重力探测器B的VLBI。VI。飞马座IM的轨道和射电辐射源的位置
VLBI for Gravity Probe B. VI. The Orbit of IM Pegasi and the Location of the Source of Radio Emission
摘要：
我们提出了一个物理解释的无线电发射源的位置在飞马座IM（IM Peg，HR 8703），美国宇航局/斯坦福大学的相对论任务重力探测器B的指导星。这种发射在我们从1997年到2005年进行的35个8.4 GHz VLBI观测中都可以看到。我们发现，无线电发射的平均位置是在或接近主要的投影中心，在其半径的27%左右，确定这个活跃的恒星作为无线电发射器。射电亮度峰值的位置分散在主星的盘面上，并稍微超出，优选地沿着位置角为p. a的轴。=（-38 +- 8）度，与轨道法线（p.a.）的天空投影紧密对齐。= -49.5 +-8.6度）和初级线圈的预期自旋轴。与模拟结果的比较表明，亮度峰值为3.6发生的可能性增加（+0.4，-0.7）倍（每单位表面积）在靠近初级极区（|latitude| >= 70度）的地方比在靠近赤道（|latitude| <= 20度）的地方更容易发生，并且也发生在靠近表面的地方，其中约2/3的高度不高于初级半径的25%。
英文摘要：
We present a physical interpretation for the locations of the sources of radio emission in IM Pegasi (IM Peg, HR 8703), the guide star for the NASA/Stanford relativity mission Gravity Probe B. This emission is seen in each of our 35 epochs of 8.4-GHz VLBI observations taken from 1997 to 2005. We found that the mean position of the radio emission is at or near the projected center of the primary to within about 27% of its radius, identifying this active star as the radio emitter. The positions of the radio brightness peaks are scattered across the disk of the primary and slightly beyond, preferentially along an axis with position angle, p.a. = (-38 +- 8) deg, which is closely aligned with the sky projections of the orbit normal (p.a. = -49.5 +- 8.6 deg) and the expected spin axis of the primary. Comparison with simulations suggests that brightness peaks are 3.6 (+0.4,-0.7) times more likely to occur (per unit surface area) near the pole regions of the primary (|latitude| >= 70 deg) than near the equator (|latitude| <= 20 deg), and to also occur close to the surface with ~2/3 of them at altitudes not higher than 25% of the radius of the primary.
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