Pub Date : 2004-01-01DOI: 10.1163/9789004490444_008
K. Schnorr, V. Mäckel, N. S. Oreshkina, S. Augustin, F. Brunner, Z. Harman, C. Keitel, J. Ullrich, José R. Crespo López-Urrutia
The green coronal line at 530.3 nm was first observed during the total solar eclipse of 1869. Once identified as emitted by Fe xiv, it became clear that this highly charged ion was typical for the range of temperatures found in coronal plasmas, stellar winds, outflows, and accretion disks. Under these conditions of high ionization, the strongest transitions are in the X-ray, extreme ultraviolet, and ultraviolet wavelength range, with only few optical lines. For these so-called forbidden coronal lines, only scarce laboratory data is available, and even advanced atomic theory codes cannot yet predict their wavelengths with the accuracy required for precise absolute velocity determinations of such plasmas. Here we report on a study of the Fe xiv line, a key coronal transition of a highly charged ion, using laser spectroscopy in an electron beam ion trap, obtaining the first laboratory measurement of 530.2801(4) nm for its rest wavelength. The result enables the determination of absolute line shifts and line broadenings in hot turbulent plasmas and astrophysical environments, with an error bar of only 0.24 km s−1. In addition, our measurement provides a much-needed benchmark for advanced atomic structure calculations, which are fundamental for astronomy.
绿色的日冕线在530.3 nm处首次被观测到是在1869年的日全食期间。一旦确定是由Fe xiv发射的，很明显，这种高电荷离子在日冕等离子体、恒星风、流出物和吸积盘的温度范围内是典型的。在这些高电离条件下，最强的跃迁发生在x射线、极紫外和紫外波长范围内，只有很少的光谱线。对于这些所谓的禁止日冕线，只有很少的实验室数据可用，即使是先进的原子理论代码也无法准确地预测它们的波长，以精确确定这种等离子体的绝对速度。本文报道了在电子束离子阱中使用激光光谱对高电荷离子的关键日冕跃迁Fe xiv线的研究，获得了其剩余波长530.2801(4)nm的首次实验室测量结果。该结果能够在热湍流等离子体和天体物理环境中确定绝对线移和线宽，误差仅为0.24 km s−1。此外，我们的测量为高级原子结构计算提供了急需的基准，这是天文学的基础。
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