太阳磁场强度观测的解释
Interpretation of Solar Magnetic Field Strength Observations
摘要：
这项研究的基础上纵向塞曼效应磁图和谱线扫描调查太阳表面磁场的依赖关系上的谱线和线的采样方式，以估计磁通量出现以上的太阳大气层和穿透日冕的磁图的山。威尔逊150英尺塔天气计划（MWO）。我们已经比较了天气程序\lambda 5250号Fe I谱线和\lambda 5233号Fe I谱线，因为后者的谱线有一个宽的形状，在其机翼的大部分上几乎是线性的。本研究使用$\lambda5233$线上的五对采样点。我们建议采用线平分线法确定的字段与采样点尽可能接近线核心的最佳估计的出射光球通量。线剖面测量值与\lambda 5250和\lambda 5233同时测量的场的互相关的组合产生了比例因子1/δ的公式，该公式乘以MWO天气磁场。新的校准表明，SOHO航天器上的MDI系统测量的磁场等于中心到边缘位置30度处真实值的0.619+/-0.018倍。Berger和Lites（2003）发现这个系数是0.64+/-0.013，基于与高级斯托克斯偏振计的比较。
英文摘要：
This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled in order to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program \lambda5250Åline of Fe I to the line of Fe I at \lambda5233Åsince this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the $\lambda5233$Åline. We recommend adoption of the field determined with a line bisector method with a sampling point as close as possible to the line core as the best estimate of the emergent photospheric flux. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with \lambda5250Åand \lambda5233Åyields a formula for the scale factor 1/δthat multiplies the MWO synoptic magnetic fields. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619+/-0.018 times the true value at a center-to-limb position 30 deg. Berger and Lites (2003) found this factor to be 0.64+/-0.013 based on a comparison the the Advanced Stokes Polarimeter.
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