  TCP J18224935-2408280 was reported to be in outburst on 2021 May 19.
Follow-up spectroscopic observations confirmed that the system was a symbiotic
star. We present optical spectra obtained from the Himalayan Chandra Telescope
during 2021-22. The early spectra were dominated by Balmer lines, He I lines
and high ionization lines such as He II. In the later observations, Raman
scattered O VI was also identified. Outburst in the system started as a disc
instability, and later the signature of enhanced shell burning and expansion of
photospheric radius of the white dwarf was identified. Hence we suggest this
outburst is of combination nova type. The post-outburst temperature of the hot
component remains above 1.5 x 10$^5$ K indicating a stable shell burning in the
system for a prolonged time after the outburst. Based on our analysis of
archival multiband photometric data, we find that the system contains a cool
giant of M1-2 III spectral type with a temperature of $\sim$ 3600K and a radius
of $\sim$ 69 R$_\odot$. The pre- and post-outburst light curve shows a
periodicity of 631.25 $\pm$ 2.93 d; we consider this as the orbital period.
