Self Consistent Models of Solar Flare Chromospheres

太阳耀斑色球层的自洽模型

• 批准号: 9022385
• 负责人: Suzanne Hawley
• 金额: $ 2.85万
• 依托单位: Carnegie Institution of Washington
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1991
• 资助国家: 美国
• 起止时间: 1991-01-15 至 1992-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9022385&HistoricalAwards=false
• 关键词: Self; Consistent; Models; Solar; Flare

It is planned to provide tools for interpretation of combined hard X-ray, soft X-ray, and optical observations of solar flares by developing self-consistent models of energy transport in flares. The MAX '91 program is providing unprecedented multiwavelength observations of flares during the current solar maximum. In particular, it is planned to compute a grid of physically self-consistent atmospheric models which are in energy balance, including energy transport by nonthermal particles, thermal conduction, and all important radiation processes (X-ray, UV, optical). It is neither necessary or desireable to carry out a fully time-dependent model. It is more useful, for interpretation of the observations to consider two simpler limiting cases: the hydrostatic limit, valid on timescales typically tens of seconds or longer, and the impulsive limit, where the mass is frozen into its preflare distribution. To determine the heating and cooling of the optically thick chromosphere, a rigorous non-LTE treatment of the radiative transfer and statistical equilibrium in all important atomic lines will be employed. These models should provide an important step toward using integrated multi-wavelength observations to discriminate between thermal and nonthermal processes in solar flare chromospheres.

计划提供工具，用于解释 结合硬X射线、软X射线和光学观察， 太阳耀斑通过发展自洽模型的能量 用照明弹运输。 MAX '91计划提供了 在2004年对耀斑进行了前所未有的多波长观测， 太阳活动最大期 特别是，计划计算一个 物理上自洽的大气模型网格， 在能量平衡中，包括通过非热传递的能量 粒子、热传导和所有重要的辐射 工艺（X射线、UV、光学）。 这既不是必要的， 期望执行完全时间依赖的模型。 更 有用的，为解释的意见，考虑两个 更简单的极限情况：流体静力极限，有效于 时间尺度通常是几十秒或更长，而冲动的 极限，质量冻结在耀斑前的分布中。 为了确定光学厚度的加热和冷却， 色球，一个严格的非LTE处理的辐射 所有重要原子的转移和统计平衡 线将被使用。 这些模型应该提供一个重要的 逐步采用综合多波长观测， 区分太阳的热过程和非热过程 耀斑色球