  We present the properties of galaxies in filaments around the Virgo cluster
with respect to their vertical distance from the filament spine using the
NASA-Sloan Atlas catalog. The filaments are mainly composed of low-mass, blue
dwarf galaxies. We observe that the g - r color of galaxies becomes blue and
stellar mass decreases with increasing vertical filament distance. The galaxies
were divided into higher-mass (log h^2M_* > 8) and lower-mass (log h^2M_* < 8)
subsamples. We also examine the g - r color, stellar mass, Halpha equivalent
width (EW(Halpha)), near-ultraviolet (NUV) - r color, and HI fraction
distributions of the two subsamples against the vertical distance. The
lower-mass galaxies exhibit a negative g - r color gradient, whereas
higher-mass galaxies have a flat g - r color distribution. We observe a
negative EW(Halpha) gradient for higher-mass galaxies, whereas lower-mass
galaxies show no distinct EW(Halpha) variation. In contrast, the NUV - r color
distribution of higher-mass galaxies shows no strong trend, whereas the
lower-mass galaxies show a negative NUV - r color gradient. We do not witness
clear gradients of HI fraction in either the higher- or lower-mass subsamples.
We propose that the negative color and stellar mass gradients of galaxies can
be explained by mass assembly from past galaxy mergers at different vertical
filament distances. In addition, galaxy interactions might be responsible for
the contrasting features of EW(Halpha) and NUV - r color distributions between
the higher- and lower-mass subsamples. The HI fraction distributions of the two
subsamples suggest that ram-pressure stripping and gas accretion could be
ignorable processes in the Virgo filaments.
