  We present an update of the open-source photochemical kinetics code VULCAN
(Tsai et al. 2017; https://github.com/exoclime/VULCAN) to include C-H-N-O-S
networks and photochemistry. Additional new features are advection transport,
condensation, various boundary conditions, and temperature-dependent UV
cross-sections. First, we validate our photochemical model for hot Jupiter
atmospheres by performing an intercomparison of HD 189733b models between Moses
et al. (2011), Venot et al. (2012), and VULCAN, to diagnose possible sources of
discrepancy. Second, we set up a model of Jupiter extending from the deep
troposphere to upper stratosphere to verify the kinetics for low temperature.
Our model reproduces hydrocarbons consistent with observations, and the
condensation scheme successfully predicts the locations of water and ammonia
ice clouds. We show that vertical advection can regulate the local ammonia
distribution in the deep atmosphere. Third, we validate the model for oxidizing
atmospheres by simulating Earth and find agreement with observations. Last,
VULCAN is applied to four representative cases of extrasolar giant planets:
WASP-33b, HD 189733b, GJ 436b, and 51 Eridani b. We look into the effects of
the C/O ratio and chemistry of titanium/vanadium species for WASP-33b; we
revisit HD 189733b for the effects of sulfur and carbon condensation; the
effects of internal heating and vertical mixing ($K_{\textrm{zz}}$) are
explored for GJ 436b; we test updated planetary properties for 51 Eridani b
with S$_8$ condensates. We find sulfur can couple to carbon or nitrogen and
impact other species such as hydrogen, methane, and ammonia. The observable
features of the synthetic spectra and trends in the photochemical haze
precursors are discussed for each case.
