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High-resolution observations of the solar chromosphere at millimeterwavelengths are now possible with the Atacama Large Millimeter Array (ALMA),promising to tackle many open problems in solar physics. Observations fromother ground and space-based telescopes will greatly benefit from coordinatedendeavors with ALMA, yet the diagnostic potential of combined optical,ultraviolet and mm observations has remained mostly unassessed. In this paperwe investigate whether mm-wavelengths could aid current inversion schemes toretrieve a more accurate representation of the temperature structure of thesolar atmosphere. We performed several non-LTE inversion experiments of theemergent spectra from a snapshot of 3D radiation-MHD simulation. We includedcommon line diagnostics such as CaII H, K, 8542 \AA$\,$ and MgII h and k,taking into account partial frequency redistribution effects, along with thecontinuum around 1.2 mm and 3 mm. We found that including the mm-continuum ininversions allows a more accurate inference of temperature as function ofoptical depth. The addition of ALMA bands to other diagnostics should improvethe accuracy of the inferred chromospheric temperatures between $\log\tau\sim[-6,-4.5]$ where the CaII and MgII lines are weakly coupled to thelocal conditions. However, we found that simultaneous multi-atom, non-LTEinversions of optical and UV lines present equally strong constraints in thelower chromosphere and thus are not greatly improved by the 1.2 mm band.Nonetheless, the 3 mm band is still needed to better constrain the mid-upperchromosphere.

Temperature constraints from inversions of synthetic solar optical, UV and radio spectra