论文标题
过渡区域的基础在哪里？来自Trace，SDO，Iris和Alma观察的证据
Where is the base of the Transition Region? Evidence from TRACE, SDO, IRIS and ALMA observations
论文作者
论文摘要
经典的太阳能模型将彩色 - 欧罗纳过渡区域（CCTR）放在$ \ sim2 $ mm上方，高于$τ_{5000} = 1 $级别，而RMHD模型将其处于较大的高度。观察性验证很少。我们很少审查和讨论来自各种工具和光谱中的1700次乘以17 00的最新结果。在EUV频段中的乐队和吸收是由于H and He I的光学化，因此在最短的AIA波长中，并考虑到光电肢体是$ \ sim0.34 $ mm，高于$τ_{5000}染色体吸收，我们推断出$ 3.0 \ pm 0.5 $ mm，高于Avrett＆loeser模型的另一个指标。 1700 a），$ 0.31 \ pm0.09 $毫米（在1600 a）和$ 3.31 \ pm 0.18 $ mm（304 a），用于太阳能磁盘的中心，先前报告的太阳能周期变化。 2832肢体，AIA/SDO图像的肢体高度为$ 1.4 \ pm 0.2 $ mm（1600 a）和$ 5.7 \ pm 0.2 $ mm（304 a）。我们得出的结论是，我们得出的结论是，平均染色器的延伸高于均质模型的预测，但在RMHD模型的范围内。
Classic solar models put the Chromosphere-Corona Transition Region (CCTR} at $\sim2$Mm above the $τ_{5000} = 1$ level, whereas rMHD models place it in a wider range of heights. Observational verification is scarce. We review and discuss recent results from various instruments and spectral domains. In SDO and TRACE images spicules appear in emission in the 1600, 1700 and 304 A bands and in absorption in the EUV bands; the latter is due to photo-ionization of H and He I. At the shortest available AIA wavelength and taking into account that the photospheric limb is $\sim0.34$Mm above the $τ_{5000}=1$ level, we found that CCTR emission starts at $\sim3.7$Mm; extrapolating to $λ=0$, where there is no chromospheric absorption, we deduced a height of $3.0\pm 0.5$Mm, above the value of 2.14Mm of the Avrett & Loeser model. Another indicator of the extent of the chromosphere is the height of the network structures. Height differences produce a limbward shift of features with respect to their counterparts in magnetograms. Using this approach, we measured heights of $0.14\pm0.04$Mm (at 1700 A), $0.31\pm0.09$Mm (at 1600 A) and $3.31\pm 0.18$Mm (at 304 A) for the center of the solar disk. A previously reported possible solar cycle variation is not confirmed. A third indicator is the position of the limb in the UV, where IRIS observations of the Mg II triplet lines show that they extend up to $\sim2.1$Mm above the 2832 A limb, while AIA/SDO images give a limb height of $1.4 \pm 0.2$Mm (1600 A) and $5.7\pm 0.2$Mm (304 A). Finally, ALMA mm-$λ$ full-disk images provide useful diagnostics, though not very accurate; values of $2.4\pm0.7$Mm at 1.26mm and $4.2\pm2.5$Mm at 3mm were obtained. Putting everything together, we conclude that the average chromosphere extends higher than homogeneous models predict, but within the range of rMHD models.
