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我在2005年的《强子杂志》上发表的《单向光速的测量》一文预测的GP-B由于光速变化引起的误差>=0.05角秒，与目前确定的GP-B误差0.05-0.1角秒的误差惊人地吻合。下面是我在《强子杂志》上发表的论文的英文原来和中文内容：
The distance of HR8703 (IM Pegasi) to the earth is 0.3 billion lightyears, its proper motion across the sky measured with VLBIA is 35 miliarcseconds per year. If the speed of starlight depends on the motion of GP-B, the maximum aberration of HR8703 will be 5+_0.05 arcseconds(as). The difference is 50 mas. It's 6500 times of the frame dragging effect given by the general relativity which is 0.0076 mas/orbit (42 mas/year), and 42 times of the geodetic effect which is 1.2 mas/orbit (6600mas/year). [2] The proper motion of HR8703 (0.007mas/orbit) can also be neglected comparative to the aberration difference per orbit. But for a year period, the aberration difference is about 200mas, much less than the geodetic effect, even if the speed of starlight depends on the motion of GP-B, the GP-B experiment will still be success to detect the geodetic effect but will fail to detect the much weaker frame dragging effect. GP-B用于定位的类星体HR8703（IM Pegasi）距离地球3亿光年，它的自行用VBLA技术确定为35毫角秒/年。如果光速与观察者的运动速度有关，GP-B观测HR8703的光行差偏离值由(24.4)式计算约为50毫角秒/轨道周期。这种光行差的偏离比广义相对论预言的参考系拖拽效应0.0076毫角秒/每轨道周期（42毫角秒/年）大约6500倍，也比测地线效应1.2毫角秒/轨道周期（6600毫秒/年，18毫秒/日）大42倍。与GP-B轨道上的光行差偏离相比，HR8703的自行也可以忽略不计。不过，在一年的地球轨道周期中，HR8703的光行差偏离仅为200毫角秒/年，即使光速与GP-B的运动速度有关，GP-B仍然能测量到测地线效应，但将无法区分参考系拖拽效应。 ※※※※※※ 黄氏时空由光频多普勒红移定义可变时间单位秒t'=tsquart[(C-V)/(C+V)].时间秒的变化导致了可变光速C'=Csquart[(C-V)/(C+V)].光速的变化导致了可变距离单位米l'=lsquart[(C-V)/(C+V)].黄氏自旋衰变相互作用模型:引力=动量变化率，电磁力=角动量变化率.超光速C=2ZM/r |