  We observed a 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 A)= (2.5+/-0.3)x10^-16 erg/s/cm^2 and
F(3800-6000 A)=(6.4+/-0.4)x10^-17 erg/s/cm^2, which correspond to luminosities
of ~5.8x10^27 and 1.4x10^27 erg/s, for d=410 pc and E(B-V)=0.03. The
optical-FUV spectrum can be described by a power-law model, f_nu~nu^alpha, with
slope alpha=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 alpha<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 0.5x10^5 and 2.1x10^5 K, for alpha 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 spatially coincident with the known Halpha bow shock,
making PSR J2124-3358 the second pulsar (after PSR J0437-4715) with a bow shock
detected in FUV.
