The work presented in this thesis is composed of two complementary fields in solar physics. The first section is devoted to current issues in instrument hardware, in particular the Ultraviolet (UV) channel of the Transition Region and Coronal Explorer (TRACE) instrument. The chapter as presented is reproduced from Handy et al. (1998). The TRACE instrument carries UV optics to image solar plasmas in the Lya {dollar}lambda{dollar} 1216 A emission line, the C IV {dollar}lambda{dollar} 1550 A resonance line doublet, the UV continuum at 1600 A and a "white light" image centered at {dollar}approx{dollar}5000 A. The C IV lines are particularly difficult to image properly as they are superimposed on a background UV continuum that increases six orders of magnitude over the wavelength range 1300-2100 A. Chapter 2 considers the problem of isolating the C IV resonance lines from the UV continuum, discusses the optics used to achieve this goal, presents a formalism for data analysis and finally shows a sample dataset from post-launch observations.; Chapter 3 considers observations from a high time-cadence joint observing campaign with the Extreme-ultraviolet Imaging Telescope (EIT, Delaboudiniere et al. 1995) and the Michelsen Doppler Imager (MDI, Scherrer et al. 1995) on the Solar and Heliospheric Observatory (SOHO, Domingo, Fleck, & Poland 1995), 10-14 August 1997. This coordinated observation makes it possible to observe the response of the (1 MK) solar corona to the evolution of the photospheric magnetic field. Qualitative observations show that coronal loops evolve continually on a discontinuous basis: small emerging loops spread, the magnetic footpoints coalesce (or cancel) with other flux concentrations, then the coronal loops reconnect to larger concentrations at a greater range of distances. We find that the quiet solar corona has a typical evolution time scale of nominally 15 hours, in very good agreement with the observations of Schrijver et al. (1997) who find that photospheric magnetic flux concentrations have a lifetime of less than 40 hours. Hence, pairs of flux concentrations must evolve on a timescale of less than 20 hours. We also evaluate two theories of coronal heating via magnetic reconnection and attempt to reconcile our observations against these theoretical predictions.
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机译：本文提出的工作由太阳物理学的两个互补领域组成。第一部分专门介绍仪器硬件中的当前问题，尤其是过渡区和日冕总管（TRACE）仪器的紫外线（UV）通道。所提供的章节摘自Handy等人。 （1998）。 TRACE仪器使用紫外线光学器件对Lya {12} A发射线，C IV {15} 1550 A共振线的双态峰，1600 A的UV连续谱和“ “白光”图像的居中位置约为{dollar}大约{dollar} 5000A。CIV线特别难于正确成像，因为它们叠加在背景UV连续体上，该连续体在1300-2100 A波长范围内增加了六个数量级。第2章考虑了将C IV共振线与UV连续体隔离的问题，讨论了用于实现此目标的光学器件，提出了进行数据分析的形式，最后显示了发射后观测值的样本数据集。第3章考虑了由极紫外成像望远镜（EIT，Delaboudiniere et al。1995）和米歇尔森多普勒成像仪（MDI，Scherrer et al。1995）在太阳和日球天文台（ SOHO，Domingo，Fleck和波兰，1995年），1997年8月10日至14日。这种协调一致的观察使观察（1 MK）太阳日冕对光球磁场演变的响应成为可能。定性观察表明，日冕环在不连续的基础上持续发展：小的新出现的环散开，磁脚点与其他通量浓度合并（或抵消），然后日冕环在更大的距离范围内重新连接到更大的浓度。我们发现，安静的日冕有一个典型的演化时间尺度，名义上为15小时，与Schrijver等人的观察非常吻合。 （1997年）发现光球磁通量浓度的寿命少于40小时。因此，成对的助焊剂浓度必须在少于20小时的时间范围内演变。我们还评估了通过磁重联进行日冕加热的两种理论，并试图使我们的观察结果与这些理论预测相一致。
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