We use simulations of large-scale structure formation to study the build-up of magnetic fields (MFs) in the intergalactic medium. Our basic assumption is that cosmological MFs grow in a magnetohy-drodynamical (MHD) amplification process driven by structure formation out of a magnetic seed field present at high redshift. This approach is motivated by previous simulations of the MFs in galaxy clusters which, under the same hypothesis that we adopt here, succeeded in reproducing Faraday rotation measurements (RMs) in clusters of galaxies. Our ACDM initial conditions for the dark matter density fluctuations have been statistically constrained by the observed large-scale density field within a sphere of 110 Mpc around the Milky Way, based on the IRAS 1.2-Jy all-sky redshift survey. As a result, the positions and masses of prominent galaxy clusters in our simulation coincide closely with their real counterparts in the Local Universe. We find excellent agreement between RMs of our simulated galaxy clusters and observational data. The improved numerical resolution of our simulations compared to previous work also allows us to study the MF in large-scale filaments, sheets and voids. By tracing the propagation of ultra high energy (UHE) protons in the simulated MF we construct full-sky maps of expected deflection angles of protons with arrival energies E = 1020 eV and 4 X 1019 eV, respectively. Accounting only for the structures within 110 Mpc, we find that strong deflections are only produced if UHE protons cross galaxy clusters. The total area on the sky covered by these structures is however very small. Over still larger distances, multiple crossings of sheets and filaments may give rise to noticeable deflections over a significant fraction of the sky; the exact amount and angular distribution depends on the model adopted for the magnetic seed field. Based on our results we argue that over a large fraction of the sky the deflections are likely to remain smaller than the present experimental angular sensitivity. Therefore, we conclude that forthcoming air shower experiments should be able to locate sources of UHE protons and shed more light on the nature of cosmological MFs.

The purpose of this paper is analyses about in 12kV/50kA vacuum interrupter with an axial magnetic field type electrode system through the studies of electromagnetic phenomena for the possess of Safety break. Vacuum interrupter is important in electric safety part. In this paper, we performed analysis of electric field, magnetic field, current density in AMF electrode using the Maxwell 3D simulation.

최근 널리 개발되고 있는 디지털형 지자기 감지형 컴퍼스의 전자장에서의 다양한 성능을 펑가하기 위한 3축형 인공자장발생장치를 실험적으로 제작하고, 그 성능 특성을 검토한 결과는 다음과 같다. 1. 3축형 인공자장발생장치의 X,Y,X 각축에 대한 자력의 변화는 전류의 증가에 따라 선형적으로 증가하였고, 측정치는 이론치와의 비교에서도 그 차의 평균 범위가 0.33～1.93uT로 이론치와 거의 일치하여 제작된 인공자장발생장치의 성능은 양호한 것으로 판단된다. 2. 헬름홀츠 코일내의 가장자리에서는 다소 불규칙한 자력의 변화가 발생하였지만, 중심으로 갈수록 그 변동이 안정되는 경향을 나타내었다. 3. 자기 컴퍼스의 제진특성의 측정치와 이론치와의 비교에서 수평자력 0.30gauss 및 0.40gauss 에서는 성능이 양호한 것으로 판단되나, 수평자력 0.50gauss 에서는 다소 큰 차이가 나타내어 0.40gauss 이상의 비교적 높은 자력에서는 신뢰도가 낮은 것으로 판단되었다. 4. 0.30gauss 의 자장 속에서 측정된 수반각은 1rpm의 회전속도에서 1˚로서 이 값은 국제성능 표준규격(6 ˚미만)에 적합하였다.

대전력을 사용하는 제강공장의 L/F설비에서 발생되는 강자계를 효율적으로 차폐하기 위하여 L/F주위의 자기장 분포를 유한해석법을 이용한 사용해석도구인 ANSYS 5.3 3차원 자기장해석기를 통해 해석하고 그 결과를 평판형태의 차폐체에 적용시키고자 하였다. 분석결과, L1 및 L2가 각각 2.7 및 2.9m 이려 높이가 3.5m인 2중차폐체(1차측 차폐: 1mmt의 전기강판, 2차측차폐: 1mmt의 Fe-Ni alloy sheet)를 설치하는 거싱 최적의 처폐방안으로 도출되었다.

We have obtained theoretical calibration curves to convert the amount of polarization into the strength of magnetic field, by a numerical calculation of radiation transfer for the polarized spectral line of FeI 6303\AA. In our calculation, three kinds of atmospheric models (VAL-C, penumbra, umbra) have been used to make a proper calibration for an active region composed of quiet, penumbral and umbral areas. It was found that firstly, the results of our calculation depend highly on a kind of atmospheric model rather than on any other input parameters used in a model. Secondly, observed line profile showed m solar spectrum atlas proved to be very similar to the calculated profiles obtained by using a penumbra model. Finally, another method except this calibration curve should be developed to estimate correctly the distribution of magnetic field in solar active region from the observation of polarized spectral line.

We examine the observations of large-scale magnetic fields in the Universe. We begin at the largest scale with clusters of galaxies and work our way down through galaxies and finally to the Milky Way. on which we concentrate in detail. We examine the observations of the Galactic magnetic field, and their interpretation, under the philosophy that the Galactic magnetic field is like that in other spiral galaxies. We use pulsar data. diffuse Galactic synchrotron emission, and starlight polarization data to discuss the Galaxy's global magnetic configuration and the uniform (Bu), random (Br), and total (Bt) components of the field strength. We find disagreement among conclusions derived from the various data sets and argue that the pulsar data are not the best indicator for large-scale Galactic field. Near the Solar circle, we find that the azimuthal average of Bt is 4.2 μG and we adopt Bu ~2.2 and Br ~3.6 μG. Bt is higher in spiral arms, reaching ~5.9 μG. Bt is higher for smaller RGal, reaching ~8.0 μG for RGal = 4.0 kpc. The pattern of field lines is not concentric circles but spirals. The inclination of the magnetic spiral may be smaller than that of the Galaxy's spiral arms if our sample, which refers primarily to the interarm region near the Sun, is representative. However, it is not inconceivable that the local field lines follow the Galaxy's spiral pattern, as is observed in external galaxies.

We present a model that rotating primordial blackholes(PBHs) produced at the end of inflation generate the random, non-oriented primordial magnetic field. PBHs are copiously produced as the Universe completes the cosmic phase transition via bubble nucleation and tunneling processes in the extended inflation hypothesis. The PBHs produced acquire angular momentum through the mutual tidal gravitational interaction. For PBHs of mass less than 1013g, one can show that the evaporation (photon) luminosity of PBHs exceeds the Eddington limit. Thus throughout the lifetime of the rotating PBH, radiation flow from the central blackhole along the Kerr-geodesic exerts torque to ambient plasma. In the process similar to the Bierman's battery mechanism electron current reaching up to the horizon scale is induced. For PBHs of Grand Unified Theories extended inflation with the symmetry breaking temperature of TGUT ~1010 GeV, which evaporate near decoupling, we find that they generate random, non-oriented magnetic fields of ~10-11G on the last-scattering surface on (the present comoving) scales of ~O(10)Mpc.

The authors have been studying about and electro-magnetic compass with a three axis magnetic sensor in order to provide and accurate ship's magnetic heading which the compass deviations can automatically compensated in the compass itself, and the theory how to derive the poisson's coefficients from ship's magnetism measured with three axis magnetic sensor. This paper describes on the analysis of deviation derived from the measured values that obtained to measure the various magnetic fields at the compass position of the M. S. ARA, training ship of Cheju University with three axis magnetic sensor at Cheju near sea from 25th, Oct, to 13th, Nov. in 1994.