研究目的
Investigating the first detection of solar flare emission at mid-ultraviolet wavelengths around 2000 ? and its consistency with hydrogen Balmer continuum emission.
研究成果
The observations confirm the non-thermal temporal behavior of emission in LYRA channels 1 and 2, consistent with hydrogen Balmer continuum emission from an optically thin chromospheric slab. This strengthens the interpretation of broadband flare emission as hydrogen recombination continua originating in the chromosphere.
研究不足
LYRA integrates the solar flux over the full solar disk and over wavelengths, which does not allow for a clear separation of different continua and spectral lines in the wavelength range of interest. Spatially and spectrally resolved observations are necessary for a better understanding.
1：Experimental Design and Method Selection:
The study utilized the Large-Yield RAdiometer (LYRA) on board the PRoject for OnBoard Autonomy 2 mission to observe solar flare emission at mid-ultraviolet wavelengths.
2：Sample Selection and Data Sources:
The X
3：3 flare on 2017 September 6 was observed. Data from LYRA channels 1 and 2, GOES-15, and SDO/HMI were used. List of Experimental Equipment and Materials:
LYRA instrument with four spectral channels, GOES-15, SDO/HMI.
4：Experimental Procedures and Operational Workflow:
High-cadence solar irradiance measurements were taken during the flare. The emission was analyzed to separate line emission from continuum emission.
5：Data Analysis Methods:
The spectral radiance increase produced by the flare was modeled assuming an optically thin chromospheric slab heated up to 10,000 K.
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