The flow of energy through the solar atmosphere and the heating of the Sun ’ s outer regions are still not understood .
Here , we report the detection of oscillatory phenomena associated with a large bright-point group that is 430,000 square kilometers in area and located near the solar disk center .
Wavelet analysis reveals full-width half-maximum oscillations with periodicities ranging from 126 to 700 seconds originating above the bright point and significance levels exceeding 99 % .
These oscillations , 2.6 kilometers per second in amplitude , are coupled with chromospheric line-of-sight Doppler velocities with an average blue shift of 23 kilometers per second .
A lack of cospatial intensity oscillations and transversal displacements rules out the presence of magneto-acoustic wave modes .
The oscillations are a signature of Alfvén waves produced by a torsional twist of \pm 22 degrees .
A phase shift of 180 degrees across the diameter of the bright point suggests that these torsional Alfvén oscillations are induced globally throughout the entire brightening .
The energy flux associated with this wave mode is sufficient to heat the solar corona .