and the comparison with earlier results for hotter stars confirm the variations in these correlations with the effective temperature. A possible explanation for the observed effects is the accretion of hydrogen and helium atoms from the interstellar medium.

• 천문학회지
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• 제38권2호
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• pp.283-287
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• 2005

The slow evolution of global magnetic fields and other dynamical processes in atmospheres of CP magnetic stars lead to the development of induced electric currents in all conductive atmospheric layers. The Lorentz force, which results from the interaction between a magnetic field and the induced currents, may modify the atmospheric structure and provide insight into the formation and evolution of stellar magnetic fields. This modification of the pressure-temperature structure influences the formation of absorption spectral features producing characteristic rotational variability of some spectral lines, especially the Balmer lines (Valyavin et al., 2004 and references therein). In order to study these theoretical predictions we began systematic spectroscopic survey of Balmer line variability in spectra of brightest CP magnetic stars. Here we present the first results of the program. A0p star $\Theta$ Aur revealed significant variability of the Balmer profiles during the star's rotation. Character of this variablity corresponds to that classified by Kroll (1989) as a result of an impact of significant Lorentz force. From the obtained data we estimate that amplitudes of the variation at H$\alpha$, H$\beta$, H$\gamma$ and H$\delta$ profiles reach up to $2.4\%$during full rotation cycle of the star. Using computation of our model atmospheres (Valyavin et al., 2004) we interpret these data within the framework of the simplest model of the evolution of global magnetic fields in chemically peculiar stars. Assuming that the field is represented by a dipole, we estimate the characteristic e.m.f. induced by the field decay electric current (and the Lorentz force as the result) on the order of $E {\~} 10^{-11}$ cgs units, which may indicate very fast (< < $10^{10}$ years) evolution rate of the field. This result strongly contradicts the theoretical point of view that global stellar magnetic fields of CP stars are fossil and their the characteristic decay time of about $10^{10}$ yr. Alternatively, we briefly discuss concurring effects (like the ambipolar diffusion) which may also lead to significant atmospheric currents producing the observable Lorentz force.

• 한국세라믹학회지
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• 제34권6호
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• pp.629-635
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• 1997

The effects of the annealing atmospheres(O2, N2) and sintering additives that Bi2O3 is a major composition on the microwave dielectric and sintering propertie of (1-x)CaTiO3-xLaAlO3 system were investigated. The annealing atmospheres and the increase of annealing time after sintering did not affect the relative dielectric constant($\varepsilon$r) and temperature coefficient of resonant frequency($\tau$f) of (1-x)CaTiO3-xLaAlO3 system. However, the Q.f0 values of (1-x)CaTiO3-xLaAlO3 were very sensitive to annealing atmospheres. As the annealing time increased under O2 atmosphere the Q.f0 values of (1-x)CaTiO3-xLaAlO3 enhanced untill 10 hrs in 0.3$\leq$x$\leq$0.6 region, but degraded over that time. The increasing rate of Q.f0 value increased wth increasing x. On the other hand, as the annealing time increased under N2 atmosphere the Q.f0 values were constant in x$\leq$0.6 region, increased gradually in x$\geq$0.7 region. When 0.97Bi2O3-0.03Al2O3 and 0.76Bi2O3-0.24NiO of 3wt% as sintering additives were added to (Ca0.5La0.5) (Ti0.5Al0.5)O3 (x=0.5) the sintering temperature of 1$600^{\circ}C$ was lowered to 140$0^{\circ}C$, and the relative dielectric constant($\varepsilon$r) and temperature coefficient of resonant frequency($\tau$f) were not nearly changed. The addition of 0.97Bi2O3-0.03Al2O3 and 0.76Bi2O3-0.24NiO of 3wt% to (Ca0.5La0.5)(Ti0.5Al0.5)O3 made the Q.f0 values to be lower about 15% and 34%, respectively.

• 한국가스학회지
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• 제23권4호
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• pp.46-64
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• 2019

폭발위험장소의 선정과 거리계산에 대한 상세기술기준 KGS GC101 2018(가스시설의 폭발위험장소 종류 구분 및 범위 산정에 관한 기준)이 제정되어, 2018년 7월 12일부터 시행되었다. IEC60079-10-1 2015 (Explosive atmospheres Part 10-1: Classification of areas - Explosive gas atmospheres)에 대한 전수 내용을 정리하고, 모호한 기준의 해석이나 기준에 대한 가이드라인을 추가하여 제정하였다. KGS GC101은 폭발위험장소 종류의 구분을 위한 방법으로 (1)누출등급의 결정 (2)누출 홀 크기의 결정 (3)누출유량의 결정 (4)희석등급의 결정 (5)환기유효성의 결정을 통하여 최종적으로 (6)위험장소의 결정 (7) 폭발위험장소 범위의 산정을 할 수 있다. 이 과정을 쉽게 계산하기 위하여 Visual Basic for Application (Excel) 언어로 구성한 프로그램(KGS-HAC, C-2018-020632)을 한국가스안전공사에서 제작하였고, 현재 시범 사용 중(2019년 4월 1일 현재 v1.14)에 있다. 그럼에도 불구하고 현장에서 어려워하여, 본 논문을 통하여 코드 및 프로그램의 사용법을 설명하는 것으로 해결코자 한다.

• Nuclear Engineering and Technology
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• 제26권4호
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• pp.484-492
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• 1994

Nb$_2$O$_{5}$가 첨가된 $UO_2$ 소결체의 미세조직을 수소와 이산화탄소 분위기에서 연구하였다. Pellet을 1$700^{\circ}C$ 수소분위기 그리고 130$0^{\circ}C$ 이산화탄소 분위기에서 1-41 시간 동안 소결하였다. Nb$_2$O$_{5}$를 첨가하면 큰 기공들이 형성되고, 이 기공들은 수소분위기에서는 어느정도 수축하지만 이산화탄소 분위기에서는 거의 소멸하지 않는다. 작은 기공들은 수소분위기에서는 거의 전부 소멸되며 이산화탄소 분위기에서는 거의 소멸하지 않는다. 그리고 결정립의 크기도 수소분위기에서 훨씬 증대한다. 따라서 Nb$_2$O$_{5}$ 첨가에 의한 우라늄 확산은 수소분위기에서 훨씬 증가하는 것으로 생각된다. 수소 분위기에서 소결한 Nb$_2$O$_{5}$ 첨가 $UO_2$ pellet의 미세조직을 노내성능의 관점에서 평가하였다. 우라늄 확산의 증가를 설명하기 위해서 Nb$_2$O$_{5}$ 첨가에 의해서 형성 가능한 결함들을 고찰하였다.함들을 고찰하였다.

• 천문학회보
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• 제29권2호
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• pp.42.1-42.1
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• 2004

• 한국원자력학회:학술대회논문집
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• 한국원자력학회 2002년도 추계학술발표회요약집
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• pp.275-275
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• 2002

• 한국섬유공학회:학술대회논문집
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• 한국섬유공학회 2001년도 학술발표회 논문집(Proceedings of the Korean Textile Conference) 상
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• pp.63-66
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• 2001

• 한국원자력학회:학술대회논문집
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• 한국원자력학회 2004년도 요약집 춘계학술발표대회
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• pp.309.1-309.1
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• 2004