  Novae, explosive events in binary star systems involving a white dwarf and a
companion star, offer profound insights into extreme astrophysical conditions.
During the eruption of a nova, material accreted onto the white dwarf's surface
undergoes a thermonuclear runaway reaction resulting in the ejection of matter
into space and the formation of a luminous shell. The classical V5668 Sgr (Nova
Sagittarii) was the second and brighter of the two novae in the southern
constellation of Sagittarius. It was discovered by John Seach of Chatsworth
Island, Australia, on March 15, 2015. In this paper, drawing on data from Karl
G. Jansky Very Large Array, the US-based radio astronomy observatory, on V5668
Sgr as well as from research that aggregates data from a range of sources
including telescope archives, this study used the Uniform Slab Model and
statistical techniques to plot the nova's light and frequency curves and
estimate its ejected shell mass and the brightness temperature. These
characteristics help us better understand the nova's formation and eruption.
The paper presents the light curves in a machine-readable format and provides
insight into the behaviour of ionised gas clouds.
