Velocities in solar pores

We use high spatial and spectral resolution filtergrams to examine the thre e-dimensional morphology and velocity fields associated with solar pores in a region of newly emerged magnetic flux. The observed amplitude of the hor izontal surface velocities decreases near the pores, Most of the pores exhi bit a downflow in the surrounding region. Time-averaged line-of-sight veloc ities in and near the pores increased with the strength of the associated m agnetic field. The LOS velocities art: such that the maximum downflow is no t centered about the continuum intensity and sometimes traces an annulus ri nglike structure around the pore. From a time sequence of continuum images, it appears that some pores shed flux at the photospheric level. "Cork movi es" of the surface velocities show that the "corks" are advected toward wea k downflows near the pore locations and that the loci of the advected corks trace boundaries that resemble mesogranular and supergranular flows. We an alyze the vertical velocity structure in pores and show that the downflow d ecreases exponentially with height, with a scale height that is a factor of 2 smaller than the photospheric scale height for granules. The line-of-sig ht flow associated with the pores appears to expand with height. Our observ ations are compared with previous measurements of Bows in and around pores that were based on both spectrograms and filtergrams, Finally, we provide a phenomenological description for pores.