提高 SDO/EVE MEGS-A 耀斑观测的光谱分辨率和波长尺度

IF 2.7 3区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Solar Physics Pub Date : 2024-10-28 DOI:10.1007/s11207-024-02394-9

Gabriela Gonzalez, Phillip Chamberlin, Vicki Herde

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引用次数: 0

摘要

极紫外可变性实验（EVE）是太阳动力学观测台（SDO）上的三台仪器之一。本文的重点是利用 EVE 上测量 5 - 37 nm 波长的多 EUV 光栅摄谱仪（MEGS-A）的 "A "通道来提高太阳耀斑期间的波长刻度精度和光谱分辨率。EVE 的最小处理（0B 级）数据产品用于创建更新的波长标度，通过该分析表明，与 EVE 2 级数据相比，其光谱测量更加精确。2011年2月15日发生的X2.2级耀斑SOL2011-02-15T0156被用来推导像素到波长的尺度。发现发射线宽的改进范围为 5.21% 至 11.35%。今后，这些测量结果可用于改进太阳耀斑期间不同温度加速等离子体的多普勒速度计算。

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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Improving the Spectral Resolution and Wavelength Scale of SDO/EVE MEGS-A Flare Observations

The Extreme ultraviolet Variability Experiment (EVE) is one of three instruments onboard the Solar Dynamics Observatory (SDO). This paper focuses on using the “A” channel on the Multiple EUV Grating Spectrographs (MEGS-A) on EVE, which measures wavelengths of 5 – 37 nm, to improve the wavelength scale accuracy and spectral resolution during solar flares. EVE’s least processed (Level 0B) data product is used to create updated wavelength scales that are shown, through this analysis, to make more precise spectral measurements compared to EVE Level 2 data. An X2.2 class flare that occurred on 15 February 2011, SOL2011-02-15T0156, was used to derive the pixel-to-wavelength scales. An improvement range of 5.21% to 11.35% was found in the emission line widths. In the future, these measurements can be used for improved Doppler velocity calculations of the accelerated plasma of various temperatures during solar flares.

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来源期刊

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.