  In this article, the association of solar radio type IV bursts with active
region location on the Sun is studied for the solar cycle 24. The active
regions associated with moving and stationary type IV bursts are categorised as
close to disk center and far from disk center regions based on their location
on the solar surface (i.e, $\leq 45^{\circ}$ or $\geq 45^{\circ}$,
respectively). The location of the active regions associated with type IV
bursts accompanied with coronal mass ejections (CMEs) are also studied. We
found that $\approx 30-40 \%$ of the active regions are located far from disk
center for all the bursts. It is found that most of the active regions
associated with stationary type IV bursts are close to disk center ($\approx
60-70 \%$). The active regions associated with moving type IV bursts are more
evenly distributed across the surface, i.e $\approx 56 \%$ and $\approx 44 \%$,
close to disk center and far from disk center regions, respectively. Most of
the burst having active region close to disk center indicate that these bursts
can be used to obtain physical properties such as electron density and magnetic
fields of the coronal mass ejections responsible for geomagnetic storms.
