A small number of active galactic nuclei are known to exhibit prominent double peak emission profiles that are well-fitted by a relativistic accretion disk model. We develop a Monte Carlo code to compute the linear polarization of a double peaked broad emission line arising from Thomson scattering. A Keplerian accretion disk is adopted for the double peak emission line region and the geometry is assumed to be Schwarzschild. Far from the accretion disk where flat Minkowski geometry is appropriate, we place an azimuthally symmetric scattering region in the shape of a spherical shell sliced with Δμ =0.1. Adopting a Monte Carlo method we generate line photons in the accretion disk in arbitrary directions in the local rest frame and follow the geodesic paths of the photons until they hit the scattering region. The profile of the polarized flux is mainly determined by the relative location of the scattering region with respect to the emission source. When the scattering region is in the polar direction, the degree of linear polarization also shows a double peak structure. Under favorable conditions we show that up to 0.6% linear polarization may be obtained. We conclude that spectropolarimetry can be a powerful probe to reveal much information regarding the accretion disk geometry of these active galactic nuclei.

Magnetars are neutron stars possessing a magnetic field of about 1014-1015 G at the surface. Thermodynamic properties of neutron star matter, approximated by pure neutron matter, are considered at finite temperature in strong magnetic fields up to 1018 G which could be relevant for the inner regions of magnetars. In the model with the Skyrme effective interaction, it is shown that a thermodynamically stable branch of solutions for the spin polarization parameter corresponds to the case when the majority of neutron spins are oriented opposite to the direction of the magnetic field (i.e. negative spin polarization). Moreover, starting from some threshold density, the self-consistent equations have also two other branches of solutions, corresponding to positive spin polarization. The influence of finite temperatures on spin polarization remains moderate in the Skyrme model up to temperatures relevant for protoneutron stars. In particular, the scenario with the metastable state characterized by positive spin polarization, considered at zero temperature in Phys. Rev. C 80, 065801 (2009), is preserved at finite temperatures as well. It is shown that, above certain density, the entropy for various branches of spin polarization in neutron matter with the Skyrme interaction in a strong magnetic field shows the unusual behavior, being larger than that of the nonpolarized state. By providing the corresponding low-temperature analysis, we prove that this unexpected behavior should be related to the dependence of the entropy of a spin polarized state on the effective masses of neutrons with spin up and spin down, and to a certain constraint on them which is violated in the respective density range.

지진전조현상을 모니터링 하기 위해 기상청이 운영하고 있는 청양 지자기관측소에서 총 6개월간 획득된 지자기장 자료를 분석하였다. 지자기 3성분 자료로부터 지하의 전기비저항 변화를 반영하는 전달함수 및 분극값을 계산하였고, 이를 동일기간 발생한 지진이벤트와 비교하였다. 전달함수의 경우 일별 전달함수 값의 변화가 상당히 심하였으며, 발생한 지진 및 Kp 인덱스와의 상관성을 찾기 어려웠다. ULF 대역 자기장은 지진발생 전 뚜렷한 분극값의 증가가 관찰되었으나, 지진이 발생하지 않은 기간에도 이러한 변동 패턴이 나타났다. 따라서 이러한 분극값의 변화는 지진 전조현상으로 단정하기에는 한계가 있고, 향후 타 관측소 자료의 추가적인 확보 및 분석을 통해 과거 발생한 일정규모 이상의 지진과 관련성을 분석할 필요가 있다.

Recently far infra-red (FIR) polarization of the 850μm continuum emission from T Tauri disks has been detected. The observed degree of polarization is around 3 %. Since thermal emission from dust grains dominates the spectral energy distribution at the FIR regime, dust grains might be the cause of the polarization. We explore alignment of dust grains by radiative torque in T Tauri disks and provide predictions for polarized emission for disks viewed at different wavelengths and viewing angles. In the presence of magnetic field, these aligned grains produce polarized emission in infrared wavelengths. When we take a Mathis-Rumpl-Nordsieck-type distribution with maximum grain size of 500-1000μm the degree of polarization is around 2-3 % level at wavelengths larger than ~100μm Our study indicates that multifrequency infrared polarimetric studies of protostellar disks can provide good insights into the details of their magnetic structure.

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.

전기투석은 이온성 물질을 분리하고 농축하는데 안정하고 효과적인 공정으로 알려져 있다. 그러나 전기투석 공정은 고가의 이온교환막 때문에 실제 공정에 적용하는데 많은 제한을 받아오고 있다. 따라서 전기 투석공정의 운전 전류밀도를 가능한 높게 공급함으로써 이온교환막의 단면적당 flux를 증가시켜 주어야 한다. 그러나 실제 공정의 운전에 있어서 운전 전류밀도는 이온교환막 표면에서의 농도분극 현상으로 제한을 받게 된다. 본 총설에서는 이온교환막을 통한 이온의 이동현상을 설명하고 전류-전압 곡선을 이용한 막특성 분석을 소개하였다. 또한 한계전류밀도 전후의 전류 영역에서 농도분극 현상과 동반하는 전기대류(Electroconvection), 물 분해 현상 등에 대한 최근 연구결과를 정리하였다.

We have made a topological study of cosmic microwave background (CMB) polarization maps by simulating the AMiBA experiment results. A ACDM CMB sky is adopted to make mock interferometric observations designed for the AMiBA experiment. CMB polarization fields are reconstructed from the AMiBA mock visibility data using the maximum entropy method. We have also considered effects of Galactic foregrounds on the CMB polarization fields. The genus statistic is calculated from the simulated Q and U polarization maps, where Q and U are Stokes parameters. Our study shows that the Galactic foreground emission, even at low Galactic latitude, is expected to have small effects on the CMB polarization field. Increasing survey area and integration time is essential to detect non-Gaussian signals of cosmological origin through genus measurement.