On the generation of modified low-frequency Farley-Buneman waves in the solar atmosphere

The possibility of the excitation of Farley-Buneman turbulence in the solar atmosphere is examined. It is found that the conditions for the generation of the modified Farley-Buneman instability can be realized in the chromosp here of the Sun 1000 km above the photosphere. While usual Farley-Buneman w aves studied in relation to the Earth's ionosphere are almost electrostatic , the modified Farley-Buneman waves in the solar atmosphere are electromagn etic ones. This means, that not only the potential electric field caused by the charge distribution, but also the perturbations of the magnetic field and the circularly-polarized electric field are essential. Although the phy sical pictures of usual and modified Farley-Buneman waves are different, th eir dispersion equations are almost the same. However, the increment of the modified Farley-Buneman waves is varied by additional electromagnetic effe cts. It is demonstrated that electromagnetic effects hinder a Farley-Buneman ins tability in occurring while xi < 1, where 5 is the square of the ratio of i on plasma frequency times ion-neutral frequency to ion-cyclotron frequency times wave number times speed of light in vacuum. Under the condition xi > 1, no Farley-Buneman disturbances appear at all. In weakly-ionized solar re gions, the modified (xi < 1) and also the usual (xi << I) Farley-Buneman tu rbulence could make "electromagnetic" contributions to the process of energ y dissipation of nonstationary streams of neutral gases. Besides, they may modify the low-frequency acoustic noise. It seems that the modified Farley-Buneman turbulence contributes to the spo radic radiation of the Sun. It is possible, that such an effect takes not o nly place in the chromosphere of the Sun, but also in the atmospheres of ot her stars.