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We report on one of the brightest flux levels of the Seyfert 2 galaxy NGC2992 ever observed in X-rays, on May 2019. The source has been monitored everyfew days from March 26, 2019 to December 14, 2019 by Swift-XRT, andsimultaneous XMM-Newton (250 ks) and NuSTAR (120 ks) observations weretriggered on May 6, 2019. The high count rate of the source (its 2-10 keV fluxranged between 0.7 and $1.0\times10^{-10}$ erg cm$^{-2}$ s$^{-1}$) allows us toperform a time-resolved spectroscopy, probing spatial scales of tens ofgravitational radii from the central black hole. By constructing a map of theexcess emission over the primary continuum, we find several emission structuresin the 5.0-7.2 keV energy band. From fitting the 50 EPIC pn spectral slices of$\sim$5 ks duration, we interpret them as a constant narrow iron K$\alpha$ lineand three variable components in the iron K complex. When a self-consistentmodel accounting for the accretion disk emission is considered (KYNrline), twoof these features (in the 5.0-5.8 keV and 6.8-7.2 keV bands) can be ascribed toa flaring region of the accretion disk located at ${r_{in}}\simeq15$-40r$_{g\rm }$ from the black hole. The third one (6.5-6.8 keV) is likely producedat much larger radii ($r_{in}>50$ r$_{g\rm }$). The inner radius and theazimuthal extension retrieved from the coadded spectra of the flaring statesare ${ r_{in}}=15\pm3$ r$_{g\rm }$ and $\phi=165^{\circ}-330^{\circ}$,suggesting that the emitting region responsible for the broad iron K componentis a relatively compact annular sector within the disk. Our findings support aphysical scenario in which the accretion disk in NGC 2992 becomes more activeat high accretion rates ($L_{\rm bol}/L_{\rm Edd}\geq4\%$).

The lively accretion disk in NGC 2992. I. Transient iron K emission lines in the high flux state