  The nature of the close-in rocky planet 55 Cnc e is puzzling despite having
been observed extensively. Its optical and infrared occultation depths show
temporal variability, in addition to a phase curve variability observed in the
optical. We wish to explore the possibility that the variability originates
from the planet being in a 3:2 spin-orbit resonance, thus showing different
sides during occultations. We proposed and were awarded Cycle 1 time at the
James Webb Space Telescope (JWST) to test this hypothesis. JWST/NIRCam observed
five occultations (secondary eclipses), of which four were observed within a
week, of the planet simultaneously at 2.1 and 4.5 {\mu}m. While the former
gives band-integrated photometry, the latter provides a spectrum between
3.9-5.0 {\mu}m. We find that the occultation depths in both bandpasses are
highly variable and change between a non-detection (-5 +/- 6 ppm and 7 +/- 9
ppm) to 96 +/- 8 ppm and 119 (+34) (-19) ppm at 2.1 {\mu}m and 4.5 {\mu}m,
respectively. Interestingly, the variations in both bandpasses are not
correlated and do not support the 3:2 spin-orbit resonance explanation. The
measured brightness temperature at 4.5 {\mu}m varies between 873-2256 K and is
lower than the expected dayside temperature of bare rock with no heat
re-distribution (2500 K) which is indicative of an atmosphere. Our atmospheric
retrieval analysis of occultation depth spectra at 4.5 {\mu}m finds that
different visits statistically favour various atmospheric scenarios including a
thin outgassed CO/CO2 atmosphere and a silicate rock vapour atmosphere. Some
visits even support a flat line model. The observed variability could be
explained by stochastic outgassing of CO/CO2, which is also hinted by
retrievals. Alternatively, the variability, observed at both 2.1 and 4.5
{\mu}m, could be the result of a circumstellar patchy dust torus generated by
volcanism on the planet.
