利用新型双区孔径X射线太阳能谱仪（DAXSS）对静止太阳活动区的软X射线观测
Soft X-Ray Observations of Quiescent Solar Active Regions using Novel Dual-zone Aperture X-ray Solar Spectrometer (DAXSS)
摘要：
双区孔径X射线太阳光谱仪（DAXSS）于2018年6月18日在NASA 36.336探空火箭飞行中飞行，并在广泛的能量范围内获得了迄今为止太阳软X射线（SXR）光谱的最高分辨率。这一观测是在太阳盘面上有静止（非耀斑）小活动区的时期进行的，当时10.7厘米射电通量（F10.7）为75个太阳通量单位（1 sfu = 10-22 W/m^2/Hz）。DAXSS仪器由LASP开发的双区孔径和Amptek的商用X射线光谱仪组成，该光谱仪测量0.5-20 keV的太阳全圆盘辐照度，分辨率为20 keV。本文讨论了光谱仪的新设计和仪器表征技术。此外，使用CHIANTI光谱模型分析了从2018年探空火箭飞行中获得的太阳测量结果，以拟合太阳日冕等离子体的温度，发射测量和相对元素丰度。在静止的太阳日冕中，铁的丰度比预期的高出35%，这表明我们的光谱模型需要额外的复杂性，或者底层的原子数据库可能需要更新。今后需要对这一光谱范围进行长期系统观测。DAXSS将于2020年底在INSPIRESat-1 CubeSat上飞行，其SXR光谱数据可以通过模拟活动区域和太阳耀斑事件发展期间相对元素丰度的变化，进一步了解日冕加热的来源。
英文摘要：
The Dual-zone Aperture X-ray Solar Spectrometer (DAXSS) was flown on 2018 June18 on the NASA 36.336 sounding rocket flight and obtained the highest resolution to date for solar soft X-ray (SXR) spectra over a broad energy range. This observation was during a time with quiescent (non-flaring) small active regions on the solar disk and when the 10.7 cm radio flux (F10.7) was 75 solar flux units (1 sfu = 10-22 W/m^2/Hz). The DAXSS instrument consists of a LASP-developed dual-zone aperture and a commercial X-ray spectrometer from Amptek that measures solar full-disk irradiance from 0.5-20 keV with a resolving power of 20 near 1 keV. This paper discusses the novel design of the spectrometer and the instrument characterization techniques. Additionally,the solar measurements obtained from the 2018 sounding rocket flight are analyzed using CHIANTI spectral models to fit the temperatures, emission measures, and relative elemental abundances of the solar corona plasma. The abundance of iron was found to be 35 percent higher than expected in the quiescent sun's corona suggesting either that our spectral models require additional sophistication or that the underlying atomic database may require updates. Future long-term systematic observations of this spectral range are needed. DAXSS will fly on the INSPIRESat-1 CubeSat in late-2020, and its SXR spectral data could provide further insight into the sources of coronal heating through modeling the changes of relative elemental abundances during developments of active regions and solar flaring events.
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