Ionospheric Response to Solar Flares of C and M Classes in January-February 2010

The ionospheric response to solar flares is analyzed for the case of the beginning of solar activity growth, when the background ionization of the ionosphere is still low enough. It is shown that the algorithms and methods of averaging variations and derivative of the total electron content (TEC) over the entire sunlit ionosphere almost always make it possible to identify the ionospheric response even to close in time weak solar flares of the C class. It is found that the response to a solar flare rather intense in the X-ray range can have almost no manifestations, which is caused by the fact that the flare does not reveal itself in the ultraviolet part of the spectrum. A map of the TEC derivative over the Japan territory with an average resolution of ~18 km is drawn for the M6.4 flare (February 7, 2010). Before the flare maximum, the TEC derivatives are synchronously increasing over the entire Japan, while after the flare maximum the values of the TEC derivative vary not so synchronously, and local differences are seen.

Yu. V. Yasyukevich, S. V. Voyeikov, I. V. Zhivetyev, and E. A. Kosogorov. Ionospheric Response to Solar Flares of C and M Classes in January-February 2010. //Cosmic Research, Vol. 51, No. 2, 2013, pp. 114-123.