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We have carried out an extensive X-ray spectral study of the bare Seyfert-1galaxy MCG--02--58--22 to ascertain the nature of the X-ray reprocessing media,using observations from Suzaku (2009) and simultaneous observations fromXMM-Newton and NuSTAR (2016) . The most significant results of ourinvestigation are: 1. The primary X-ray emission from the corona is constant inthese observations, both in terms of the power law slope ($\Gamma=1.80$) andluminosity ($L_{2-10 \rm keV}= 2.55\times 10^{44} $ erg/s). 2. The soft excessflux decreased by a factor of two in 2016, the Compton hump weakened/vanishedin 2016, and the narrow FeK$\alpha$ emission line became marginally broad($\sigma=0.35\pm0.08$ keV) and its flux doubled in 2016. 3. From physical modelfits we find that the normalization of the narrow component of the FeK$\alpha$line does not change in the two epochs, although the Compton hump vanishes inthe same time span. Since the primary X-ray continuum does not change, wepresume that any changes in the reprocessed emission must arise due to changesin the reprocessing media. Our primary conclusions are: A. The vanishing of theCompton hump in 2016 can probably be explained by a dynamic clumpy torus whichis infalling/outflowing, or by a polar torus wind. B. The torus in this AGNpossibly has two structures: an equatorial toroidal disk (producing the narrowFeK$\alpha$ emission) and a polar component (producing the variable Comptonhump), C. The reduction of the soft-excess flux by half and increase in theFeK$\alpha$ flux by a factor of two in the same period cannot be adequatelyexplained by ionized disk reflection model alone.

A weakening Compton hump and soft X-ray excess detected in the Seyfert-1 galaxy MCG-02-58-22