• 천문학회지
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• 제48권3호
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• pp.195-202
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• 2015

Star forming galaxies found in the early universe exhibit asymmetric Lyα emission line that results from multiple scattering in a neutral thick medium surrounding the Lyα emission source. It is expected that emergent Lyα will be significantly polarized through a large number of resonance scattering events followed by a number of successive wing scatterings. In this study we adopt a Monte Carlo method to calculate the polarization of Lyα transferred in a very thick static slab of H_I. Resonantly scattered radiation associated with transitions between is only weakly polarized and therefore linear polarization of the emergent Lyα is mainly dependent on the number of off-resonant wing scattering events. The number of wing scattering events just before escape from the slab is determined by the product of the Doppler parameter a and the line center optical depth τ₀, which, in turn, determines the behavior of the linear polarization of Lyα. This result is analogous to the study of polarized radiative transfer of Thomson scattered photons in an electron slab, where the emergent photons are polarized in the direction perpendicular to the slab when the scattering optical depth is small and polarized in the parallel direction when the slab is optically thick. Our simulated spectropolarimetry of Lyα shows that the line center is negligibly polarized, the near wing parts polarized in the direction parallel to the slab and the far wing parts are polarized in the direction perpendicular to the slab. We emphasize that the flip of polarization direction in the wing parts of Lyα naturally reflects the diffusive nature of the Lyα transfer process in thick neutral media.

• 천문학회보
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• 제30권2호
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• pp.74.1-74.1
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• 2005

• 한국인터넷방송통신학회논문지
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• 제22권1호
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• pp.29-34
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• 2022

본 논문에서는 접지된 2중 유전체층 사이의 저항띠 격자구조에 의한 H-polarized 산란 문제는 전자파 수치해석 방법으로 알려진 PMM(point matching method)을 이용하여 해석하였다. 경계조건들은 미지의 계수를 구하기 위하여 이용하였고, 산란 전자계는 Floquet 모드 함수의 급수로 전개하였고, 저항띠의 해석을 위해 저항경계조건을 적용하였다. 유전층의 비유전율과 정방행렬의 행수의 크기에 따른 반사전력의 수렴도의 %error를 비교하였으며, 정방행렬의 행수의 크기가 클수록 반사전력의 정확도는 증가하였다. 저항띠의 저항율이 작아지거나, 유전층의 두께가 작아지거나, 그리고 유전체 층의 비유전율이 증가하면, 반사전력은 증가하였다. 접지된 2중 유전체층을 가지는 본 논문의 제안된 구조에 대한 수치결과들은 기존 논문의 수치해석 결과들과 비교하여 잘 일치하였다.

• 천문학회보
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• 제41권2호
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• pp.33.2-34
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• 2016

The unification model of active galactic nuclei invokes the presence of a thick molecular torus that hides the broad emission line region from a line of sight toward observers with low latitude. It is expected that the illuminated side of the molecular torus may be photodissociated by strong far UV radiation from the central AGN, forming an H I region with a high neutral column density. We propose that the Rayleigh scattering optical depth of this HI region can be significant for most broad $Ly{\alpha}$ line photons with the Doppler factor not exceeding 104 km s-1. Rayleigh scattered $Ly{\alpha}$ photons can be characterized by strong linear polarization depending on their scattering optical depth. We performed Monte Carlo simulations of polarized radiative transfer of $Ly{\alpha}$ adopting simple scattering geometries relevant to the unification model of AGN. We find that for a low torus the Rayleigh scattered $Ly{\alpha}$ is polarized in the direction parallel to the symmetry axis with the polarization degree dependent on wavelength. In the case of a high torus, the core part of $Ly{\alpha}$ is polarized in the direction perpendicular to the symmetry axis whereas the wing part is parallelly polarized. We conclude that careful spectropolarimetry around $Ly{\alpha}$ can be useful in testing the AGN unification model.

• 한국초전도ㆍ저온공학회논문지
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• 제26권1호
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• pp.14-19
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• 2024

In this study, we explore the anisotropy of electron-phonon coupling (EPC) constant in epitaxially grown MgB₂ films on c-axis oriented Al₂O₃, examining its correlation with the critical temperature (T_c) and local structural disorder assessed through polarized Raman scattering. Analysis of the polarized Raman spectra reveals angle-dependent variations in the intensity of the phonon spectra. The Raman active mode originating from the boron plane, along with two additional phonon modes from the phonon density of states (PDOS) induced by lattice distortion, was distinctly observed. Persistent impurity scattering, likely attributed to oxygen diffusion, was noted at consistent frequencies across all measurement angles. The EPC values derived from the primary Raman active phonon do not significantly vary with changing observation angles, followed by that the T_c values calculated using the Allen and Dynes formula remain relatively constant across all polarization angles. Although the E_2g phonon mode plays a crucial role in the EPC mechanism, the determination of T_c values in MgB₂ involves not only electron-E_2g coupling but also contributions from other phonon modes.

