• Journal of Astronomy and Space Sciences
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• 제13권1호
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• pp.79-89
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• 1996

We calculate the theoretical line profiles for 32 Cyg in order to investigate the influence of various velocity fields. Line profiles are calculated with wind accelerations driven by Alfven waves and described by velocity parameters. The results for Alfvenic wave model show weakened line profiles. For the orbital phases ${\Phi}$=0.78 and ${\Phi}$=0.06 the Alfvenic models show strong absorption part due to very low densities at the surface of the supergiant. Hence, we conclude the velocity gradient of the wind near the supergiant could influence on the theoretical line formation.

• 천문학회지
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• 제29권spc1호
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• pp.235-236
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• 1996

Using a phenomenological model for the accretion onto the magnetic white dwarf, we calclliated some optical line profiles from the magnetosphere of such systems. Line profiles of these systems seem to be produced in the magnetosphere of the compact star due to the reemission of X-ray produced near the stellar surface. Some results of our new calculation and the analysis of these results will be presented. Our results show that the model used here can reproduce the observed optical line profiles and open the possiblity to determine the parameters of individual systems.

• Journal of Astronomy and Space Sciences
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• 제9권2호
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• pp.165-170
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• 1992

$\zeta$ Aur형의 쌍성계인 32 Cyg 에 대해 복사 전달 방정식을 수치적분하여 이론적인 선 윤곽을 구하였다. 원천함수를 구하기 위해 2 준위 원자와 완전 재분배를 가정 하고 Sobolev 근사를 이용하였다. 선 윤곽을 궤도위상에 따라 구한 결과, 공전궤도 위상 0.99에서는 선 윤곽이 적색편이를 보였으며, 공전궤도 위상 0.70에서는 파장이 짧은 쪽으로 약간 치우쳤다. 또한 궤도면 기울기에 따른 효과를 보기 위해 같은 위상에서 각기 다른 기울기를 주고 계산하였는데, 기울기가 작은 경우에 빛의 세기가 증가하였다.

• 천문학회보
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• 제43권1호
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• pp.35.3-35.3
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• 2018

Incorporating the fully quantum mechanical computation of scattering cross-section and statistical moment analysis of absorption profiles, we investigate the Lyman line asymmetry of extremely high column density systems. Recent high redshift observations detected strong damped Lyman alpha systems (DLAs) whose column density is larger than N_HI ~ [10]^21.3 cm^(-2). Absorption profiles of these DLAs are characterized by the broad and asymmetric damping wing. For accurate description of radiation damping, the second-order time-dependent perturbation theory is adopted. To quantitatively address line asymmetry, we define a distribution function for each Lyman line, and compute statistical moments (mean, standard deviation, skewness and kurtosis) regarding column densities N_HI > [10]^18 cm^(-2). In this work, we present statistical properties of the intrinsic line profiles, and compare them with the Lorentzian cases.

• Journal of Astronomy and Space Sciences
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• 제15권1호
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• pp.101-110
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• 1998

32Cyg의 B형 별 주위에 형성된 $str{\"{o}}mgren$ 구를 가정하고 공전궤도위상 0.06과 0.78에서 이론적인 선 윤곽을 계산하였다. 항성 풍의 속도분포에 따라 alfv n 파 모형의 선윤곽이 누승 함수의 속도 분포를 이용한 모형의 선 윤곽 보다 전체적으로 낮은 세기를 보였다. HII 모형은 HII 영역이 없는 경우보다 약한 선 윤곽을 보였으나 $\phi$ = 0.06에서는 HII 영역이 없는 모형이 HII 영역을 가진 모형에 비해 단지 적색편이 쪽에서만 약간의 차이를 보였다. 한편 $\phi$ = 0.79에서 HII 영역을 가진 $Alfv{\'{e}}n$ 파 모형의 선 윤곽은 적색편이와 청색 편이 쪽에서 각각 다른 속도기울기의 누승 함수 모형으로써 나타낼 수 있었다. 이는 급격한 초기 속도 기울기를 고려하여 2개의 가속영역을 가진 누승 함수 모형이라면 항성 풍의 가속과정을 고려하지 않음으로써 생기는 오차를 줄일 수 있음을 의미한다.의미한다.

