  We study the size of BLRs of low luminosity Active Galactic Nuclei, also
called 'dwarf AGN', defined as having ($L_{H\alpha}\le10^{41}{\rm erg\cdot
s^{-1}}$)). We more than double the sample size analyzed previously (Wang &
Zhang 2003, hereafter Paper I). In this study we first confirm our previous
result that the sizes of BLRs of low luminosity AGN are larger than the ones
expected from the empirical relation $R_{BLRs} - L_{H\alpha}$ valid for
'normal' AGN: Seyfert 1s and quasars, except for the objects with accretion
rate $\dot{m_{H\alpha}}>10^{-5.5}$. Second, we find a positive correlation
between the line width of the narrow emission line (as tracer of velocity
dipersion and thus bulge and black hole mass) and the size of BLRs for both
normal and low luminosity AGN. In this paper we find a non-linear dependence of
the BLRs sizes of low luminosity AGN on BH masses. We also show that their
sizes of BLRs are more strongly dominated by the 'specific accretion rate'
$\dot{m_{H\alpha}}$ defined as $\dot{m_{H\alpha}} = L_{H\alpha}/L_{Edd}$, than
by the masses of their cetral black holes. As an expected result, the distance
of emission regions of low-ionization broad H$\alpha$ of NGC 4395 should be
consistent with the value from the empirical relation of $R_{BLRs} -
L_{H\alpha}$, according to the high accretion rate.