• 한국항행학회논문지
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• 제15권3호
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• pp.349-354
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• 2011

본 논문에서는 스트립 폭과 격자주기, 유전체 층의 비유전율과 두께, 그리고 transverse electric (TE) 평면파의 입사각에 따른 접지된 유전체 평면위의 스트립 양끝에서 0 저항율을 갖는 저항띠 격자구조에 의한 H-분극산란 문제를 Fourier-Galerkin Moment Method (FGMM)를 이용하여 해석하였다. 저항띠의 변하는 저항율은 저항띠의 양끝에서 0으로 변하는 경우를 취급하였고, 이때 저항띠 위에서 유도되는 전류밀도는 직교다항식의 일종인 2종 Chebyshev 다항식의 급수로 전개하였다. 반사전력의 급변점들은 공진효과에 기인한 것으로 과거에 wood's anomallies라고 불리워지며, 반사전력에 대한 수치결과들은 기존 논문의 균일 저항율의 수치 결과들과 비교하였다.

• 한국항행학회논문지
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• 제15권4호
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• pp.543-548
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• 2011

본 논문에서는 스트립 폭과 격자주기, 유전체 층의 비유전율과 두께, 그리고 TE(transverse electric) 평면파의 입사각에 따른 접지된 유전체 평면위의 변하는 저항율을 갖는 저항띠 격자구조에 의한 H-분극 전자파 산란문제를 FGMM(Fourier-Galerkin Moment Method)를 이용하여 해석하였다. 저항띠의 변하는 저항율은 한쪽 모서리에서는 유한하고 다른쪽 모서리에서 0 저항율을 가지며, 이때 저항띠 위에서 유도되는 표면 전류밀도는 직교다항식의 일종인 차수가 ${\alpha}=1$, ${\beta}=0$인 Jacobi 다항식의 급수로 전개하였다. 정규화된 반사전력의 수치결과는 기존의 수치결과와 매우 일치하였다.

• 한국인터넷방송통신학회논문지
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• 제20권1호
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• pp.77-82
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• 2020

본 논문에서는 2중 유전체층 사이의 완전도체띠 격자구조에 의한 E-분극 전자파 산란 문제는 전자파 수치해석 방법으로 알려진 FGMM(Fourier-Galerkin moment method)를 이용하여 해석하였다. 경계조건들은 미지의 계수를 구하기 위하여 이용하였고, 도체띠의 해석을 위해 완전도체 경계조건을 적용하였다. 도체띠의 폭과 주기, 2중 유전층 사이의 비유전율과 두께 및 입사각에 대해 정규화된 반사전력과 투과전력을 계산하였다. 전반적으로 2중 유전체 층의 비유전율이 증가할수록 반사전력은 증가하였으며, 상대적으로 투과전력은 감소하였다. 2중 유전체 층의 비유전율이 증가할수록 도체띠에 유도되는 전류밀도는 스트립 중앙에서 증가하였다. 본 논문의 제안된 구조에 대한 수치결과들은 기존 논문의 수치해석 결과들과 비교하여 매우 잘 일치하였다.

• 천문학회보
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• 제46권2호
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• pp.40.1-40.1
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• 2021

Hydrogen is the most abundant element in the universe, which is, in the cosmological context, attributed to its simplest structure consisting of a proton and an electron. Hydrogen interacts with an electromagnetic wave in astrophysical environments. Rayleigh scattering refers to elastic scattering, where the frequencies of the incident and scattered photons are the same. Rayleigh and resonance scattering is a critical role study Lyman Alpha objects in the early universe. The scattering causes the frequency and spatial diffusion of Lyα. In the case of Raman scattering, the energies of the incident and scattered photons are different. The photons near Lyβ convert to the optical photons near Hα through Raman scattering. The photon scattered by atomic hydrogen can carry both of the properties of the H I region and the emission region. I adopt a Monte Carlo approach to investigate the formation of the various spectral line features through Rayleigh and Raman scattering in highly thick media of atomic hydrogen. In this thesis, I present my works on radiative transfer involving the scattering processes between far UV photon and atomic hydrogen. I introduce scattering processes with atomic hydrogen and the spectral, spatial, and polarized information originating from the scattering.

• 천문학논총
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• 제15권spc1호
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• pp.147-151
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• 2000

Symbiotic stars, believed to be binary systems of a mass-losing giant and a white dwarf with an emission nebula, are known to exhibit very broad wings around Hex that extend to $\~10^3km\;s^{-1}$. The wing formation mechanism is not a settled matter and recently Lee (2000) proposed that Raman scattering of Ly$\beta$ by neutral hydrogen is responsible for the broad H$\alpha$ wings. In this model, it is predicted that. the Hex wings will be polarized depending on the geometric and kinematic distribution of the scatterers relative to the UV emission region. In this paper, we investigate the polarization of Hex wings in symbiotic stars. Noting that many symbiotic stars possess bipolar nebular morphology, we assume that the distribution of neutral scatterers follows the similar pattern with a receding velocity of several tens of km $s^{-1}$ that mimics the expansion of the neutral envelope of the nebula. It is found that the red wing is more strongly polarized than the blue and main part and that the polarization direction is along the equatorial plane. We obtain a typical degree of polarization $\~10$ percent, however, it varies depending on the detailed distribution of H I scatterers We conclude that spectropolarimetry will provide very important information on the origin of the Hex wings.