Measuring the Magnetic Fields of Our Galaxy
I report our efforts on measuring the magnetic fields of our Galaxy. Through observing Faraday rotation (i.e. the rotation measure, RM) of a large sample of pul sars, we can determine the large-scale structure of magnetic fields in the Galactic disk. Magnetic fields are found to reverse their directions from arm to arm. The distribution of magnetic fields measured from OH masers of a sample of the star formation or HII regions shows field reversals in large scale. Together with pulsar dispersion measures (DMs), we obtained the strength of maagnetic fields and its variation with the Galac tocentric radius. Considering RMs are the integration of magnetic fields with electron density over the path from the pulsar to the Sun in the line of sight, we derived the different fiuctuations of magnetic fields on various length-scales, which is the spa tial magnetic energy spectrum in the interstellar medium. From the antisymmetric RM sky distribution, we identified the azimuthal magnetic fields in the Galactic halo, which reverse their directions below and above the Galactic plane.
ISM magnetic fields pulsars
J. L. Han
Natianal Astronomical Observatories, Chinese Academy of Sciences, Jia-20 DaTun Road, Chaoyang District, Beijing 100012, China
国际会议
The 10th Asian-Pacific Regional International Astronomical Union Meeting(第十届亚洲及太平洋地区天文学大会 APRIM)
昆明
英文
116-120
2008-08-03（万方平台首次上网日期，不代表论文的发表时间）