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The evolution of the photospheric magnetic field plays a key role in theenergy transport into the chromosphere and the corona. In active regions, newlyemerging magnetic flux interacts with the pre-existent magnetic field, whichcan lead to reconnection events that convert magnetic energy to thermal energy.We aim to study the heating caused by a strong reconnection event that wastriggered by magnetic flux cancellation. We use imaging-spectropolarimetricdata in the Fe I 6301A, Fe I 6302A, Ca II 8542A and Ca II K obtained with theCRISP and CHROMIS instruments at the Swedish 1-m Solar Telescope. This data wasinverted using multi-atom, multi-line non-LTE inversions using the STiC code.The inversion yielded a three-dimensional model of the reconnection event andsurrounding atmosphere, including temperature, velocity, microturbulence,magnetic file configuration, and the radiative loss rate. The model atmosphereshows the emergence of magnetic loops with a size of several arcsecs into apre-existing predominantly unipolar field. Where the reconnection region isexpected to be, we see an increase in the chromospheric temperature of roughly2000 K as well as bidirectional flows of the order of 10 km s$^{-1}$ emanatingfrom the region. We see bright blobs of roughly 0.2 arcsec diameter in the CaII K moving at a plane-of-the-sky velocity of order 100 km s$^{-1}$ and ablueshift of 100 km s$^{-1}$, which we interpret as plasmoids ejected from thesame region. This evidence is consistent with theoretical models ofreconnection and we thus conclude that reconnection is taking place. Thechromospheric radiative losses at the reconnection site in our inferred modelare as high as 160 kW m$^{-2}$, providing a quantitative constraint ontheoretical models that aim to simulate reconnection caused by flux emergencein the chromosphere.

astronomy and astrophysics

An observationally-constrained model of strong magnetic reconnection in  the solar chromosphere. Atmospheric stratification and estimates of heating  rates