论文标题
在DME恒星的弹性阶段的光辐射的起源上。 I.气体动态模型的讨论
On the Origin of Optical Radiation during the Impulsive Phase of Flares on dMe Stars. I. Discussion of Gas Dynamic Models
论文作者
论文摘要
关于发表的批评，作者证明，使用一动不动的纯氢等离子体平面层是合理的，该平面均接近局部热力学平衡（LTE），用于分析从厚度$Δz_m= 10 \ text {km} $ s s s s stellar flar的厚度$Δz_m= 10 \ tevts {km} $的厚度的辐射特征。结果表明，与Kostyuk和Pikelner模型相反，Belova和Bychkov提出的耀斑的冲击波模型由于排除了热波（温度跳跃）和非平稳性辐射冲击之间的相互作用，因此具有不可忽视的内部缺陷。 In particular, this model (a) does not make it possible to increase the geometric thickness of a chromospheric condensation owing to divergence of the fronts of the thermal and shock waves during impulsive heating, (b) cannot provide heating of the chromospheres of red dwarfs over significant distances, and (c) predicts $\mathrm{H}_α$ line profiles in conflict with observational data. It is argued that: (a) the shock-wave model by Belova and Bychkov represents a development of the kinematic model of solar flares (Nakagawa et al.) and its application to dMe stars, specifically: a study of the radiative response of the chromosphere of a red dwarf to impulsive heating in the simplest gas dynamic statement of the problem (a thermal wave is excluded, a stationary approach is used); （b）就kostyuk和pikelner模型而言，固定冲击阵线背后的区域并不对应于随时间变化的厚度的色球凝结，而是与血浆放松到热平衡状态的区域。有人强调，Kostyuk和Pikelner模型将其分离为“热”和“冲击波”组件是根本上不可能的。
In connection with a published critique, the author justifies the use of a motionless homogeneous plane layer of pure hydrogen plasma that is near local thermodynamic equilibrium (LTE) for analyzing the characteristics of the radiation from a chromospheric condensation of thickness $Δz_m=10\text{ km}$ in a gas dynamic model of stellar flares. It is shown that the shock-wave model of flares proposed by Belova and Bychkov, as opposed to the model of Kostyuk and Pikelner, has irremovable internal defects owing to exclusion of the interaction between a thermal wave (temperature jump) and a non-stationary radiative shock. In particular, this model (a) does not make it possible to increase the geometric thickness of a chromospheric condensation owing to divergence of the fronts of the thermal and shock waves during impulsive heating, (b) cannot provide heating of the chromospheres of red dwarfs over significant distances, and (c) predicts $\mathrm{H}_α$ line profiles in conflict with observational data. It is argued that: (a) the shock-wave model by Belova and Bychkov represents a development of the kinematic model of solar flares (Nakagawa et al.) and its application to dMe stars, specifically: a study of the radiative response of the chromosphere of a red dwarf to impulsive heating in the simplest gas dynamic statement of the problem (a thermal wave is excluded, a stationary approach is used); (b) in terms of the Kostyuk and Pikelner model, the regions behind the stationary shock fronts do not correspond to a chromospheric condensation with time-varying thickness but to zones in which the plasma relaxes to a state of thermal equilibrium. It is emphasized that the separation of the Kostyuk and Pikelner model into "thermal" and "shock-wave" components is fundamentally impossible.
