  Active galactic nuclei (AGNs) are occasionally seen in pairs, suggesting that
tidal encounters are responsible for the accretion of material by both central
supermassive black holes (BHs). In Paper I of this series, we selected a sample
of AGN pairs with projected separations r_p < 100 kpc and velocity offsets <
600 km/s from the SDSS DR7 and quantified their frequency. In this paper, we
address the BH accretion and recent star formation properties in their host
galaxies. AGN pairs experience stronger BH accretion, as measured by their [O
III]5007 luminosities (corrected for contribution from star formation) and
Eddington ratios, than do control samples of single AGNs matched in redshift
and host stellar mass. Their host galaxies have stronger post-starburst
activity and younger mean stellar ages, as indicated by stronger H-delta
absorption and smaller 4000 A break in their spectra. The BH accretion and
recent star formation in the host galaxies both increase with decreasing
projected separation in AGN pairs, for r_p ~< 10-30 kpc. The intensity of BH
accretion, the post-starburst strength, and the mean stellar ages are
correlated between the two AGNs in a pair. The luminosities and Eddington
ratios of AGN pairs are correlated with recent star formation in their host
galaxies, with a scaling relation consistent with that observed in single AGNs.
Our results suggest that galaxy tidal interactions enhance both BH accretion
and star formation in AGN pairs, even though the majority of low redshift AGNs
is not coincident with on-going interactions.
