There has been ubiquitous observations of wave-like motions in the solar atmosphere for decades .
Recent improvements to space- and ground-based observatories has allowed the focus to shift to smaller magnetic structures on the solar surface .
In this paper , high-resolution ground-based data taken using the Swedish 1-m Solar Telescope ( SST ) is combined with co-spatial and co-temporal data from the Atmospheric Imaging Assembly ( AIA ) on-board the Solar Dynamics Observatory ( SDO ) satellite to analyse Running Penumbral Waves ( RPWs ) .
RPWs have always thought to be radial wave propagation that occur within sunspots .
Recent research has suggested that they are in fact upwardly propagating field-aligned waves ( UPWs ) .
Here , RPWs within a solar pore are observed for the first time and are interpreted as UPWs due to the lack of a penumbra that is required to support RPWs .
These UPWs are also observed co-spatially and co-temporally within several SDO/AIA elemental lines that sample the Transition Region ( TR ) and low corona .
The observed UPWs are travelling at a horizontal velocity of around 17 \pm 0.5 km s ^ { -1 } and a minimum vertical velocity of 42 \pm 21 km s ^ { -1 } .
The estimated energy of the waves is around 150 W m ^ { -2 } , which is on the lower bounds required to heat the quiet-Sun corona .
This is a new yet unconsidered source of wave energy within the solar chromosphere and low corona .