Context : Pores are one of the various features forming in the photosphere by the emergence of magnetic field onto the solar surface .
They lie at the border between tiny magnetic elements and larger sunspots .
Light bridges , in such structures , are bright features separating umbral areas in two or more irregular regions .
Commonly , light bridges indicate that a the merging of magnetic regions or , conversely , the breakup of the area is underway :

Aims : We investigate the velocity structure of a solar pore ( AR10812 ) with light bridge , and of the quiet solar photosphere nearby , analyzing high spatial and spectral resolution images .

Methods : The pore area has been observed with the Interferometric BI-dimensional Spectrometer ( IBIS ) at the Dunn Solar Telescope , acquiring monochromatic images in the Ca II 854.2 nm line and in the Fe I 709.0 nm line as well as G-band and broad-band images .
We also computed the Line of Sight ( LoS ) velocity field associated to the Fe I and Fe II photospheric lines .

Results : The amplitude of the LoS velocity fluctuations , inside the pore , is smaller than that observed in the quiet granulation near the active region .
We computed the azimuthal average LoS velocity and derived its radial profile .
The whole pore is characterized by a downward velocity \simeq - 200 ~ { } m \cdot s ^ { -1 } and by an annular downflow structure with an average velocity of \simeq - 350 ~ { } m \cdot s ^ { -1 } with respect to the nearby quiet sun . The light bridge inside the pore , when observed in the broad-band channel of IBIS and in the red wing of Ca II 854.2 nm line , shows an elongated dark structure running along its axis , that we explain with a semi-analytical model .
In the highest resolution LoS velocity images the light bridge shows a profile consistent with a convective roll : a weak upflow , \sim 50 \div 100 ~ { } m \cdot s ^ { -1 } , in correspondence of the dark lane , flanked by a downflow , \sim - ( 200 \div 300 ) ~ { } m \cdot s ^ { -1 } .

Conclusions :