Magnetically coupled atmosphere and magnetic field reconnection forced by passing tadpole wave (UT times (a) are related to individual rows of plots). Magnetic field perturbations are marked by arrows (except 17:20 UT, (c)). The slit position X = −62″ is displayed by vertical red lines. (a)–(b): The blue background represents the B_z HMI magnetograms. The best-fit magnetic field lines (orange curves) were computed for AIA 1600Å with the VCA-NLFFF code: Footpoints are in a 150 × 150 grid, field strength of |B_z| > 180 G. The field lines were obtained from line-of-sight angles ((a)) and the 90 deg rotated to north angles ((b)). (c)–(e): Evolution of magnetic field perturbation in SDO/HMI magnetograms. Dark mottles (orange arrows, (c)) show that places of magnetic field strength decrease. The magnetic field strength distributions ((d)) exhibit a hill shape. They are related to the area size (white rectangle, (c)). The magnetic field strength profiles ((e)) are at selected positions (yellow horizontal lines, (c)–(d)). The SDO/AIA 1700Å waveguide width is marked by vertical cyan lines ((d)–(e)).