  The primary objective of this thesis is to identify the key dynamical
mechanisms responsible for the superthin stellar discs. We use HI 21cm
radio-synthesis observations and stellar photometry to construct detailed
dynamical models of a sample of superthin galaxies to determine the primary
mechanism responsible for the existence of superthin stellar discs in these
galaxies. Our study is based on a sample of superthin galaxies with $\rm 10<
a/b < 16$ for which H1 21cm radio-synthesis data were already available in the
literature. In addition, we had the two thinnest galaxies in our sample with
$\rm a/b \sim 21$, for which we carried out Giant Meterwave Radio Telescope
(GMRT) 21cm radio-synthesis observations. To identify the physical mechanism
primarily responsible for the superthin vertical structure, we carry out a
Principal Component Analysis of the following dynamical parameters: 1) Dark
matter dominance at inner galactocentric radii given by
$V_{\rm{rot}}/{(R_{c}/R_{d})}$, 2) the ratio of the vertical-to-radial stellar
velocity dispersion $(\sigma_{z,s}/\sigma_{R,s})$, 3) Disc dynamical stability
against local axisymmetric perturbations $Q_{RW}$, 4) Specific angular momentum
of the disc $(j_{*})$, along with $a/b$ for all superthins and the extremely
thin galaxies. We note that the first two principal components explain $\sim$
80$\%$ of the variation in the data, and the major contributions are from
$a/b$, $Q_{RW}$ and $V_{\rm{rot}}/{(R_{c}/R_{d})}$. This possibly indicates
that high values of the disc dynamical stability and dark matter dominance at
inner galactocentric radii are fundamentally responsible for the superthin
stellar discs.
