We present an updated version of the multilayer spectral inversion (MLSI) recently proposed as a technique to infer the physical parameters of plasmas in the solar chromosphere from a strong absorption line. In the original MLSI, the absorption prole was constant over each layer of the chromosphere, whereas the source function was allowed to vary with optical depth. In our updated MLSI, the absorption prole is allowed to vary with optical depth in each layer and kept continuous at the interface of two adjacent layers. We also propose a new set of physical requirements for the parameters useful in the constrained model tting. We apply this updated MLSI to two sets of Hα and Ca ii line spectral data taken by the Fast Imaging Solar Spectrograph (FISS) from a quiet region and an active region, respectively. We nd that the new version of the MLSI satisfactorily ts most of the observed line proles of various features, including a network feature, an internetwork feature, a mottle feature in a quiet region, and a plage feature, a superpenumbral bril, an umbral feature, and a fast down ow feature in an active region. The MLSI can also yield physically reasonable estimates of hydrogen temperature and nonthermal speed as well as Doppler velocities at different atmospheric levels. We conclude that the MLSI is a very useful tool to analyze the Hα line and the Ca ii 8542 line spectral daya, and will promote the investigation of physical processes occurring in the solar photosphere and chromosphere.

About 10 percent of quasars are known to exhibit deep broad absorption troughs blueward of prominent permitted emission lines, which are usually attributed to the existence of outflows slightly above he accretion disk around the supermassive black hole. Typical widths up to 0.2c of these absorption roughs indicate the velocity scales in which special relativistic effects may not be negligible. Under he assumption of the ubiquity of the broad absorption line region in quasars, the broad emission line flux will exhibit Thomson scattered components from these fast outflows. In this paper, we provide our Monte Carlo calculation of linear polarization of singly Thomson scattered line radiation with the careful considerations of special relativistic effects. The scattering region is approximated by a collection of rings that are moving outward with speeds υ =cβ < 0.2c near the equatorial plane, and the scattered line photons are collected according to its direction and wavelength in the observer's rest frame. We find that the significantly extended red tail appears in the scattered radiation. We also find that the linear degree of polarization of singly Thomson scattered line radiation is wavelength-dependent and hat there are significant differences in the linear degree of polarization from that computed from classical physics in the far red tail. We propose that the semi-forbidden broad emission line C III]1909 may be significantly contributed from Thomson scattering because this line has small resonance scattering optical depth in the broad absorption line region, which leads to distinct and significant polarized flux in this broad emission line.

In this paper, we present observations of absorption line spectrum of QSO 1225+317 with resolution of 18 km sec-1. Four possible new heavy element line systems are identified. The properties of Lyman α forest lines are discussed.

본 연구에서는 자연에서 산출빈도가 높은 3가 비소(아비산염)와 two-line ferrihydrite와의 표면흡착반응의 기작을 살펴보기 위하여 3가 비소를 흡착시킨 two-line ferrihydrite에 대한 X선 흡수분광 분석을 수행하였다 연구에 사용된 two-line ferrihydrite는 실험실에서 합성하여 사용하였으며, 산성과 염기성 환경에서의 표면반응 기작을 비교하기 위하여 pH 4와 10에서 연구를 수행하였다. 또한 각 pH 조건별 3가 비소의 흡착농도에 따른 표면반응의 차이를 비교 평가하였다. X선 흡수분광 분석결과에서 얻은 EXAFS 영역에서의 비소 3가에 대한 구조 변수들을 살펴보면 As-O 배위수는 3.1~3.3개 거리는 1.74~1.79 a으로 two-line ferrihydrite 표면에 흡착된 As(III) complex의 구조 단위체가 AsO3임이 확인되었다. As(III)-Fe쌍은 주로 안정된 형태의 bidentate binuclear comer-sharing (2C)의 결합구조를 갖는 것으로 나타났으며, bidentate mononuclear edge-sharing (2E)와 2C가 혼합된 결합구조도 공존하는 것으로 조사되었다. pH 4에서는 흡착농도에 따라 다른 표면구조를 가지는 반면, pH 10에서는 흡착 농도에 상관없이 동일한 표면구조를 보이는 것으로 나타났다. 이러한 결과는 3가 비소와 two-line ferrihydrite의 표면반응은 pH와 농도에 의해서 영향을 받는다는 거시적인(macroscopic) 흡착실험 연구결과가 미시적인(microscopic) X선 흡수분광 결과에 의해서 해석될 수 있음을 의미한다.