Spectroscopic Detection of the 3.934 Micron Line of Si IX in the Solar Corona
Spectroscopic Detection of the 3.934 Micron Line of Si IX in the Solar Corona
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日冕中 3.934 微米 Si IX 谱线的光谱检测
DOI：
10.1086/343730
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发表时间：
2002
期刊：
影响因子：
--
通讯作者：
M. Penn
中科院分区：
文献类型：
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作者：
Philip G. Judge;Steven Tomczyk;W. Livingston;Christoph U. Keller;M. Penn
我们报道了利用位于基特峰的麦克马斯-皮尔斯望远镜对Si IX的2s 22 p2 3 P1 → 0谱线的探测。2002年5月13日至17日期间，在非理想天空条件下，使用13.5米垂直摄谱仪和InSb单二极管探测器对太阳盘和边缘以上不同高度进行了观测。我们报告了一个新的休息波长的线，并讨论其潜在的用途作为一个诊断的日冕磁场使用地面望远镜。我们的观测给出λrest = 3.93434 ± 0.00007 μm，与早期不太准确的值一致，但它将线的蓝翼置于强大地N2 O线之下。在观测到的活动区域，谱线的强度与早期对安静太阳的预测相当或更大。
We report the detection of the 2s22p2 3P1 → 0 line of Si IX using the McMath-Pierce telescope on Kitt Peak. Observations were made of the solar disk and at various heights above the limb between 2002 May 13 and 17, under nonideal sky conditions, using the 13.5 m vertical spectrograph and an InSb single-diode detector. We report a new rest wavelength for the line and discuss its potential use as a diagnostic of coronal magnetic fields using ground-based telescopes. Our observations give λrest = 3.93434 ± 0.00007 μm, consistent with earlier less accurate values, but it places the blue wing of the line under a strong telluric N2O line. In the active regions observed, the line's intensity is comparable to or larger than predicted in earlier work for the quiet Sun.