Sympathetic solar flare: characteristics and homogeneities

We studied 2204 sympathetic flares detected by the GOES during 1975–2017. Sympathetic flares have nearby, or homogeneous, GOES classes. The secondary solar flare is just a mirror image of the primary solar flare of the sympathetic flare. It has two types: 1) Twins: This type represents most of them (∼78.6%). 2) Non-twins: It is an associated heterogeneous pair of solar flares. A negative relationship between the interval between the start times of primary and secondary flares was found with the duration of the primary flare with the solar cycle progress. Also, the stronger the solar cycle, the lower the maximum value of the timing ratio at the quiet Sun’s epoch, while the timing ratio’s value reaches a higher value during the weaker cycles. A positive relationship between the angular distance between pairs of sympathetic flares and SSN has been found. During the epoch of the active sun, the distance is as far as possible, while that distance becomes shorter during the epoch of the quiet sun. Sympathetic flares are equatorial in alignment. The higher inclination (slope of about −20° each cycle) is associated with the X-Class of the primary flare. It is more than this non-association. We found that the time series of inclinations is given a “Wings diagram” diagram.