We observed the nearby millisecond pulsar J2124-3358 with the Hubble Space Telescope in broad far-UV (FUV) and optical filters. The pulsar is detected in both bands with fluxes F(1250-2000 Å) = (2.5 ± 0.3) × 10-16 erg s-1 cm-2 and F(3800-6000 Å) = (6.4 ± 0.4) × 10-17 erg s-1 cm-2, which corresponds to luminosities of ≈5.8 × 1027 and 1.4 × 1027 erg s-1, for d = 410 pc and E(B – V) = 0.03. The optical-FUV spectrum can be described by a power-law model, fν ~ ν α , with slope α = 0.18-0.48 for a conservative range of color excess, E(B – V) = 0.01-0.08. Since a spectral flux rising with frequency is unusual for pulsar magnetospheric emission in this frequency range, it is possible that the spectrum is predominantly magnetospheric (power law with α < 0) in the optical, while it is dominated by thermal emission from the neutron star surface in the FUV. For a neutron star radius of 12 km, the surface temperature would be between 0.5 × 105 and 2.1 × 105 K for α ranging from -1 to 0, E(B – V) = 0.01-0.08, and d = 340-500 pc. In addition to the pulsar, the FUV images reveal extended emission that is spatially coincident with the known Hα bow shock, making PSR J2124-3358 the second pulsar (after PSR J0437-4715) with a bow shock detected in the FUV. Read more here.