Extreme Ultraviolet ExplorerObservations of PSR B0656+14

The pulsar PSR B0656+14 has been observed at γ-ray, X-ray, EUV, and optical energies. These data are consistent with emission originating from a thermal stellar surface augmented by a hot, thermal "polar-cap" and an additional magnetospheric component. We have combined archival Extreme Ultraviolet Explorer ( EUVE ) and ROSAT data, together with recent analyses of optical photometry, to char acterize the surface thermal emission from PSR B0656+14. Because of differences in the EUVE and ROSAT flux for E < 0.18 keV, our combined-data models require a softer surface thermal component at closer distance with a larger intervening column, compared to models using only X-ray data. For a 0.1-2.0 keV source consisting of a dominant soft thermal blackbody that is augmented by both a smaller hot blackbody and a power-law optical component, we derive the source properties at 90% confidence to be T soft = (4.7-5.5) × 10 5 K, an absorbing column density of N H = (1.45-1.65) × 10 20 cm -2 , a distance of d / R 10 = 135-190 pc, and T hot = (1.13-1.18) × 10 6 K.