Synthetic Resonance and Thomson Scattering of a Chromospheric \(\text{Ly}\alpha \) Profile Using the Bastille Day CME Model Corona: Part 1

IF 2.4 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Nelson Reginald, Lutz Rastaetter
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引用次数: 0

Abstract

In this article, Part 1, we have synthetically resonance scattered and Thomson scattered a measured solar chromospheric \(\mathrm{Ly}\alpha \) spectral radiance (CLSR) spectrum off the neutral hydrogen [\(N_{1}\)] atoms in ground state and free electrons [\(N_{\mathrm{e}}\)], respectively, contained in a 3D coronal model of the 14 July 2000 (“Bastille Day”) Coronal Mass Ejection (CME). From these two scatters, we have computed maps of the associated resonance scattered spectral radiance (RSSR) spectrum and the Thomson scattered spectral radiance (TSSR) spectrum in ultraviolet (UV) from 121.3 to 121.8 nm with a wavelength resolution of 0.1 nm, which encompasses the \(\mathrm{Ly}\alpha \) center line at 121.57 nm. We then integrated the maps over the above wavelength range and have created two 2D resonance scattered radiance (RSR) and Thomson scattered radiance (TSR) maps. As expected, the TSSR spectrum is \(\approx 1000\) times dimmer than the RSSR spectrum, which we can deem for it to contribute towards noise in the center of the RSSR spectrum. In a follow up article, Part 2, we intend to do the following with these maps. First, we will use the computed RSSR spectra along each line of sight (LOS) to derive the proton temperature [\(T_{\mathrm{p}}\)] and speed [\(V_{\mathrm{p}}\)] using the Doppler Dimming technique (DDT). Second, we will compare these derived proton parameters along each LOS with the actual values contained within the Bastille Day CME model at the plane of the sky and compute the differences. If we find they are different we will then determine where along the LOS they closely match and their distances from the plane of the sky. Finally, we will quantify an estimate of the systematic error from using DDT to measure the proton parameters at the plane of the sky, which is different from the statistical error margins reported in the literature from real RSSR experiments conducted from space-based instruments.

利用巴士底日CME模型日冕的色球\(\text{Ly}\alpha \)剖面的合成共振和汤姆森散射:第1部分
在本文的第1部分中,我们对2000年7月14日(“巴士底日”)日冕物质抛射(CME)的三维日冕模型中分别包含基态中性氢[\(N_{1}\)]原子和自由电子[\(N_{\mathrm{e}}\)]的合成共振散射和汤姆森散射测量的太阳色球\(\mathrm{Ly}\alpha \)光谱辐射(CLSR)光谱。从这两个散射体中,我们得到了相关的共振散射光谱辐射(RSSR)光谱和汤姆逊散射光谱辐射(TSSR)光谱的计算图,波长分辨率为0.1 nm,在121.57 nm处包含\(\mathrm{Ly}\alpha \)中心线。然后,我们在上述波长范围内整合了这些地图,并创建了两个二维共振散射辐射(RSR)和汤姆森散射辐射(TSR)地图。正如预期的那样,TSSR光谱比RSSR光谱暗\(\approx 1000\)倍,我们可以认为这是由于它导致了RSSR光谱中心的噪声。在后续文章第2部分中,我们打算对这些映射执行以下操作。首先,我们将利用计算得到的沿每条视距(LOS)的RSSR光谱,利用多普勒调光技术(DDT)推导出质子温度[\(T_{\mathrm{p}}\)]和速度[\(V_{\mathrm{p}}\)]。其次,我们将这些导出的质子参数与巴士底日CME模型在天空平面上的实际值进行比较,并计算差异。如果我们发现它们是不同的,我们就会确定它们在视力线上的匹配位置以及它们与天空平面的距离。最后,我们将量化使用DDT在天空平面上测量质子参数的系统误差估计,这与文献中报道的在天基仪器上进行的真实RSSR实验的统计误差范围不同。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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来源期刊
Solar Physics
Solar Physics 地学天文-天文与天体物理
CiteScore
5.10
自引率
17.90%
发文量
146
审稿时长
1 months
期刊介绍: Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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