论文标题
1985年4月12日的Ad Leo大耀斑
Near-Ultraviolet Continuum Modeling of the 1985 April 12 Great Flare of AD Leo
论文作者
论文摘要
现在，数千人在长基线，高精度，宽带光度法中报道了白光恒星耀斑，来自开普勒，K2和苔丝等任务。这些观察结果是评估系外球星大气中生物签名的至关重要输入，以及在低质量恒星周围可居住区行星的表面紫外线辐射剂量。然而，这些评估的局限性是缺乏恒星耀斑的近粉状光谱观察结果。为了激励进一步的实证研究，我们使用辐射流动力学模拟的网格，对氢管的压力扩大的压力进行了更新的处理，以预测$λ\约1800-3300 $Å的连续性通量在上升和峰值阶段的峰值阶段和峰值阶段，这是DM3E STAR STAR STAR AD AD LEO的峰值超级浮华。这些预测基于辐射通量光谱的半经验叠加，由高升力电子束仿真组成，具有大型，低功能的截止（$ \ gtrsim 85 $ keV）和低频率电子束仿真，具有较小的低功能较小，低功能的临界值（$ \ \ \ \ \ \ \ \ \ kev）。两组分模型全面解释了氢Balmer线的宽阔，光学连续体色温，Balmer跳跃强度以及该耀斑的上升/峰值相机的远图相结合强度和形状。 We use spatially resolved analyses of solar flare data from the Interface Region Imaging Spectrograph, combined with the results of previous radiative-hydrodynamic modeling of the 2014 Mar 29 X1 solar flare (SOL20140329T17:48), to interpret the two-component electron beam model as representing the spatial superposition of bright kernels and fainter ribbons over a larger area.
White-light stellar flares are now reported by the thousands in long-baseline, high precision, broad-band photometry from missions like Kepler, K2, and TESS. These observations are crucial inputs for assessments of biosignatures in exoplanetary atmospheres and surface ultraviolet radiation dosages for habitable zone planets around low-mass stars. A limitation of these assessments, however, is the lack of near-ultraviolet spectral observations of stellar flares. To motivate further empirical investigation, we use a grid of radiative-hydrodynamic simulations with an updated treatment of the pressure broadening of hydrogen lines to predict the $λ\approx 1800-3300$ Å continuum flux during the rise and peak phases of a well-studied superflare from the dM3e star AD Leo. These predictions are based on semi-empirical superpositions of radiative flux spectra consisting of a high-flux electron beam simulation with a large, low-energy cutoff ($\gtrsim 85$ keV) and a lower-flux electron beam simulation with a smaller, low-energy cutoff ($\lesssim 40$ keV). The two-component models comprehensively explain the hydrogen Balmer line broadening, the optical continuum color temperature, the Balmer jump strength, and the far-ultraviolet continuum strength and shape in the rise/peak phase of this flare. We use spatially resolved analyses of solar flare data from the Interface Region Imaging Spectrograph, combined with the results of previous radiative-hydrodynamic modeling of the 2014 Mar 29 X1 solar flare (SOL20140329T17:48), to interpret the two-component electron beam model as representing the spatial superposition of bright kernels and fainter ribbons over a larger area.
