太阳自转立体观测与磁场外推的微波源三维结构
3D Structure of Microwave Sources from Solar Rotation Stereoscopy vs Magnetic Extrapolations
摘要：
我们使用旋转体视法来估计相对于光球的稳态太阳特征的高度，基于其在几天的观测中记录的图像平面中的明显运动。体视算法适于与一维或二维数据（即，来自图像或来自记录源沿任意轴的投影位置的观察）一起工作。利用西伯利亚太阳射电望远镜5.7GHz附近、野边山射电日像仪17 GHz、以及从RATAN-600仪器在跨越5.98- 15.95GHz频率范围的多个频率下的一维扫描。陀螺共振发射机制，这是敏感的日冕磁场强度，被施加到转换的估计无线电源高度在不同的频率，h（f），信息的磁场与高度B（h），并比较结果与磁场外推来自光球磁场观测获得的Hinode和MDI。我们发现，回旋共振辐射来自于超出第三层回旋层位置的高度，与磁场外推法无关，并讨论了这一发现对日冕磁象学和日冕等离子体物理的意义。
英文摘要：
We use rotation stereoscopy to estimate the height of a steady-state solar feature relative to the photosphere, based on its apparent motion in the image plane recorded over several days of observation. The stereoscopy algorithm is adapted to work with either one- or two-dimensional data (i.e. from images or from observations that record the projected position of the source along an arbitrary axis). The accuracy of the algorithm is tested on simulated data, and then the algorithm is used to estimate the coronal radio source heights associated with the active region NOAA 10956, based on multifrequency imaging data over 7 days from the Siberian Solar Radio Telescope near 5.7 GHz, the Nobeyama Radio Heliograph at 17 GHz, as well as one-dimensional scans at multiple frequencies spanning the 5.98--15.95 GHz frequency range from the RATAN-600 instrument. The gyroresonance emission mechanism, which is sensitive to the coronal magnetic field strength, is applied to convert the estimated radio source heights at various frequencies, h(f), to information about magnetic field vs. height B(h), and the results are compared to a magnetic field extrapolation derived from photospheric magnetic field observations obtained by Hinode and MDI. We found that the gyroresonant emission comes from the heights exceeding location of the third gyrolayer irrespectively on the magnetic extrapolation method; implications of this finding for the coronal magnetography and coronal plasma physics are discussed.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
