Origin of low surface brightness galaxies: A dynamical study
  Low Surface Brighness Galaxies (LSBs), inspite of being gas rich, have low
star formation rates and are, therefore, low surface brightness in nature. We
calculate Q$_{\rm{RW}}$, the 2-component disc stability parameter as proposed
by Romeo \& Wiegert (2011), as a function of galactocentric radius $R$ for a
sample of five LSBs, for which mass models, as obtained from HI 21cm
radio-sythesis observations and R-band photometry, were available in the
literature. We find that the median value of Q$_{\rm{RW}}^{\rm{min}}$, the
minimum of Q$_{\rm{RW}}$ over $R$, lies between 2.6 and 3.1 for our sample
LSBs, which is higher than the median value of 1.8 $\pm$ 0.3 for
Q$_{\rm{RW}}^{\rm{min}}$ for a sampleof high surface brightness galaxies (HSBs)
as obtained in earlier studies. This clearly shows that LSBs have more stable
discs than HSBs, which could explain their low star formation rates and,
possibly, their low surface brightness nature. Interestingly, the calculated
values of Q$_{\rm{RW}}$ decrease only slightly (median Q$_{\rm{RW}}^{\rm{min}}$
$\sim$ 2.3 - 3) if the discs were taken to respond to the gravitational
potential of the dark matter halo only, but reduce by $\sim$ a factor of 2-3
(median Q$_{\rm{RW}}^{\rm{min}}$ $\sim$ 0.7 - 1.5) if they respond to their
self-gravity alone. This implies that the dark matter halo is crucial in
regulating disc stability in LSBs, which may have important implications for
models of galaxy formation and evolution.
