Model of THE sunspotless flare
The model CSHKP well enough describes a finishing phase of solar flare - a phase dispersing flare ribbons, however it is not applicable to an initial phase of the flare, including to occurrence of primary flare ribbons over an inversion line of the photospheric magnetic field. Data of the analysis of large statistical researches of solar flares for the last hundred years are cited in the paper. We used observational data of the solar chromosphere in the H<sub>α</sub> lines taken at the Baikal Astrophysical Observatory (BAO) and magnetic field data obtained at the Kitt Peak Observatory (USA). We present a model of the sunspotless solar flare on the basis of the acquired data and analysis of theoretical models of the solar flares available in the literature, including model CSHKP. The model allows us to explain the main stages of development of the flare and observed “phenomenon” - extended bright chromospheric “streamer” over the polarity reversal line section of the longitudinal magnetic field.