• 천문학회보
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• 제35권2호
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• pp.73.1-73.1
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• 2010

Using the spectroscopic data secured with the Hamilton Echelle Spectrograph attached to a 3-m telescope at the Lick Observatory, we derived the expansion velocities from various line profiles in the 3600 $\AA$ to 10,000 $\AA$ based on the full width at half maximum and double peak of the high dispersion line profiles. The symmetrical shapes of the permitted line profiles indicate that the permitted line zone is symmetrical e.g., a spherical shell or bipolar + torus structures, which might be evidence of relatively recent ejection from the central star. Most other stronger forbidden lines might be coming from a main shell which appears as a bilateral symmetrical morphology, seen in HST and other ground-based telescopic images. The overall expansion velocities of this main shell structure that are responsible for most lines, seem to show the Hubble type expansion, i.e., accelerating shell. The faster expansion velocities of the permitted OII, NII, NIII and perhaps CII lines that do not suit to the Hubble type expansion, imply the existence of a somewhat smaller inner shell inside the outer main shell. We conclude that the nebular shell consists of a swiftly expanding inner shell and an outer normal shell excited by a central star of about 55,000K. The former compact zone appears to be responsible for the permitted C, N, and O lines while the latter extended shell appears to be responsible for H, He, and forbidden lines. We present some evidence that NGC 6833 be a member of the Galactic halo.

• 천문학회지
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• 제25권2호
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• pp.67-78
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• 1992

Effects of cloud rotation 011 the profiles of CO J=$1{\rightarrow}0$ lines arc investigated by theoretically general ing line profiles under physical conditions similar to t he ones in large globules. The synthesized profiles are presented and their characteristics are discussed. It is found that when the Doppler shift of the observed CO lines is interpreted as the rotation velocity, the optically thin $^{13}CO$ lines underestimate the rotation velocity by up to 10 percents, while the self-reversed optically thick $^{12}CO$ lines overestimate the velocity up to 20 percents. The optically thin line is shown to be of use in probing the distribution of rotation velocity in dark globules.

• 천문학회지
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• 제35권3호
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• pp.123-130
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• 2002

An elliptical accretion disk may be formed by tidally disrupted debris of a flying-by star in an active galactic nucleus (AGN) or by tidal perturbation due to a companion in a binary black hole system. We investigate the iron K$\alpha$ line profiles expecting from a geometrically thin, relativistic, elliptical disk in terms of model parameters, and find that a broad and skewed line profile can be reproduced well. Its shape is variable to the model parameters, such as, the emissivity power-law index, the ellipticity of the disk, and the major axis orientation of the elliptical accretion disk. We suggest that our results may be useful to search for such an elliptical disk and consequently the tidal disruption event.

• 천문학회지
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• 제35권4호
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• pp.175-185
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• 2002

Almost half of primeval galaxies show P-Cygni type profiles in the Ly$\alpha$ emission line. The main underlying mechanism for the profile formation in these systems is thought to be the frequency re-distribution of the line photons in expanding scattering media surrounding the emission source. A Monte Carlo code is developed to investigate the Ly$\alpha$ line transfer in an optically thick and moving medium with a careful consideration of the scattering in the damping wings. Typical column densities and expansion velocities of neutral hydrogen investigated in this study are $N_{H1}{\~}10^{17-20}\;cm^{-2}$ and ${\Delta}V{\~} 100 km\;s^{-1}$. We investigate the dependence of the emergent profiles on the kinematics and on the column density. Our numerical results are applied to show that the damped Ly$\alpha$ absorbers may possess an expanding H I supershell with bulk flow of ${\~}200 km\;s^{-l}$ and H I column density $N_{H1}{\~}10^{19}\;cm^{-2}$. We briefly discuss the observational implications.

• 소성∙가공
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• 제24권2호
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• pp.107-114
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• 2015

The current study presents a geometric measurement and analysis of the section profile for a feature line surface on an automotive outer panel. A feature line surface is the geometry which is a visually noticeable creased line on a smooth panel. In the current study the section profile of a feature line surface is analyzed geometrically. The section profile on the real press panel was measured using a coordinate measuring machine. The section profiles from the CAD model and the real panel are aligned using the same coordinate system defined by two holes near the feature line. In the aligned section profiles the chord length and height of the curved part were measured and analyzed. The results show that the feature line surface on the real panel is doubled in width size.